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id="p-vector-user-menu-notifications" class="vector-menu mw-portlet emptyPortlet" > <div class="vector-menu-content"> <ul class="vector-menu-content-list"> </ul> </div> </div> <div id="p-vector-user-menu-overflow" class="vector-menu mw-portlet" > <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li id="pt-sitesupport-2" class="user-links-collapsible-item mw-list-item user-links-collapsible-item"><a data-mw="interface" href="//donate.wikimedia.org/wiki/Special:FundraiserRedirector?utm_source=donate&utm_medium=sidebar&utm_campaign=C13_af.wikipedia.org&uselang=af" class=""><span>Skenkings</span></a> </li> <li id="pt-createaccount-2" class="user-links-collapsible-item mw-list-item user-links-collapsible-item"><a data-mw="interface" href="/w/index.php?title=Spesiaal:SkepRekening&returnto=Veranderlike+ster" title="U word aangemoedig om 'n gebruiker te skep en aan te meld, hoewel dit nie verpligtend is nie." class=""><span>Skep gebruiker</span></a> </li> <li 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[o]" accesskey="o" class=""><span>Meld aan</span></a> </li> </ul> </div> </div> </div> <div id="vector-user-links-dropdown" class="vector-dropdown vector-user-menu vector-button-flush-right vector-user-menu-logged-out" title="Meer opsies" > <input type="checkbox" id="vector-user-links-dropdown-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-vector-user-links-dropdown" class="vector-dropdown-checkbox " aria-label="Persoonlike gereedskap" > <label id="vector-user-links-dropdown-label" for="vector-user-links-dropdown-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--icon-only " aria-hidden="true" ><span class="vector-icon mw-ui-icon-ellipsis mw-ui-icon-wikimedia-ellipsis"></span> <span class="vector-dropdown-label-text">Persoonlike gereedskap</span> </label> <div class="vector-dropdown-content"> <div id="p-personal" class="vector-menu mw-portlet mw-portlet-personal user-links-collapsible-item" title="User menu" > <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li id="pt-sitesupport" class="user-links-collapsible-item mw-list-item"><a href="//donate.wikimedia.org/wiki/Special:FundraiserRedirector?utm_source=donate&utm_medium=sidebar&utm_campaign=C13_af.wikipedia.org&uselang=af"><span>Skenkings</span></a></li><li id="pt-createaccount" class="user-links-collapsible-item mw-list-item"><a href="/w/index.php?title=Spesiaal:SkepRekening&returnto=Veranderlike+ster" title="U word aangemoedig om 'n gebruiker te skep en aan te meld, hoewel dit nie verpligtend is nie."><span class="vector-icon mw-ui-icon-userAdd mw-ui-icon-wikimedia-userAdd"></span> <span>Skep gebruiker</span></a></li><li id="pt-login" class="user-links-collapsible-item mw-list-item"><a href="/w/index.php?title=Spesiaal:Teken_in&returnto=Veranderlike+ster" title="U word aangemoedig om aan te meld. 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[o]" accesskey="o"><span class="vector-icon mw-ui-icon-logIn mw-ui-icon-wikimedia-logIn"></span> <span>Meld aan</span></a></li> </ul> </div> </div> <div id="p-user-menu-anon-editor" class="vector-menu mw-portlet mw-portlet-user-menu-anon-editor" > <div class="vector-menu-heading"> Bladsye vir uitgemelde redakteurs <a href="/wiki/Hulp:Inleiding" aria-label="Leer meer oor redigering"><span>leer meer</span></a> </div> <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li id="pt-anoncontribs" class="mw-list-item"><a href="/wiki/Spesiaal:Mybydrae" title="A list of edits made from this IP address [y]" accesskey="y"><span>Bydraes</span></a></li><li id="pt-anontalk" class="mw-list-item"><a href="/wiki/Spesiaal:Mybespreking" title="Bespreking oor bydraes van hierdie IP-adres [n]" accesskey="n"><span>Bespreking</span></a></li> </ul> </div> </div> </div> </div> </nav> </div> </header> </div> <div class="mw-page-container"> <div class="mw-page-container-inner"> <div class="vector-sitenotice-container"> <div id="siteNotice"></div> </div> <div class="vector-column-start"> <div class="vector-main-menu-container"> <div id="mw-navigation"> <nav id="mw-panel" class="vector-main-menu-landmark" aria-label="Werf"> <div id="vector-main-menu-pinned-container" class="vector-pinned-container"> </div> </nav> </div> </div> <div class="vector-sticky-pinned-container"> <nav id="mw-panel-toc" aria-label="Inhoud" data-event-name="ui.sidebar-toc" class="mw-table-of-contents-container vector-toc-landmark"> <div id="vector-toc-pinned-container" class="vector-pinned-container"> <div id="vector-toc" class="vector-toc vector-pinnable-element"> <div class="vector-pinnable-header vector-toc-pinnable-header vector-pinnable-header-pinned" data-feature-name="toc-pinned" data-pinnable-element-id="vector-toc" > <h2 class="vector-pinnable-header-label">Inhoud</h2> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-pin-button" data-event-name="pinnable-header.vector-toc.pin">skuif na kantbalk</button> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-unpin-button" data-event-name="pinnable-header.vector-toc.unpin">versteek</button> </div> <ul class="vector-toc-contents" id="mw-panel-toc-list"> <li id="toc-mw-content-text" class="vector-toc-list-item vector-toc-level-1"> <a href="#" class="vector-toc-link"> <div class="vector-toc-text">Inleiding</div> </a> </li> <li id="toc-Ontdekking" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Ontdekking"> <div class="vector-toc-text"> <span class="vector-toc-numb">1</span> <span>Ontdekking</span> </div> </a> <ul id="toc-Ontdekking-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Die_bespeuring_van_veranderlikheid" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Die_bespeuring_van_veranderlikheid"> <div class="vector-toc-text"> <span class="vector-toc-numb">2</span> <span>Die bespeuring van veranderlikheid</span> </div> </a> <button aria-controls="toc-Die_bespeuring_van_veranderlikheid-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Wissel Die bespeuring van veranderlikheid subafdeling</span> </button> <ul id="toc-Die_bespeuring_van_veranderlikheid-sublist" class="vector-toc-list"> <li id="toc-Waarnemings" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Waarnemings"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1</span> <span>Waarnemings</span> </div> </a> <ul id="toc-Waarnemings-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Interpretasie_van_waarnemings" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Interpretasie_van_waarnemings"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.2</span> <span>Interpretasie van waarnemings</span> </div> </a> <ul id="toc-Interpretasie_van_waarnemings-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Benaming_van_veranderlike_sterre" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Benaming_van_veranderlike_sterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">3</span> <span>Benaming van veranderlike sterre</span> </div> </a> <ul id="toc-Benaming_van_veranderlike_sterre-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Klassifikasie" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Klassifikasie"> <div class="vector-toc-text"> <span class="vector-toc-numb">4</span> <span>Klassifikasie</span> </div> </a> <ul id="toc-Klassifikasie-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Intrinsieke_veranderlike_sterre" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Intrinsieke_veranderlike_sterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">5</span> <span>Intrinsieke veranderlike sterre</span> </div> </a> <button aria-controls="toc-Intrinsieke_veranderlike_sterre-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Wissel Intrinsieke veranderlike sterre subafdeling</span> </button> <ul id="toc-Intrinsieke_veranderlike_sterre-sublist" class="vector-toc-list"> <li id="toc-Pulserende_veranderlikes" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Pulserende_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1</span> <span>Pulserende veranderlikes</span> </div> </a> <ul id="toc-Pulserende_veranderlikes-sublist" class="vector-toc-list"> <li id="toc-Cepheïede_en_Cepheïed-agtige_veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Cepheïede_en_Cepheïed-agtige_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.1</span> <span>Cepheïede en Cepheïed-agtige veranderlikes</span> </div> </a> <ul id="toc-Cepheïede_en_Cepheïed-agtige_veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Langperiode-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Langperiode-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.2</span> <span>Langperiode-veranderlikes</span> </div> </a> <ul id="toc-Langperiode-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Beta_Cephei-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Beta_Cephei-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.3</span> <span>Beta Cephei-veranderlikes</span> </div> </a> <ul id="toc-Beta_Cephei-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Stadig_pulserende_B-sterre" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Stadig_pulserende_B-sterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.4</span> <span>Stadig pulserende B-sterre</span> </div> </a> <ul id="toc-Stadig_pulserende_B-sterre-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-PV_Telescopii-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#PV_Telescopii-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.5</span> <span>PV Telescopii-veranderlikes</span> </div> </a> <ul id="toc-PV_Telescopii-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-RV_Tauri-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#RV_Tauri-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.6</span> <span>RV Tauri-veranderlikes</span> </div> </a> <ul id="toc-RV_Tauri-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Alpha_Cygni-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Alpha_Cygni-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.7</span> <span>Alpha Cygni-veranderlikes</span> </div> </a> <ul id="toc-Alpha_Cygni-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Gamma_Doradus-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Gamma_Doradus-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.8</span> <span>Gamma Doradus-veranderlikes</span> </div> </a> <ul id="toc-Gamma_Doradus-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Pulserende_witdwerge" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Pulserende_witdwerge"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.9</span> <span>Pulserende witdwerge</span> </div> </a> <ul id="toc-Pulserende_witdwerge-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Sonagtige_skommelings" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Sonagtige_skommelings"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.10</span> <span>Sonagtige skommelings</span> </div> </a> <ul id="toc-Sonagtige_skommelings-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Uitbarstende_veranderlikes" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Uitbarstende_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2</span> <span>Uitbarstende veranderlikes</span> </div> </a> <ul id="toc-Uitbarstende_veranderlikes-sublist" class="vector-toc-list"> <li id="toc-Protosterre" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Protosterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.1</span> <span>Protosterre</span> </div> </a> <ul id="toc-Protosterre-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Reuse_en_superreuse" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Reuse_en_superreuse"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.2</span> <span>Reuse en superreuse</span> </div> </a> <ul id="toc-Reuse_en_superreuse-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Wolf-Rayet-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Wolf-Rayet-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.3</span> <span>Wolf-Rayet-veranderlikes</span> </div> </a> <ul id="toc-Wolf-Rayet-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Gamma_Cassiopeiae-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Gamma_Cassiopeiae-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.4</span> <span>Gamma Cassiopeiae-veranderlikes</span> </div> </a> <ul id="toc-Gamma_Cassiopeiae-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Opvlamsterre" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Opvlamsterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.5</span> <span>Opvlamsterre</span> </div> </a> <ul id="toc-Opvlamsterre-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-RS_Canum_Venaticorum-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#RS_Canum_Venaticorum-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2.6</span> <span>RS Canum Venaticorum-veranderlikes</span> </div> </a> <ul id="toc-RS_Canum_Venaticorum-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Kataklismiese_veranderlikes" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Kataklismiese_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3</span> <span>Kataklismiese veranderlikes</span> </div> </a> <ul id="toc-Kataklismiese_veranderlikes-sublist" class="vector-toc-list"> <li id="toc-Supernovas" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Supernovas"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3.1</span> <span>Supernovas</span> </div> </a> <ul id="toc-Supernovas-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Novas" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Novas"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3.2</span> <span>Novas</span> </div> </a> <ul id="toc-Novas-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> </ul> </li> <li id="toc-Ekstrinsieke_veranderlikes" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Ekstrinsieke_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">6</span> <span>Ekstrinsieke veranderlikes</span> </div> </a> <button aria-controls="toc-Ekstrinsieke_veranderlikes-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Wissel Ekstrinsieke veranderlikes subafdeling</span> </button> <ul id="toc-Ekstrinsieke_veranderlikes-sublist" class="vector-toc-list"> <li id="toc-Roterende_veranderlikes" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Roterende_veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.1</span> <span>Roterende veranderlikes</span> </div> </a> <ul id="toc-Roterende_veranderlikes-sublist" class="vector-toc-list"> <li id="toc-Niesferiese_sterre" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Niesferiese_sterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.1.1</span> <span>Niesferiese sterre</span> </div> </a> <ul id="toc-Niesferiese_sterre-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Stervlekke" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Stervlekke"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.1.2</span> <span>Stervlekke</span> </div> </a> <ul id="toc-Stervlekke-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Magneetvelde" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Magneetvelde"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.1.3</span> <span>Magneetvelde</span> </div> </a> <ul id="toc-Magneetvelde-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Verduisterende_dubbelsterre" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Verduisterende_dubbelsterre"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.2</span> <span>Verduisterende dubbelsterre</span> </div> </a> <ul id="toc-Verduisterende_dubbelsterre-sublist" class="vector-toc-list"> <li id="toc-Algol-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Algol-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.2.1</span> <span>Algol-veranderlikes</span> </div> </a> <ul id="toc-Algol-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Beta_Lyrae-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Beta_Lyrae-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.2.2</span> <span>Beta Lyrae-veranderlikes</span> </div> </a> <ul id="toc-Beta_Lyrae-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-W_Ursae_Majoris-veranderlikes" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#W_Ursae_Majoris-veranderlikes"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.2.3</span> <span>W Ursae Majoris-veranderlikes</span> </div> </a> <ul id="toc-W_Ursae_Majoris-veranderlikes-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Planetêre_oorgange" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Planetêre_oorgange"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.3</span> <span>Planetêre oorgange</span> </div> </a> <ul id="toc-Planetêre_oorgange-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Verwysings" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Verwysings"> <div class="vector-toc-text"> <span class="vector-toc-numb">7</span> <span>Verwysings</span> </div> </a> <ul id="toc-Verwysings-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Eksterne_skakels" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Eksterne_skakels"> <div class="vector-toc-text"> <span class="vector-toc-numb">8</span> <span>Eksterne skakels</span> </div> </a> <ul id="toc-Eksterne_skakels-sublist" class="vector-toc-list"> </ul> </li> </ul> </div> </div> </nav> </div> </div> <div class="mw-content-container"> <main id="content" class="mw-body"> <header class="mw-body-header vector-page-titlebar"> <nav aria-label="Inhoud" class="vector-toc-landmark"> <div id="vector-page-titlebar-toc" class="vector-dropdown vector-page-titlebar-toc vector-button-flush-left" > <input type="checkbox" id="vector-page-titlebar-toc-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-vector-page-titlebar-toc" class="vector-dropdown-checkbox " aria-label="Wissel die inhoudsopgawe" > <label id="vector-page-titlebar-toc-label" for="vector-page-titlebar-toc-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--icon-only " aria-hidden="true" ><span class="vector-icon mw-ui-icon-listBullet mw-ui-icon-wikimedia-listBullet"></span> <span class="vector-dropdown-label-text">Wissel die inhoudsopgawe</span> </label> <div class="vector-dropdown-content"> <div id="vector-page-titlebar-toc-unpinned-container" class="vector-unpinned-container"> </div> </div> </div> </nav> <h1 id="firstHeading" class="firstHeading mw-first-heading"><span class="mw-page-title-main">Veranderlike ster</span></h1> <div id="p-lang-btn" class="vector-dropdown mw-portlet mw-portlet-lang" > <input type="checkbox" id="p-lang-btn-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-p-lang-btn" class="vector-dropdown-checkbox mw-interlanguage-selector" aria-label="Gaan na 'n artikel in 'n ander taal. Beskikbaar in 65 tale" > <label id="p-lang-btn-label" for="p-lang-btn-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--action-progressive mw-portlet-lang-heading-65" aria-hidden="true" ><span class="vector-icon mw-ui-icon-language-progressive mw-ui-icon-wikimedia-language-progressive"></span> <span class="vector-dropdown-label-text">65 tale</span> </label> <div class="vector-dropdown-content"> <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li class="interlanguage-link interwiki-ar mw-list-item"><a href="https://ar.wikipedia.org/wiki/%D9%86%D8%AC%D9%85_%D9%85%D8%AA%D8%BA%D9%8A%D8%B1" title="نجم متغير – Arabies" lang="ar" hreflang="ar" data-title="نجم متغير" data-language-autonym="العربية" data-language-local-name="Arabies" class="interlanguage-link-target"><span>العربية</span></a></li><li class="interlanguage-link interwiki-ast mw-list-item"><a href="https://ast.wikipedia.org/wiki/Estrella_variable" title="Estrella variable – Asturies" lang="ast" hreflang="ast" data-title="Estrella variable" data-language-autonym="Asturianu" data-language-local-name="Asturies" class="interlanguage-link-target"><span>Asturianu</span></a></li><li class="interlanguage-link interwiki-az mw-list-item"><a href="https://az.wikipedia.org/wiki/D%C9%99yi%C5%9F%C9%99n_ulduz" title="Dəyişən ulduz – Azerbeidjans" lang="az" hreflang="az" data-title="Dəyişən ulduz" data-language-autonym="Azərbaycanca" data-language-local-name="Azerbeidjans" class="interlanguage-link-target"><span>Azərbaycanca</span></a></li><li class="interlanguage-link interwiki-be mw-list-item"><a href="https://be.wikipedia.org/wiki/%D0%9F%D0%B5%D1%80%D0%B0%D0%BC%D0%B5%D0%BD%D0%BD%D0%B0%D1%8F_%D0%B7%D0%BE%D1%80%D0%BA%D0%B0" title="Пераменная зорка – Belarussies" lang="be" hreflang="be" data-title="Пераменная зорка" data-language-autonym="Беларуская" data-language-local-name="Belarussies" class="interlanguage-link-target"><span>Беларуская</span></a></li><li class="interlanguage-link interwiki-bg mw-list-item"><a href="https://bg.wikipedia.org/wiki/%D0%9F%D1%80%D0%BE%D0%BC%D0%B5%D0%BD%D0%BB%D0%B8%D0%B2%D0%B0_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Променлива звезда – Bulgaars" lang="bg" hreflang="bg" data-title="Променлива звезда" data-language-autonym="Български" data-language-local-name="Bulgaars" class="interlanguage-link-target"><span>Български</span></a></li><li class="interlanguage-link interwiki-bn mw-list-item"><a href="https://bn.wikipedia.org/wiki/%E0%A6%AC%E0%A6%BF%E0%A6%B7%E0%A6%AE%E0%A6%A4%E0%A6%BE%E0%A6%B0%E0%A6%BE" title="বিষমতারা – Bengaals" lang="bn" hreflang="bn" data-title="বিষমতারা" data-language-autonym="বাংলা" data-language-local-name="Bengaals" class="interlanguage-link-target"><span>বাংলা</span></a></li><li class="interlanguage-link interwiki-bs mw-list-item"><a href="https://bs.wikipedia.org/wiki/Promjenjiva_zvijezda" title="Promjenjiva zvijezda – Bosnies" lang="bs" hreflang="bs" data-title="Promjenjiva zvijezda" data-language-autonym="Bosanski" data-language-local-name="Bosnies" class="interlanguage-link-target"><span>Bosanski</span></a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Estrella_variable" title="Estrella variable – Katalaans" lang="ca" hreflang="ca" data-title="Estrella variable" data-language-autonym="Català" data-language-local-name="Katalaans" class="interlanguage-link-target"><span>Català</span></a></li><li class="interlanguage-link interwiki-cs mw-list-item"><a href="https://cs.wikipedia.org/wiki/Prom%C4%9Bnn%C3%A1_hv%C4%9Bzda" title="Proměnná hvězda – Tsjeggies" lang="cs" hreflang="cs" data-title="Proměnná hvězda" data-language-autonym="Čeština" data-language-local-name="Tsjeggies" class="interlanguage-link-target"><span>Čeština</span></a></li><li class="interlanguage-link interwiki-cv mw-list-item"><a href="https://cv.wikipedia.org/wiki/%D0%A3%D0%BB%D1%88%C4%83%D0%BD%D1%83%D0%BB%D0%BB%C4%83_%C3%A7%C4%83%D0%BB%D1%82%C4%83%D1%80" title="Улшăнуллă çăлтăр – Chuvash" lang="cv" hreflang="cv" data-title="Улшăнуллă çăлтăр" data-language-autonym="Чӑвашла" data-language-local-name="Chuvash" class="interlanguage-link-target"><span>Чӑвашла</span></a></li><li class="interlanguage-link interwiki-de mw-list-item"><a href="https://de.wikipedia.org/wiki/Ver%C3%A4nderlicher_Stern" title="Veränderlicher Stern – Duits" lang="de" hreflang="de" data-title="Veränderlicher Stern" data-language-autonym="Deutsch" data-language-local-name="Duits" class="interlanguage-link-target"><span>Deutsch</span></a></li><li class="interlanguage-link interwiki-el mw-list-item"><a href="https://el.wikipedia.org/wiki/%CE%9C%CE%B5%CF%84%CE%B1%CE%B2%CE%BB%CE%B7%CF%84%CF%8C%CF%82_%CE%B1%CF%83%CF%84%CE%AD%CF%81%CE%B1%CF%82" title="Μεταβλητός αστέρας – Grieks" lang="el" hreflang="el" data-title="Μεταβλητός αστέρας" data-language-autonym="Ελληνικά" data-language-local-name="Grieks" class="interlanguage-link-target"><span>Ελληνικά</span></a></li><li class="interlanguage-link interwiki-en mw-list-item"><a href="https://en.wikipedia.org/wiki/Variable_star" title="Variable star – Engels" lang="en" hreflang="en" data-title="Variable star" data-language-autonym="English" data-language-local-name="Engels" class="interlanguage-link-target"><span>English</span></a></li><li class="interlanguage-link interwiki-eo mw-list-item"><a href="https://eo.wikipedia.org/wiki/Varia_stelo" title="Varia stelo – Esperanto" lang="eo" hreflang="eo" data-title="Varia stelo" data-language-autonym="Esperanto" data-language-local-name="Esperanto" class="interlanguage-link-target"><span>Esperanto</span></a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/Estrella_variable" title="Estrella variable – Spaans" lang="es" hreflang="es" data-title="Estrella variable" data-language-autonym="Español" data-language-local-name="Spaans" class="interlanguage-link-target"><span>Español</span></a></li><li class="interlanguage-link interwiki-et mw-list-item"><a href="https://et.wikipedia.org/wiki/Muutlik_t%C3%A4ht" title="Muutlik täht – Estnies" lang="et" hreflang="et" data-title="Muutlik täht" data-language-autonym="Eesti" data-language-local-name="Estnies" class="interlanguage-link-target"><span>Eesti</span></a></li><li class="interlanguage-link interwiki-eu mw-list-item"><a href="https://eu.wikipedia.org/wiki/Izar_aldakor" title="Izar aldakor – Baskies" lang="eu" hreflang="eu" data-title="Izar aldakor" data-language-autonym="Euskara" data-language-local-name="Baskies" class="interlanguage-link-target"><span>Euskara</span></a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%B3%D8%AA%D8%A7%D8%B1%D9%87_%D9%85%D8%AA%D8%BA%DB%8C%D8%B1" title="ستاره متغیر – Persies" lang="fa" hreflang="fa" data-title="ستاره متغیر" data-language-autonym="فارسی" data-language-local-name="Persies" class="interlanguage-link-target"><span>فارسی</span></a></li><li class="interlanguage-link interwiki-fi mw-list-item"><a href="https://fi.wikipedia.org/wiki/Muuttuva_t%C3%A4hti" title="Muuttuva tähti – Fins" lang="fi" hreflang="fi" data-title="Muuttuva tähti" data-language-autonym="Suomi" data-language-local-name="Fins" class="interlanguage-link-target"><span>Suomi</span></a></li><li class="interlanguage-link interwiki-fr mw-list-item"><a href="https://fr.wikipedia.org/wiki/%C3%89toile_variable" title="Étoile variable – Frans" lang="fr" hreflang="fr" data-title="Étoile variable" data-language-autonym="Français" data-language-local-name="Frans" class="interlanguage-link-target"><span>Français</span></a></li><li class="interlanguage-link interwiki-ga mw-list-item"><a href="https://ga.wikipedia.org/wiki/R%C3%A9alta_athraitheach" title="Réalta athraitheach – Iers" lang="ga" hreflang="ga" data-title="Réalta athraitheach" data-language-autonym="Gaeilge" data-language-local-name="Iers" class="interlanguage-link-target"><span>Gaeilge</span></a></li><li class="interlanguage-link interwiki-he mw-list-item"><a href="https://he.wikipedia.org/wiki/%D7%9B%D7%95%D7%9B%D7%91_%D7%9E%D7%A9%D7%AA%D7%A0%D7%94" title="כוכב משתנה – Hebreeus" lang="he" hreflang="he" data-title="כוכב משתנה" data-language-autonym="עברית" data-language-local-name="Hebreeus" class="interlanguage-link-target"><span>עברית</span></a></li><li class="interlanguage-link interwiki-hi mw-list-item"><a href="https://hi.wikipedia.org/wiki/%E0%A4%AA%E0%A4%B0%E0%A4%BF%E0%A4%B5%E0%A4%B0%E0%A5%8D%E0%A4%A4%E0%A5%80_%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE" title="परिवर्ती तारा – Hindi" lang="hi" hreflang="hi" data-title="परिवर्ती तारा" data-language-autonym="हिन्दी" data-language-local-name="Hindi" class="interlanguage-link-target"><span>हिन्दी</span></a></li><li class="interlanguage-link interwiki-hr mw-list-item"><a href="https://hr.wikipedia.org/wiki/Promjenljiva_zvijezda" title="Promjenljiva zvijezda – Kroaties" lang="hr" hreflang="hr" data-title="Promjenljiva zvijezda" data-language-autonym="Hrvatski" data-language-local-name="Kroaties" class="interlanguage-link-target"><span>Hrvatski</span></a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/V%C3%A1ltoz%C3%B3csillag" title="Változócsillag – Hongaars" lang="hu" hreflang="hu" data-title="Változócsillag" data-language-autonym="Magyar" data-language-local-name="Hongaars" class="interlanguage-link-target"><span>Magyar</span></a></li><li class="interlanguage-link interwiki-hy mw-list-item"><a href="https://hy.wikipedia.org/wiki/%D5%93%D5%B8%D6%83%D5%B8%D5%AD%D5%A1%D5%AF%D5%A1%D5%B6_%D5%A1%D5%BD%D5%BF%D5%B2%D5%A5%D6%80" title="Փոփոխական աստղեր – Armeens" lang="hy" hreflang="hy" data-title="Փոփոխական աստղեր" data-language-autonym="Հայերեն" data-language-local-name="Armeens" class="interlanguage-link-target"><span>Հայերեն</span></a></li><li class="interlanguage-link interwiki-ia mw-list-item"><a href="https://ia.wikipedia.org/wiki/Stella_variabile" title="Stella variabile – Interlingua" lang="ia" hreflang="ia" data-title="Stella variabile" data-language-autonym="Interlingua" data-language-local-name="Interlingua" class="interlanguage-link-target"><span>Interlingua</span></a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Bintang_variabel" title="Bintang variabel – Indonesies" lang="id" hreflang="id" data-title="Bintang variabel" data-language-autonym="Bahasa Indonesia" data-language-local-name="Indonesies" class="interlanguage-link-target"><span>Bahasa Indonesia</span></a></li><li class="interlanguage-link interwiki-io mw-list-item"><a href="https://io.wikipedia.org/wiki/Varianta_stelo" title="Varianta stelo – Ido" lang="io" hreflang="io" data-title="Varianta stelo" data-language-autonym="Ido" data-language-local-name="Ido" class="interlanguage-link-target"><span>Ido</span></a></li><li class="interlanguage-link interwiki-it mw-list-item"><a href="https://it.wikipedia.org/wiki/Stella_variabile" title="Stella variabile – Italiaans" lang="it" hreflang="it" data-title="Stella variabile" data-language-autonym="Italiano" data-language-local-name="Italiaans" class="interlanguage-link-target"><span>Italiano</span></a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/%E5%A4%89%E5%85%89%E6%98%9F" title="変光星 – Japannees" lang="ja" hreflang="ja" data-title="変光星" data-language-autonym="日本語" data-language-local-name="Japannees" class="interlanguage-link-target"><span>日本語</span></a></li><li class="interlanguage-link interwiki-kk mw-list-item"><a href="https://kk.wikipedia.org/wiki/%D0%90%D0%B9%D0%BD%D1%8B%D0%BC%D0%B0%D0%BB%D1%8B_%D0%B6%D2%B1%D0%BB%D0%B4%D1%8B%D0%B7" title="Айнымалы жұлдыз – Kazaks" lang="kk" hreflang="kk" data-title="Айнымалы жұлдыз" data-language-autonym="Қазақша" data-language-local-name="Kazaks" class="interlanguage-link-target"><span>Қазақша</span></a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/%EB%B3%80%EA%B4%91%EC%84%B1" title="변광성 – Koreaans" lang="ko" hreflang="ko" data-title="변광성" data-language-autonym="한국어" data-language-local-name="Koreaans" class="interlanguage-link-target"><span>한국어</span></a></li><li class="interlanguage-link interwiki-ky mw-list-item"><a href="https://ky.wikipedia.org/wiki/%D3%A8%D0%B7%D0%B3%D3%A9%D1%80%D0%BC%D3%A9_%D0%B6%D1%8B%D0%BB%D0%B4%D1%8B%D0%B7" title="Өзгөрмө жылдыз – Kirgisies" lang="ky" hreflang="ky" data-title="Өзгөрмө жылдыз" data-language-autonym="Кыргызча" data-language-local-name="Kirgisies" class="interlanguage-link-target"><span>Кыргызча</span></a></li><li class="interlanguage-link interwiki-lb mw-list-item"><a href="https://lb.wikipedia.org/wiki/Ver%C3%A4nnerleche_St%C3%A4r" title="Verännerleche Stär – Luxemburgs" lang="lb" hreflang="lb" data-title="Verännerleche Stär" data-language-autonym="Lëtzebuergesch" data-language-local-name="Luxemburgs" class="interlanguage-link-target"><span>Lëtzebuergesch</span></a></li><li class="interlanguage-link interwiki-lt mw-list-item"><a href="https://lt.wikipedia.org/wiki/Kintamoji_%C5%BEvaig%C5%BEd%C4%97" title="Kintamoji žvaigždė – Litaus" lang="lt" hreflang="lt" data-title="Kintamoji žvaigždė" data-language-autonym="Lietuvių" data-language-local-name="Litaus" class="interlanguage-link-target"><span>Lietuvių</span></a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%9F%D1%80%D0%BE%D0%BC%D0%B5%D0%BD%D0%BB%D0%B8%D0%B2%D0%B0_%D1%95%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Променлива ѕвезда – Masedonies" lang="mk" hreflang="mk" data-title="Променлива ѕвезда" data-language-autonym="Македонски" data-language-local-name="Masedonies" class="interlanguage-link-target"><span>Македонски</span></a></li><li class="interlanguage-link interwiki-ml mw-list-item"><a href="https://ml.wikipedia.org/wiki/%E0%B4%9A%E0%B4%B0%E0%B4%A8%E0%B4%95%E0%B5%8D%E0%B4%B7%E0%B4%A4%E0%B5%8D%E0%B4%B0%E0%B4%82" title="ചരനക്ഷത്രം – Malabaars" lang="ml" hreflang="ml" data-title="ചരനക്ഷത്രം" data-language-autonym="മലയാളം" data-language-local-name="Malabaars" class="interlanguage-link-target"><span>മലയാളം</span></a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Bintang_berubah" title="Bintang berubah – Maleis" lang="ms" hreflang="ms" data-title="Bintang berubah" data-language-autonym="Bahasa Melayu" data-language-local-name="Maleis" class="interlanguage-link-target"><span>Bahasa Melayu</span></a></li><li class="interlanguage-link interwiki-nl mw-list-item"><a href="https://nl.wikipedia.org/wiki/Veranderlijke_ster" title="Veranderlijke ster – Nederlands" lang="nl" hreflang="nl" data-title="Veranderlijke ster" data-language-autonym="Nederlands" data-language-local-name="Nederlands" class="interlanguage-link-target"><span>Nederlands</span></a></li><li class="interlanguage-link interwiki-nn mw-list-item"><a href="https://nn.wikipedia.org/wiki/Variabel_stjerne" title="Variabel stjerne – Nuwe Noors" lang="nn" hreflang="nn" data-title="Variabel stjerne" data-language-autonym="Norsk nynorsk" data-language-local-name="Nuwe Noors" class="interlanguage-link-target"><span>Norsk nynorsk</span></a></li><li class="interlanguage-link interwiki-no mw-list-item"><a href="https://no.wikipedia.org/wiki/Variabel_stjerne" title="Variabel stjerne – Boeknoors" lang="nb" hreflang="nb" data-title="Variabel stjerne" data-language-autonym="Norsk bokmål" data-language-local-name="Boeknoors" class="interlanguage-link-target"><span>Norsk bokmål</span></a></li><li class="interlanguage-link interwiki-nov mw-list-item"><a href="https://nov.wikipedia.org/wiki/Variabli_stele" title="Variabli stele – Novial" lang="nov" hreflang="nov" data-title="Variabli stele" data-language-autonym="Novial" data-language-local-name="Novial" class="interlanguage-link-target"><span>Novial</span></a></li><li class="interlanguage-link interwiki-oc mw-list-item"><a href="https://oc.wikipedia.org/wiki/Estela_variabla" title="Estela variabla – Oksitaans" lang="oc" hreflang="oc" data-title="Estela variabla" data-language-autonym="Occitan" data-language-local-name="Oksitaans" class="interlanguage-link-target"><span>Occitan</span></a></li><li class="interlanguage-link interwiki-pl mw-list-item"><a href="https://pl.wikipedia.org/wiki/Gwiazda_zmienna" title="Gwiazda zmienna – Pools" lang="pl" hreflang="pl" data-title="Gwiazda zmienna" data-language-autonym="Polski" data-language-local-name="Pools" class="interlanguage-link-target"><span>Polski</span></a></li><li class="interlanguage-link interwiki-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Estrela_vari%C3%A1vel" title="Estrela variável – Portugees" lang="pt" hreflang="pt" data-title="Estrela variável" data-language-autonym="Português" data-language-local-name="Portugees" class="interlanguage-link-target"><span>Português</span></a></li><li class="interlanguage-link interwiki-ro mw-list-item"><a href="https://ro.wikipedia.org/wiki/Stea_variabil%C4%83" title="Stea variabilă – Roemeens" lang="ro" hreflang="ro" data-title="Stea variabilă" data-language-autonym="Română" data-language-local-name="Roemeens" class="interlanguage-link-target"><span>Română</span></a></li><li class="interlanguage-link interwiki-ru badge-Q17437796 badge-featuredarticle mw-list-item" title="voorbladartikel"><a href="https://ru.wikipedia.org/wiki/%D0%9F%D0%B5%D1%80%D0%B5%D0%BC%D0%B5%D0%BD%D0%BD%D0%B0%D1%8F_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Переменная звезда – Russies" lang="ru" hreflang="ru" data-title="Переменная звезда" data-language-autonym="Русский" data-language-local-name="Russies" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-sh mw-list-item"><a href="https://sh.wikipedia.org/wiki/Promenljiva_zvezda" title="Promenljiva zvezda – Serwo-Kroaties" lang="sh" hreflang="sh" data-title="Promenljiva zvezda" data-language-autonym="Srpskohrvatski / српскохрватски" data-language-local-name="Serwo-Kroaties" class="interlanguage-link-target"><span>Srpskohrvatski / српскохрватски</span></a></li><li class="interlanguage-link interwiki-simple mw-list-item"><a href="https://simple.wikipedia.org/wiki/Variable_star" title="Variable star – Simple English" lang="en-simple" hreflang="en-simple" data-title="Variable star" data-language-autonym="Simple English" data-language-local-name="Simple English" class="interlanguage-link-target"><span>Simple English</span></a></li><li class="interlanguage-link interwiki-sk mw-list-item"><a href="https://sk.wikipedia.org/wiki/Premenn%C3%A1_hviezda" title="Premenná hviezda – Slowaaks" lang="sk" hreflang="sk" data-title="Premenná hviezda" data-language-autonym="Slovenčina" data-language-local-name="Slowaaks" class="interlanguage-link-target"><span>Slovenčina</span></a></li><li class="interlanguage-link interwiki-sl mw-list-item"><a href="https://sl.wikipedia.org/wiki/Spremenljivka_(zvezda)" title="Spremenljivka (zvezda) – Sloweens" lang="sl" hreflang="sl" data-title="Spremenljivka (zvezda)" data-language-autonym="Slovenščina" data-language-local-name="Sloweens" class="interlanguage-link-target"><span>Slovenščina</span></a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/%D0%9F%D1%80%D0%BE%D0%BC%D0%B5%D0%BD%D1%99%D0%B8%D0%B2%D0%B0_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Променљива звезда – Serwies" lang="sr" hreflang="sr" data-title="Променљива звезда" data-language-autonym="Српски / srpski" data-language-local-name="Serwies" class="interlanguage-link-target"><span>Српски / srpski</span></a></li><li class="interlanguage-link interwiki-sv badge-Q17437796 badge-featuredarticle mw-list-item" title="voorbladartikel"><a href="https://sv.wikipedia.org/wiki/Variabel_stj%C3%A4rna" title="Variabel stjärna – Sweeds" lang="sv" hreflang="sv" data-title="Variabel stjärna" data-language-autonym="Svenska" data-language-local-name="Sweeds" class="interlanguage-link-target"><span>Svenska</span></a></li><li class="interlanguage-link interwiki-sw mw-list-item"><a href="https://sw.wikipedia.org/wiki/Nyotabadilifu" title="Nyotabadilifu – Swahili" lang="sw" hreflang="sw" data-title="Nyotabadilifu" data-language-autonym="Kiswahili" data-language-local-name="Swahili" class="interlanguage-link-target"><span>Kiswahili</span></a></li><li class="interlanguage-link interwiki-ta mw-list-item"><a href="https://ta.wikipedia.org/wiki/%E0%AE%AE%E0%AE%BE%E0%AE%B1%E0%AF%81%E0%AE%AA%E0%AE%9F%E0%AF%81%E0%AE%AE%E0%AF%8D_%E0%AE%B5%E0%AE%BF%E0%AE%A3%E0%AF%8D%E0%AE%AE%E0%AF%80%E0%AE%A9%E0%AF%8D" title="மாறுபடும் விண்மீன் – Tamil" lang="ta" hreflang="ta" data-title="மாறுபடும் விண்மீன்" data-language-autonym="தமிழ்" data-language-local-name="Tamil" class="interlanguage-link-target"><span>தமிழ்</span></a></li><li class="interlanguage-link interwiki-th mw-list-item"><a href="https://th.wikipedia.org/wiki/%E0%B8%94%E0%B8%B2%E0%B8%A7%E0%B9%81%E0%B8%9B%E0%B8%A3%E0%B9%81%E0%B8%AA%E0%B8%87" title="ดาวแปรแสง – Thai" lang="th" hreflang="th" data-title="ดาวแปรแสง" data-language-autonym="ไทย" data-language-local-name="Thai" class="interlanguage-link-target"><span>ไทย</span></a></li><li class="interlanguage-link interwiki-tr mw-list-item"><a href="https://tr.wikipedia.org/wiki/De%C4%9Fi%C5%9Fen_y%C4%B1ld%C4%B1z" title="Değişen yıldız – Turks" lang="tr" hreflang="tr" data-title="Değişen yıldız" data-language-autonym="Türkçe" data-language-local-name="Turks" class="interlanguage-link-target"><span>Türkçe</span></a></li><li class="interlanguage-link interwiki-uk mw-list-item"><a href="https://uk.wikipedia.org/wiki/%D0%97%D0%BC%D1%96%D0%BD%D0%BD%D1%96_%D0%B7%D0%BE%D1%80%D1%96" title="Змінні зорі – Oekraïens" lang="uk" hreflang="uk" data-title="Змінні зорі" data-language-autonym="Українська" data-language-local-name="Oekraïens" class="interlanguage-link-target"><span>Українська</span></a></li><li class="interlanguage-link interwiki-uz mw-list-item"><a href="https://uz.wikipedia.org/wiki/O%CA%BBzgaruvchan_yulduzlar" title="Oʻzgaruvchan yulduzlar – Oezbeeks" lang="uz" hreflang="uz" data-title="Oʻzgaruvchan yulduzlar" data-language-autonym="Oʻzbekcha / ўзбекча" data-language-local-name="Oezbeeks" class="interlanguage-link-target"><span>Oʻzbekcha / ўзбекча</span></a></li><li class="interlanguage-link interwiki-vi mw-list-item"><a href="https://vi.wikipedia.org/wiki/Sao_bi%E1%BA%BFn_quang" title="Sao biến quang – Viëtnamees" lang="vi" hreflang="vi" data-title="Sao biến quang" data-language-autonym="Tiếng Việt" data-language-local-name="Viëtnamees" 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id="mw-content-subtitle"></div></div> <div id="mw-content-text" class="mw-body-content"><div class="mw-content-ltr mw-parser-output" lang="af" dir="ltr"><figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:New_View_of_the_Great_Nebula_in_Carina.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/New_View_of_the_Great_Nebula_in_Carina.jpg/300px-New_View_of_the_Great_Nebula_in_Carina.jpg" decoding="async" width="300" height="285" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/New_View_of_the_Great_Nebula_in_Carina.jpg/450px-New_View_of_the_Great_Nebula_in_Carina.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4c/New_View_of_the_Great_Nebula_in_Carina.jpg/600px-New_View_of_the_Great_Nebula_in_Carina.jpg 2x" data-file-width="1509" data-file-height="1434" /></a><figcaption>Die veranderlike ster Eta Carinae, wat in die Carina-newel lê.</figcaption></figure> <p>’n <a href="/wiki/Ster" title="Ster">Ster</a> word as ’n <b>veranderlike ster</b> of <b>wisselster</b> geklassifiseer wanneer sy <a href="/wiki/Skynbare_magnitude" class="mw-redirect" title="Skynbare magnitude">skynbare helderheid</a>, soos van die <a href="/wiki/Aarde" title="Aarde">Aarde</a> af gesien, wisselvallig is. Soms is dit vanweë die werklike helderheid van die ster en ander kere vanweë die hoeveelheid lig wat versper word voor dit die Aarde bereik. Baie sterre, waarskynlik die meeste, het die een of ander vorm van wisseling in helderheid: die lig van ons <a href="/wiki/Son" title="Son">Son</a> wissel byvoorbeeld met sowat 0,1% oor ’n siklus van elf jaar.<sup id="cite_ref-1" class="reference"><a href="#cite_note-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> </p><p>Veranderlike sterre, ook net <b>veranderlikes</b> genoem, word as twee soorte geklassifiseer: </p> <ul><li>Intrinsieke of inherente veranderlikes, waarvan die helderheid in werklikheid wissel, byvoorbeeld omdat die ster met tussenposes uitsit en krimp;</li> <li>Ekstrinsieke of uiterlike veranderlikes, waarvan die oënskynlike wisseling in helderheid veroorsaak word deur die hoeveelheid lig wat die Aarde bereik, bv. wanneer die ster ’n metgesel het wat daarom wentel en sodoende lig versper.</li></ul> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Ontdekking">Ontdekking</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=1" title="Wysig afdeling: Ontdekking" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=1" title="Edit section's source code: Ontdekking"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Eclipsing_binary_star_animation_2.gif" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/0/07/Eclipsing_binary_star_animation_2.gif" decoding="async" width="160" height="120" class="mw-file-element" data-file-width="160" data-file-height="120" /></a><figcaption>’n Verduisterende dubbelster, soos Algol. Onder die sterre kan die ligkurwe gesien word wat hulle vorm.</figcaption></figure> <p>’n <a href="/wiki/Antieke_Egipte" title="Antieke Egipte">Antieke Egiptiese</a> kalender van gelukkige en ongelukkige dae wat sowat 3 200 jaar gelede saamgestel is, is dalk die oudste bewaarde historiese bewys van die ontdekking van ’n veranderlike ster, die <a href="/wiki/Verduisterende_dubbelster" class="mw-redirect" title="Verduisterende dubbelster">verduisterende dubbelster</a> <a href="/wiki/Algol" title="Algol">Algol</a>.<sup id="cite_ref-2" class="reference"><a href="#cite_note-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-3" class="reference"><a href="#cite_note-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> </p><p>Onder moderne sterrekundiges was Johannes Holwarda in <a href="/wiki/1638" title="1638">1638</a> die eerste wat ’n veranderlike ster geïdentifiseer het toe hy opgemerk het dat <a href="/wiki/Omicron_Ceti" class="mw-redirect" title="Omicron Ceti">Omicron Ceti</a> (later Mira genoem) pulseer met ’n periode van 11 maande; die ster is vantevore (in 1596) deur David Fabricius as ’n <a href="/wiki/Nova" title="Nova">nova</a> beskryf. Hierdie ontdekking, tesame met <a href="/wiki/Supernova" title="Supernova">supernovas</a> wat in 1572 en 1604 waargeneem is, het bewys die hemelruim is nie ewig onveranderlik soos wat <a href="/wiki/Aristoteles" title="Aristoteles">Aristoteles</a> en ander <a href="/wiki/Filosoof" class="mw-redirect" title="Filosoof">filosowe</a> geleer het nie. Die ontdekking van veranderlike sterre het dus bygedra tot die sterrekundige omwenteling van die 16de en vroeë 17de eeu. </p><p>Die tweede veranderlike ster wat as ’n verduisterende veranderlike beskryf is, is Algol, in 1669 deur Geminiano Montanari; John Goodricke het sy veranderlikheid in 1784 korrek verklaar. <a href="/wiki/Chi_Cygni" title="Chi Cygni">Chi Cygni</a> is in 1686 deur Gottfried Kirch geïdentifiseer en R Hydrae in 1704 deur Giovanni Maraldi. Teen 1786 was 10 veranderlike sterre bekend. John Goodricke het daarna <a href="/wiki/Delta_Cephei" title="Delta Cephei">Delta Cephei</a> en <a href="/wiki/Beta_Lyrae" title="Beta Lyrae">Beta Lyrae</a> ontdek. Die getal bekende veranderlike sterre het sedert 1850 geweldig toegeneem, veral ná 1890 toe dit moontlik geword het om veranderlike sterre deur middel van <a href="/wiki/Fotografie" title="Fotografie">fotografie</a> te identifiseer. </p><p>Die nuutste uitgawe van die <a href="/wiki/General_Catalogue_of_Variable_Stars" title="General Catalogue of Variable Stars">General Catalogue of Variable Stars</a><sup id="cite_ref-4" class="reference"><a href="#cite_note-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> (2008) lys meer as 46 000 veranderlike sterre in die <a href="/wiki/Melkweg" title="Melkweg">Melkweg</a>, sowel as 10 000 in ander <a href="/wiki/Sterrestelsel" title="Sterrestelsel">sterrestelsels</a> en meer as 10 000 "vermoedelike" veranderlikes. </p> <div class="mw-heading mw-heading2"><h2 id="Die_bespeuring_van_veranderlikheid">Die bespeuring van veranderlikheid</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=2" title="Wysig afdeling: Die bespeuring van veranderlikheid" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=2" title="Edit section's source code: Die bespeuring van veranderlikheid"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Die algemeenste soort veranderlikheid behels wisselings in helderheid, maar ander soorte veranderlikheid is ook moontlik, soos veranderings in die <a href="/wiki/Spektraallyn" title="Spektraallyn">spektrum</a>. Deur <a href="/wiki/Ligkurwe" title="Ligkurwe">ligkurwe-data</a> te kombineer met waargenome spektrale veranderings kan <a href="/wiki/Sterrekundige" class="mw-redirect" title="Sterrekundige">sterrekundiges</a> dikwels verduidelik hoekom ’n spesifieke ster veranderlik is. </p> <div class="mw-heading mw-heading3"><h3 id="Waarnemings">Waarnemings</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=3" title="Wysig afdeling: Waarnemings" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=3" title="Edit section's source code: Waarnemings"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Delta_Cephei_lightcurve.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/6/6c/Delta_Cephei_lightcurve.jpg/280px-Delta_Cephei_lightcurve.jpg" decoding="async" width="280" height="148" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/6c/Delta_Cephei_lightcurve.jpg/420px-Delta_Cephei_lightcurve.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/6c/Delta_Cephei_lightcurve.jpg/560px-Delta_Cephei_lightcurve.jpg 2x" data-file-width="720" data-file-height="381" /></a><figcaption>Die ligkurwe van Delta Cephei, wat saamgestel is uit die ligwisseling van die ster.</figcaption></figure> <p>Veranderlike sterre word gewoonlik ontleed met behulp van <a href="/w/index.php?title=Fotometrie&action=edit&redlink=1" class="new" title="Fotometrie (bladsy bestaan nie)">fotometrie</a> en <a href="/wiki/Spektroskopie" title="Spektroskopie">spektroskopie</a>. Deur die wisseling in helderheid te meet kan ’n <a href="/wiki/Ligkurwe" title="Ligkurwe">ligkurwe</a> saamgestel word. Vir gereelde veranderlikes kan die <a href="/wiki/Frekwensie" title="Frekwensie">periode</a> van veranderlikheid en die omvang daarvan bepaal word; by baie veranderlikes kan dié eienskappe egter mettertyd verskil, selfs van een periode tot die volgende. Die helderste dele in die ligkurwe word "maksimums" genoem en die dofste dele "minimums". </p><p>Sterrekundiges kan veranderlike sterre bestudeer deur hulle visueel met ander sterre in dieselfde <a href="/wiki/Teleskoop" title="Teleskoop">teleskopiese sigveld</a> te vergelyk waarvan die <a href="/wiki/Magnitude" title="Magnitude">magnitude</a> bekend en konstant is. Deur die veranderlike ster se magnitude te beraam en die tyd van waarneming aan te teken, kan ’n visuele ligkurwe saamgestel word. </p><p>Van die ligkurwe kan die volgende data afgelei word: </p> <ul><li>Is die ligwisseling reëlmatig, halfreëlmatig, onreëlmatig of uniek?</li> <li>Wat is die periode van die ligwisseling?</li> <li>Wat is die vorm van die ligkurwe (simmetries of nie, hoekig of veranderlik)? Het elke periode een of meer minimums?</li></ul> <p>Van die spektrum kan die volgende afgelei word: </p> <ul><li>Watter soort ster is dit: wat is sy temperatuur, ligsterkteklas (<a href="/wiki/Dwergster" title="Dwergster">dwergster</a>, <a href="/wiki/Reusester" title="Reusester">reusester</a>, <a href="/wiki/Superreus" title="Superreus">superreus</a>) ens.?</li> <li>Is dit ’n enkel- of <a href="/wiki/Dubbelster" title="Dubbelster">dubbelster</a>? (Die gesamentlike spektrum van ’n dubbelster kan elemente toon van die spektrums van albei sterre.)</li> <li>Verander die spektrum mettertyd (is dit soms kouer of warmer)?</li> <li>Wisselings in helderheid kan afhang van die deel van die spektrum wat waargeneem word (byvoorbeeld groot wisselings in sigbare lig, maar feitlik geen in die <a href="/wiki/Infrarooi" title="Infrarooi">infrarooi</a>).</li> <li>As die golflengtes van <a href="/wiki/Spektraallyn" title="Spektraallyn">spektraallyne</a> verander, kan dit dui op beweging, byvoorbeeld die periodieke uitsetting of inkrimping van die ster, of sy rotasie, of ’n uitdyende gaslaag (<a href="/wiki/Doppler-effek" title="Doppler-effek">Doppler-effek</a>).</li> <li>Sterk <a href="/wiki/Magneetveld" title="Magneetveld">magneetvelde</a> van die ster kan in die spektrum gesien word.</li> <li>Abnormale <a href="/wiki/Spektraallyn" title="Spektraallyn">emissie- of absorpsielyne</a> kan ’n aanduiding wees van ’n warm steratmosfeer, of van gasnewels wat die ster omring.</li></ul> <div class="mw-heading mw-heading3"><h3 id="Interpretasie_van_waarnemings">Interpretasie van waarnemings</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=4" title="Wysig afdeling: Interpretasie van waarnemings" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=4" title="Edit section's source code: Interpretasie van waarnemings"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Deur ligkurwes en spektraaldata te kombineer, kan dikwels ’n aanduiding gekry word van die veranderings wat in ’n veranderlike ster plaasvind. Bewyse van ’n pulserende ster kan byvoorbeeld gevind word in sy veranderende spektrum, aangesien sy oppervlak met tussenposes na en weg van ons beweeg, teen dieselfde frekwensie as die wisselende helderheid. </p><p>Sowat twee derdes van veranderlike sterre blyk pulserend te wees. In die 1930's het die sterrekundige Arthur Eddington bewys die wiskundige vergelykings wat die binnekant van ’n ster beskryf, kan lei tot onstabiliteit wat veroorsaak dat die ster pulseer. Die algemeenste soort onstabiliteit hou verband met skommelings in die mate van <a href="/wiki/Ioon" title="Ioon">ionisasie</a> in die buitenste <a href="/wiki/Konveksie" title="Konveksie">konveksielae</a> van die ster. </p><p>Veronderstel ’n ster is in die uitsettingsfase. Die buitenste lae sit uit, en dit veroorsaak dat hulle afkoel. Vanweë die afnemende temperatuur neem die mate van ionisasie ook af. Dit maak die gas meer uitsendend, en maak dit dus makliker vir die ster om sy energie uit te straal. Dit sal weer tot gevolg hê dat die ster begin krimp. Omdat die gas daardeur saamgepers word, word dit warmer en die mate van ionisasie neem weer toe. Dit maak die gas meer absorberend en straling word tydelik in die gas vasgevang. Dit verhit die gas nog meer, en dit lei daartoe dat dit weer uitsit. So word ’n siklus van uitsetting en inkrimping gehandhaaf. </p><p>Die pulserings van <a href="/wiki/Cephe%C3%AFed" title="Cepheïed">Cepheïede</a> word veroorsaak deur skommelings in die ionisasie van <a href="/wiki/Helium" title="Helium">helium</a> (van He<sup>++</sup> na He<sup>+</sup> en terug na He<sup>++</sup>). </p> <div class="mw-heading mw-heading2"><h2 id="Benaming_van_veranderlike_sterre">Benaming van veranderlike sterre</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=5" title="Wysig afdeling: Benaming van veranderlike sterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=5" title="Edit section's source code: Benaming van veranderlike sterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>In ’n gegewe <a href="/wiki/Sterrebeeld" title="Sterrebeeld">sterrebeeld</a> het die eerste veranderlikes wat ontdek is, voorvoegsels wat bestaan uit die letters R tot Z, gevolg deur die sterrebeeld se naam in <a href="/wiki/Genitief" title="Genitief">genitief</a>, byvoorbeeld R Andromedae. Die sterrekundige Friedrich W. Argelander het dié manier uitgedink om sterre name te gee en het die eerste veranderlike sonder ’n naam in ’n sterrebeeld die letter R vooraan gegee – dit was die eerste letter wat nie deur <a href="/wiki/Bayer-naam" title="Bayer-naam">Bayer</a> gebruik is nie. </p><p>Vir die volgende ontdekkings is die letters RR tot RZ, SS tot SZ ensovoorts tot by ZZ gebruik, byvoorbeeld RR Lyrae. Vir latere ontdekkings is die letters AA tot AZ, BB tot BZ ensovoorts tot QQ tot QZ gebruik (J is uitgelaat). Wanneer dié 334 kombinasies uitgeput is, word veranderlike sterre genommer in die volgorde van ontdekking – dit begin met die voorvoegsel V335. </p> <div class="mw-heading mw-heading2"><h2 id="Klassifikasie">Klassifikasie</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=6" title="Wysig afdeling: Klassifikasie" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=6" title="Edit section's source code: Klassifikasie"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Veranderlike sterre kan óf intrinsiek óf ekstrinsiek wees. </p> <ul><li><b>Intrinsieke veranderlikes</b> is sterre waar die veranderlikheid veroorsaak word deur veranderings in die fisiese eienskappe van die sterre self. Dié kategorie kan in drie subgroepe verdeel word: <ul><li>Pulserende veranderlikes is sterre waarvan die radius alternatiewelik uitsit en krimp as deel van hul natuurlike evolusie.</li> <li>Uitbarstende veranderlikes is sterre wat uitbarstings, soos die massa-uitwerping van materie, op hul oppervlak ondervind.</li> <li>Kataklismiese veranderlikes is sterre wat die een of ander kataklismiese of katastrofale verandering ondergaan, soos <a href="/wiki/Nova" title="Nova">novas</a> en <a href="/wiki/Supernova" title="Supernova">supernovas</a>.</li></ul></li></ul> <ul><li><b>Ekstrinsieke veranderlikes</b> is sterre waar die ligwisseling veroorsaak word deur eksterne faktore soos rotasie of verduisterings.</li></ul> <p>Daar is twee hoofgroepe: </p> <ul><li><ul><li>Roterende veranderlikes is sterre waarvan die ligwisselings veroorsaak word deur verskynsels wat met hul rotasie verband hou. Voorbeelde is sterre met uiters groot <a href="/wiki/Sonvlek" title="Sonvlek">sonvlekke</a>, wat hul helderheid beïnvloed, of sterre met ’n vinnige rotasiesnelheid wat veroorsaak dat hulle ovaalvormig is.</li> <li>Verduisterende veranderlikes is <a href="/wiki/Dubbelster" title="Dubbelster">dubbelsterre</a> wat, soos van die Aarde af gesien, mekaar se lig verduister terwyl hulle om mekaar wentel.</li></ul></li></ul> <p>Hierdie subgroepe word verder verdeel in spesifieke soorte veranderlike sterre wat gewoonlik genoem word na hul prototipe-ster. So word ’n sekere tipe dwerg-nova U Geminorum-veranderlikes genoem – na die eerste ster wat in dié groep erken is, U Geminorum. </p> <div class="mw-heading mw-heading2"><h2 id="Intrinsieke_veranderlike_sterre">Intrinsieke veranderlike sterre</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=7" title="Wysig afdeling: Intrinsieke veranderlike sterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=7" title="Edit section's source code: Intrinsieke veranderlike sterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="mw-heading mw-heading3"><h3 id="Pulserende_veranderlikes">Pulserende veranderlikes</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=8" title="Wysig afdeling: Pulserende veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=8" title="Edit section's source code: Pulserende veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:HR-vartype_af.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c2/HR-vartype_af.svg/300px-HR-vartype_af.svg.png" decoding="async" width="300" height="343" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c2/HR-vartype_af.svg/450px-HR-vartype_af.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c2/HR-vartype_af.svg/600px-HR-vartype_af.svg.png 2x" data-file-width="700" data-file-height="800" /></a><figcaption>Veranderlike sterre op die HR-diagram.</figcaption></figure> <p>Pulserende sterre sit uit en krimp, en dit beïnvloed hul helderheid en spektrum.<sup id="cite_ref-asteroseismology_5-0" class="reference"><a href="#cite_note-asteroseismology-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-pulsating_7-0" class="reference"><a href="#cite_note-pulsating-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> Hulle word gewoonlik in twee groepe verdeel: radiale veranderlikes, waar die hele ster uitsit en krimp; en nieradiaal, waar ’n deel van die ster uitsit en ’n ander deel krimp. </p><p>Na gelang van die soort pulsering en die ligging daarvan in die ster, is daar ’n natuurlike frekwensie wat die periode van die ster bepaal. Pulserende sterre het soms ’n enkele, goed gedefinieerde periode, maar soms wissel die periodes en ’n patroon moet dan vasgestel word. Sommige sterre het glad nie ’n bepaalde frekwensie nie en pulserings vind lukraak plaas (dit word stogasties genoem). Die bestudering van sterre met behulp van hul pulserings word <a href="/wiki/Asteroseismologie" title="Asteroseismologie">asteroseismologie</a> genoem. </p><p>Pulserings in ’n ster word veroorsaak deur ’n ongebalanseerde dryfkrag met ’n teenwerkende krag. In pulserende veranderlikes is die dryfkrag die inherente energie van die ster, gewoonlik vanweë <a href="/wiki/Kernfusie" title="Kernfusie">kernfusie</a>, maar soms is dit opgegaarde energie, wat altyd probeer om uitwaarts te versprei. Op sekere plekke op die <a href="/wiki/Hertzsprung-Russell-diagram" title="Hertzsprung-Russell-diagram">Hertzsprung-Russell-diagram</a> (regs), wat afhang van sekere kombinasies van temperature, groottes en innerlike chemie, wissel die uitwaartse vloei van energie deur straling baie na gelang van die digtheid of temperatuur van die materie wat betrokke is. Wanneer die absorpsie van ’n laag in die ster hoog is, sit dié laag uit, en wanneer die afname in temperatuur of druk veroorsaak dat die absorpsie afneem, is daar ’n teenwerkende krag – en dit veroorsaak gereelde pulse. Dit gebeur gewoonlik wanneer die <a href="/wiki/Ioon" title="Ioon">ionisasievlak</a> van die materie verander. </p><p>Vir pulse om sigbaar te wees, moet dié wisselwerking op ’n sekere diepte in die ster plaasvind. As dit te diep is, sal die pulse nie op die oppervlak sigbaar wees nie, en as dit te na aan die oppervlak is, sal daar dalk nie ’n teenwerkende krag wees om pulserings te veroorsaak nie. </p> <div class="mw-heading mw-heading4"><h4 id="Cepheïede_en_Cepheïed-agtige_veranderlikes"><span id="Cephe.C3.AFede_en_Cephe.C3.AFed-agtige_veranderlikes"></span>Cepheïede en Cepheïed-agtige veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=9" title="Wysig afdeling: Cepheïede en Cepheïed-agtige veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=9" title="Edit section's source code: Cepheïede en Cepheïed-agtige veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dd><i>Hoofartikel: <a href="/wiki/Cephe%C3%AFed" title="Cepheïed">Cepheïed</a></i></dd></dl> <p>Cepheïede word onderverdeel in verskeie subklasse volgens hul massa, ouderdom en evolusiegeskiedenis, onder meer in klassieke, tipe II- en dwerg-Cepheïede (Delta Scuti-veranderlikes). Elke subklas het ’n vasgestelde verhouding tussen periode en <a href="/wiki/Absolute_magnitude" title="Absolute magnitude">absolute magnitude</a>, sowel as tussen periode en die gemiddelde digtheid van die ster. Eersgenoemde verhouding vir Delta-Cepheïede is die eerste keer aan die begin van die <a href="/wiki/20ste_eeu" title="20ste eeu">20ste eeu</a> deur Henrietta Swan Leavitt vasgestel, en dit maak dié helder Cepheïede ’n baie belangrike instrument in die bepaling van afstande na <a href="/wiki/Sterrestelsel" title="Sterrestelsel">sterrestelsels</a> binne en buite die <a href="/wiki/Plaaslike_Groep" title="Plaaslike Groep">Plaaslike Groep</a>. <a href="/wiki/Edwin_Hubble" title="Edwin Hubble">Edwin Hubble</a> het dié metode gebruik om te bewys sogenaamde "spiraalnewels" is in werklikheid verafgeleë sterrestelsels. </p><p>Let wel: Cepheïede verwys net na sterre soos <a href="/wiki/Delta_Cephei" title="Delta Cephei">Delta Cephei</a>; ’n heel aparte klas veranderlikes is genoem na <a href="/wiki/Beta_Cephei" title="Beta Cephei">Beta Cephei</a>. </p> <dl><dt>Klassieke Cepheïed-veranderlikes</dt></dl> <p>Klassieke Cepheïede (of Delta Cephei-veranderlikes) is <a href="/wiki/Metaal_(astronomie)#Populasie_I,_II_en_III" class="mw-redirect" title="Metaal (astronomie)">populasie I-sterre</a> (jong, helder sterre met ’n groot massa). Hulle is <a href="/wiki/Superreus" title="Superreus">geelsuperreuse</a> waarvan die pulserings met gereelde periodes plaasvind wat wissel van dae tot maande. Edward Pigott het op 10 September 1784 die veranderlike <a href="/wiki/Eta_Aquilae" title="Eta Aquilae">Eta Aquilae</a> ontdek wat die eerste bekende Cepheïed-veranderlike was. Die klassieke Cepheïede is egter genoem na Delta Cephei, wat ’n paar maande later deur John Goodricke as ’n veranderlike uitgeken is. </p> <dl><dt>Tipe II-Cepheïede</dt></dl> <p>Tipe II-Cepheïede (historiese naam W Virginis-sterre) het uiters gereelde pulse en ’n helderheidsverhouding wat baie ooreenstem met dié van Delta-Cepheïede. Hulle is aanvanklik met laasgenoemde kategorie verwar. Tipe II-Cepheïede is van <a href="/wiki/Metaal_(astronomie)#Populasie_I,_II_en_III" class="mw-redirect" title="Metaal (astronomie)">populasie II</a>, ouer sterre as die tipe I-Cepheïede. Hul <a href="/wiki/Metaal_(astronomie)" class="mw-redirect" title="Metaal (astronomie)">metaalinhoud</a> en helderheid is effens laer en hul massa baie laer. Hulle het ’n effens afwykende periode-helderheidsverhouding en dit is dus belangrik om in gedagte te hou watter tipe ster waargeneem word. </p> <dl><dt>RR Lyrae-veranderlikes</dt> <dd><i>Hoofartikel: <a href="/wiki/RR_Lyrae-ster" title="RR Lyrae-ster">RR Lyrae-ster</a></i></dd></dl> <p>Hierdie sterre is baie soos Cepheïede, maar is nie so helder nie en het korter periodes. Hulle is ouer as tipe I-Cepheïede en behoort tot populasie II, maar hul massa is kleiner as dié van tipe II-Cepheïede. Omdat hulle dikwels in <a href="/wiki/Bolswerm" class="mw-redirect" title="Bolswerm">bolswerms</a> voorkom, word hulle soms "swerm-Cepheïede" genoem. Hulle het ook ’n goed vasgestelde periode-helderheidsverhouding en is dus ook nuttig om afstande mee te bepaal. Hierdie <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">spektraaltipe A-sterre</a> wissel van helderheid met sowat 0,2 tot 2 magnitude (’n verandering van 20% tot meer as 500%) oor ’n periode van ’n paar uur tot ’n dag of langer. </p> <dl><dt>Delta Scuti-veranderlikes</dt></dl> <p>Delta Scuti (δ Sct)-veranderlikes is soortgelyk aan Cepheïede, maar baie flouer en hul periodes is baie korter. Hulle is voorheen "dwerg-Cepheïede" genoem. Hulle het soms baie oorvleuelende periodes, wat saam ’n baie ingewikkelde ligkurwe vorm. ’n Tipiese δ Scuti-ster het ’n omvang van 0,003 tot 0,9 magnitude ('n wisseling van 0,3% tot sowat 130%) en hul periodes is 0,01 tot 0,2 dae. Hulle is gewoonlik van <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">spektraaltipe A0</a> en <a href="/wiki/Sterreklassifikasie#Klas_F" title="Sterreklassifikasie">F5</a>. </p> <dl><dt>SX Phoenicis-veranderlikes</dt></dl> <p>Hierdie sterre, van spektraaltipe A2 tot F5 en soortgelyk aan δ Scuti-veranderlikes, word hoofsaaklik in bolswerms aangetref. Hulle toon wisselings in helderheid van sowat 0,7 magnitude (sowat 100%) elke een tot twee uur. </p> <dl><dt>Kortperiode-Ap-veranderlikes</dt></dl> <p>Hierdie sterre van spektraaltipe A of soms F0, is ’n subklas van die δ Scuti-veranderlikes in die <a href="/wiki/Hoofreeks" title="Hoofreeks">hoofreeks</a>. Hulle het uiters vinnige wisselings in helderheid van ’n paar duisendstes van ’n magnitude, met periodes van ’n paar minute. </p> <div class="mw-heading mw-heading4"><h4 id="Langperiode-veranderlikes">Langperiode-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=10" title="Wysig afdeling: Langperiode-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=10" title="Edit section's source code: Langperiode-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Die langperiode-veranderlikes is pulserende, koel reusesterre regs bo op die <a href="/wiki/HR-diagram" class="mw-redirect" title="HR-diagram">HR-diagram</a>. Hulle het periodes van ’n paar weke tot ’n paar jaar en is soms onreëlmatig. Hulle is van spektraaltipe F en rooier, maar die meeste is <a href="/wiki/Rooireus" title="Rooireus">rooi-</a> en <a href="/wiki/Asimptotiese_reus" class="mw-redirect" title="Asimptotiese reus">asimptotiese reuse</a>, dus spektraaltipe M, S of C. Hulle is gewoonlik dieporanje of rooi. </p><p>Die volgende klasse val in dié kategorie: Mira-veranderlikes, sterre met lang, redelik reëlmatige, periodes in die omgewing van 80 tot 1 000 dae, en groot ligwisselings, van 2,5 tot 11 magnitude; halfreëlmatige veranderlikes waarvan die periodes met dié van Mira-veranderlikes ooreenstem maar met ’n laer omvang en dikwels onreëlmatighede wat dit moeilik maak om die periode te bepaal; en stadige onreëlmatige veranderlikes wat met laasgenoemde groep ooreenstem, maar periodes het wat nie bepaal kan word nie vanweë die onreëlmatigheid van die ligwisselings. </p> <dl><dt>Mira-veranderlikes</dt> <dd><i>Hoofartikel: <a href="/wiki/Mira-veranderlike" title="Mira-veranderlike">Mira-veranderlike</a></i></dd></dl> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Mira_1997.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/e8/Mira_1997.jpg/240px-Mira_1997.jpg" decoding="async" width="240" height="240" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/e8/Mira_1997.jpg/360px-Mira_1997.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/e8/Mira_1997.jpg/480px-Mira_1997.jpg 2x" data-file-width="502" data-file-height="502" /></a><figcaption>Die ster Mira, ook bekend as Omicron Ceti.</figcaption></figure> <p>Mira-veranderlikes is asimptotiese <a href="/wiki/Rooireus" title="Rooireus">rooireuse</a>. Oor periodes van baie maande wissel hul helderheid met 2,5 tot 11 magnitude, tussen 6 en 30 000 keer hul oorspronklike magnitude. <a href="/wiki/Mira" title="Mira">Mira</a> self, ook bekend as Omicron Ceti (ο Cet), se helderheid wissel van 2de magnitude tot so flou as 10de magnitude, met ’n periode van rofweg 332 dae. Die baie groot sigbare omvang is hoofsaaklik vanweë die verskuiwing van energie-uitset tussen sigbare lig en <a href="/wiki/Infrarooi" title="Infrarooi">infrarooi</a> namate die temperatuur van die ster verander. In ’n paar gevalle toon Mira-veranderlikes oor ’n paar dekades ’n dramatiese wisseling in periodes. Dit hou waarskynlik verband met die termiese pulseringsiklus van die meeste sterre op die <a href="/wiki/Asimptotiese_reusetak" title="Asimptotiese reusetak">asimptotiese reusetak</a>. </p> <dl><dt>Halfreëlmatige veranderlikes</dt></dl> <p>Hulle is rooireuse of rooisuperreuse en toon soms ’n bepaalde periode, maar het meestal minder spesifieke wisselings. ’n Bekende voorbeeld is <a href="/wiki/Betelgeuse" title="Betelgeuse">Betelgeuse</a>, wat wissel van sowat magnitudes 0,2 tot 1,2 (’n faktorverandering van 2,5 in helderheid). Minstens sommige van die halfreëlmatige veranderlikes is na verwant aan Mira-veranderlikes en die enigste verskille is in die harmonie van die pulserings. </p> <div class="mw-heading mw-heading4"><h4 id="Beta_Cephei-veranderlikes">Beta Cephei-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=11" title="Wysig afdeling: Beta Cephei-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=11" title="Edit section's source code: Beta Cephei-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Beta Cephei- of β Cep-veranderlikes ondergaan kortperiode-pulserings van 0,1 tot 0,6 dae met ’n omvang van 0,01 tot 0,3 magnitude (’n verandering van 1% tot 30% in helderheid). Baie sterre in dié klas het veelvuldige pulseringsperiodes. Hulle is hoofreekssterre met massas van tussen 7 en 20 <a href="/wiki/Sonmassa" title="Sonmassa">sonmassas</a>. Die prototipe van dié sterre, <a href="/wiki/Beta_Cephei" title="Beta Cephei">Beta Cephei</a>, toon wisselings van tussen 3,16 en 3,27 in magnitude in ’n periode van 4,57 uur. </p><p>Hierdie sterre moenie verwar word met <a href="/wiki/Cephe%C3%AFed" title="Cepheïed">Cepheïede</a>, wat na die ster <a href="/wiki/Delta_Cephei" title="Delta Cephei">Delta Cephei</a> genoem is, nie. </p> <div class="mw-heading mw-heading4"><h4 id="Stadig_pulserende_B-sterre">Stadig pulserende B-sterre</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=12" title="Wysig afdeling: Stadig pulserende B-sterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=12" title="Edit section's source code: Stadig pulserende B-sterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Stadig pulserende B-sterre (<a href="/wiki/Asimptotiese_reusetak" title="Asimptotiese reusetak">ART-sterre</a>) is warm <a href="/wiki/Hoofreeks" title="Hoofreeks">hoofreekssterre</a> wat effens dowwer is as die Beta Cephei-sterre, met langer periodes en groter wisselings.<sup id="cite_ref-spb_8-0" class="reference"><a href="#cite_note-spb-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> Hulle was vroeër bekend as "53 Persei-veranderlikes". Hulle wissel van <a href="/wiki/Sterreklassifikasie#Klas_B" title="Sterreklassifikasie">spektraaltipe B2 tot B9</a> (met ’n massa van 3 tot 9 keer dié van die Son) en pulseer met periodes van tussen ’n halwe dag tot vyf dae,<sup id="cite_ref-AAVSO_9-0" class="reference"><a href="#cite_note-AAVSO-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> hoewel die meeste sterre van dié klas veelvuldige periodes het.<sup id="cite_ref-Waelkens93_10-0" class="reference"><a href="#cite_note-Waelkens93-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> Hulle toon veranderlikheid in beide hul helderheid en <a href="/wiki/Spektraallyn" title="Spektraallyn">spektraallynprofiel</a>. Die wisselings in magnitude is gewoonlik kleiner as 0,1,<sup id="cite_ref-AAVSO_9-1" class="reference"><a href="#cite_note-AAVSO-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> en dit is dus in die meeste gevalle moeilik om die veranderlikheid met die blote oog waar te neem. Hul veranderlikheid is ook makliker om in die <a href="/wiki/Ultraviolet" title="Ultraviolet">ultravioletspektrum</a> te sien as in sigbare lig. </p><p>Dié sterre se pulserings is nieradiaal, wat beteken hulle wissel in vorm eerder as volume; verskillende dele van die ster sit uit en krimp tegelykertyd.<sup id="cite_ref-Percy_11-0" class="reference"><a href="#cite_note-Percy-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> </p><p>Hulle is die eerste keer in 1985 deur die sterrekundiges Christoffel Waelkens en Fredy Rufener as ’n groep uitgeken terwyl die twee sterrekundiges veranderlikheid in warm blousterre ondersoek het. Verbeterings in fotometrie het dit moontlik gemaak om klein ligwisselings makliker waar te neem, en hulle het bevind ’n groot persentasie van warm sterre was intrinsiek veranderlik. Hulle het dié sterre 53 Persei-sterre genoem, na die prototipe, 53 Persei.<sup id="cite_ref-Waelkens85_12-0" class="reference"><a href="#cite_note-Waelkens85-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup> Teen 1993 was tien van hulle reeds ontdek, maar Waelkens was onseker of die prototipe werklik ’n lid was en het voorgestel die klas word "stadig pulserende sterre" (SPS'e) genoem.<sup id="cite_ref-Waelkens93_10-1" class="reference"><a href="#cite_note-Waelkens93-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> Teen 2007 was 51 SPS'e al geïdentifiseer, met nog 65 moontlike SPS'e. Ses sterre – Iota Herculis, 53 Piscium, Nu Eridani, Gamma Pegasi, HD 13745 (V354 Persei) en 53 Arietis – toon beide Beta Cephei- en SPS-veranderlikheid.<sup id="cite_ref-decat07_13-0" class="reference"><a href="#cite_note-decat07-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading4"><h4 id="PV_Telescopii-veranderlikes">PV Telescopii-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=13" title="Wysig afdeling: PV Telescopii-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=13" title="Edit section's source code: PV Telescopii-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Sterre in dié klas is tipe Bp-superreuse met ’n periode van 0,1 tot 1 dag en ’n omvang van gemiddeld 0,1 magnitude. Hul spektra is uitsonderlik omdat hulle swak <a href="/wiki/Waterstof" title="Waterstof">waterstoflyne</a> het, maar ekstra sterk <a href="/wiki/Koolstof" title="Koolstof">koolstof-</a> en <a href="/wiki/Helium" title="Helium">heliumlyne</a>.<sup id="cite_ref-ibvs5817_14-0" class="reference"><a href="#cite_note-ibvs5817-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup> In dié opsig verskil hulle dus van ander B-tipe-sterre. Die prototipe vir dié groep is <a href="/wiki/HD_168476" class="mw-redirect" title="HD 168476">HD 168476</a>, ook bekend as PV Telescopii, wat klein maar ingewikkelde wisselings in helderheid en <a href="/wiki/Radiale_snelheid" title="Radiale snelheid">radiale snelheid</a> ondergaan.<sup id="cite_ref-15" class="reference"><a href="#cite_note-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup> </p><p>PV Telescopii-veranderlikes word in drie subgroepe verdeel volgens hul spektraaltipe: tipe I bestaan uit laat B- en A-sterre, tipe II uit O- en vroeë B-sterre en tipe III uit F- en G-sterre. Laasgenoemde groep is altyd koolstofryk en waterstof-arm, terwyl tipe I en II nie noodwendig uitermate baie koolstof bevat nie. Die pulserings van die warm tipes is vinniger as dié van die koeler sterre.<sup id="cite_ref-AAVSO_9-2" class="reference"><a href="#cite_note-AAVSO-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading4"><h4 id="RV_Tauri-veranderlikes">RV Tauri-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=14" title="Wysig afdeling: RV Tauri-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=14" title="Edit section's source code: RV Tauri-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Hulle is geelsuperreuse (eintlik post-ART-sterre met ’n lae massa wat in die heel helderste stadium van hul bestaan is). Hulle het afwisselende diep en vlak minimums. Hulle het gewoonlik ’n periode van 30 tot 100 dae en ’n omvang van 3 tot 4 magnitude. Daar kan ook langtermynwisselings oor tydperke van verskeie jare voorkom. Hulle is op hul helderste van <a href="/wiki/Sterreklassifikasie#Klas_F" title="Sterreklassifikasie">spektraaltipe F</a> of <a href="/wiki/Sterreklassifikasie#Klas_G" title="Sterreklassifikasie">spektraaltipe G</a> en op hul dofste van <a href="/wiki/Sterreklassifikasie#Klas_K" title="Sterreklassifikasie">spektraaltipe K</a> of <a href="/wiki/Sterreklassifikasie#Klas_M" title="Sterreklassifikasie">spektraaltipe M</a>. Hulle lê naby die <a href="/wiki/Onstabiele_strook" title="Onstabiele strook">onstabiele strook</a> op die <a href="/wiki/HR-diagram" class="mw-redirect" title="HR-diagram">HR-diagram</a>; hulle is koeler as tipe I- en helderder as tipe II-Cepheïede. Hul pulserings word deur dieselfde basiese meganisme veroorsaak wat met heliumabsorpsie verband hou, maar hulle is in ’n ander fase van hul bestaan. </p> <div class="mw-heading mw-heading4"><h4 id="Alpha_Cygni-veranderlikes">Alpha Cygni-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=15" title="Wysig afdeling: Alpha Cygni-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=15" title="Edit section's source code: Alpha Cygni-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Hertzsprung-Russel_StarData_af.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/91/Hertzsprung-Russel_StarData_af.jpg/350px-Hertzsprung-Russel_StarData_af.jpg" decoding="async" width="350" height="354" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/91/Hertzsprung-Russel_StarData_af.jpg/525px-Hertzsprung-Russel_StarData_af.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/91/Hertzsprung-Russel_StarData_af.jpg/700px-Hertzsprung-Russel_StarData_af.jpg 2x" data-file-width="2662" data-file-height="2690" /></a><figcaption>Deneb se plek bo in die middel van die <a href="/wiki/HR-diagram" class="mw-redirect" title="HR-diagram">HR-diagram</a>.</figcaption></figure> <p>Alpha Cygni- of α Cyg-veranderlikes is nieradiale pulserende superreuse van <a href="/wiki/Sterreklassifikasie#Klas_B" title="Sterreklassifikasie">spektraaltipe B<sub>ep</sub></a> tot <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">spektraaltipe A<sub>ep</sub>Ia</a>. Hul periode wissel van verskeie dae tot weke, en die omvang van hul ligwisseling is sowat 0,1 magnitude. Die veranderings in helderheid, wat dikwels onreëlmatig voorkom, word veroorsaak deur baie skommelings met periodes wat na aan mekaar is. Die ster <a href="/wiki/Deneb" title="Deneb">Deneb</a> (Alpha Cygni), in die <a href="/wiki/Sterrebeeld" title="Sterrebeeld">sterrebeeld</a> <a href="/wiki/Swaan_(sterrebeeld)" title="Swaan (sterrebeeld)">Swaan</a>, is die prototipe van dié klas. </p> <div class="mw-heading mw-heading4"><h4 id="Gamma_Doradus-veranderlikes">Gamma Doradus-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=16" title="Wysig afdeling: Gamma Doradus-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=16" title="Edit section's source code: Gamma Doradus-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Gamma Doradus- of γ Dor-veranderlikes is nieradiale pulserende hoofreekssterre van <a href="/wiki/Sterreklassifikasie#Klas_F" title="Sterreklassifikasie">spektraaltipe F</a> tot <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">laat A</a>. Hul periodes is sowat ’n dag en die omvang van hul verandering gewoonlik sowat 0,1 magnitude. Dit is ’n relatief nuwe klas veranderlike sterre wat maar in die tweede helfte van die 1990's geïdentifiseer is, en besonderhede van die oorsaak van hul veranderlikheid word nog bestudeer. Die prototipe is Gamma Doradus. </p> <div class="mw-heading mw-heading4"><h4 id="Pulserende_witdwerge">Pulserende witdwerge</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=17" title="Wysig afdeling: Pulserende witdwerge" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=17" title="Edit section's source code: Pulserende witdwerge"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Hierdie nieradiale pulserende sterre het kort periodes van honderde tot duisende sekondes met baie klein ligwisselings van 0,001 tot 0,2 magnitude. Bekende voorbeelde van pulserende <a href="/wiki/Witdwerg" title="Witdwerg">witdwerge</a> (of pre-witdwerge) sluit die DAV- of ZZ Ceti-sterre in, met waterstofoorheersende atmosfere en van <a href="/wiki/Sterreklassifikasie#Witdwerg-klassifikasies" title="Sterreklassifikasie">spektraaltipe DA</a>;<sup id="cite_ref-physrev_16-0" class="reference"><a href="#cite_note-physrev-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup> DBV- of V777 Her-sterre, met heliumoorheersende atmosfere en van <a href="/wiki/Sterreklassifikasie#Witdwerg-klassifikasies" title="Sterreklassifikasie">spektraaltipe DB</a>;<sup id="cite_ref-wden_17-0" class="reference"><a href="#cite_note-wden-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> en GW Vir-sterre, met atmosfere wat deur helium, <a href="/wiki/Koolstof" title="Koolstof">koolstof</a> en <a href="/wiki/Suurstof" title="Suurstof">suurstof</a> oorheers word. GW Vir-sterre kan onderverdeel word in DOV- en PNNV-sterre.<sup id="cite_ref-quirion_18-0" class="reference"><a href="#cite_note-quirion-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-19" class="reference"><a href="#cite_note-19"><span class="cite-bracket">[</span>19<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading4"><h4 id="Sonagtige_skommelings">Sonagtige skommelings</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=18" title="Wysig afdeling: Sonagtige skommelings" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=18" title="Edit section's source code: Sonagtige skommelings"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Sun920607.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Sun920607.jpg/200px-Sun920607.jpg" decoding="async" width="200" height="199" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Sun920607.jpg/300px-Sun920607.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Sun920607.jpg/400px-Sun920607.jpg 2x" data-file-width="466" data-file-height="463" /></a><figcaption>Die son se ligskommelings word veroorsaak deur konveksie in sy buitenste lae.</figcaption></figure> <p>Die <a href="/wiki/Son" title="Son">son</a> ondervind helderheidskommelings met ’n lae omvang in ’n groot aantal modusse met ’n periode van sowat 5 minute. Dié skommelings is stogasties en word veroorsaak deur <a href="/wiki/Konveksie" title="Konveksie">konveksie</a> in sy buitenste lae. Die term "sonagtige skommelings" word gebruik om skommelings in ander sterre te beskryf wat op dieselfde manier opgewek word en dit is een van die hoofnavorsingsvelde van asteroseismologie. </p> <div class="mw-heading mw-heading3"><h3 id="Uitbarstende_veranderlikes">Uitbarstende veranderlikes</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=19" title="Wysig afdeling: Uitbarstende veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=19" title="Edit section's source code: Uitbarstende veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Uitbarstende veranderlike sterre toon onreëlmatige of halfreëlmatige ligwisselings wat veroorsaak word deur materie wat die ster verloor of, in sommige gevalle, aantrek. Ondanks die naam is dit nie ploffende voorvalle nie – sulke sterre word <a href="#Kataklismiese_veranderlikes">kataklismiese veranderlikes</a> genoem. </p> <div class="mw-heading mw-heading4"><h4 id="Protosterre">Protosterre</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=20" title="Wysig afdeling: Protosterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=20" title="Edit section's source code: Protosterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Protosterre is jong voorwerpe wat nog nie die proses voltooi het om ’n <a href="/wiki/Ster" title="Ster">ster</a> uit ’n <a href="/wiki/Newel" title="Newel">gasnewel</a> te vorm nie. Die meeste protosterre toon onreëlmatige skommelings. </p> <dl><dt>Herbig Ae/Be-sterre</dt> <dd><i>Hoofartikel: <a href="/wiki/Herbig_Ae/Be-ster" title="Herbig Ae/Be-ster">Herbig Ae/Be-ster</a></i></dd></dl> <p>Die ligwisselings van <a href="/wiki/Herbig_Ae/Be-ster" title="Herbig Ae/Be-ster">Herbig Ae/Be-sterre</a> met ’n groot massa (2 tot 8 <a href="/wiki/Sonmassa" title="Sonmassa">sonmassas</a>) is waarskynlik die gevolg van bolle gas en stof wat om die ster wentel. Sommige sterre het aansienlike ligskommelings, waarskynlik vanweë <a href="/wiki/Protoplanete" class="mw-redirect" title="Protoplanete">protoplanete</a> en <a href="/wiki/Planetesimale" class="mw-redirect" title="Planetesimale">planetesimale</a> in die gas en stof wat voor die sterre verbybeweeg. </p> <dl><dt>Orion-veranderlikes</dt></dl> <p>Hulle is jong, warm voor-<a href="/wiki/Hoofreeks" title="Hoofreeks">hoofreekssterre</a> wat gewoonlik omring is deur newels. Hulle het onreëlmatige periodes met ’n omvang van verskeie magnitudes. ’n Bekende subtipe-Orion-veranderlikes is die <a href="/wiki/T_Tauri-ster" title="T Tauri-ster">T Tauri-sterre</a>. Hul ligwisselings is vanweë vlekke op die sterre se oppervlak asook gas en stof wat om die sterre wentel. </p><p>Die woord "Orion-veranderlike" was ’n nuttige, allesomvattende term, maar word nou al hoe minder gebruik. Om historiese redes gebruik die GCVS dit steeds. Sterrekundiges onderskei egter deesdae tussen dié soort sterre met meer spesifieke name soos "klassieke T Tauri"- of "UX Orionis"-sterre na aanleiding van hul fisiese verskille. </p> <dl><dt>FU Orionis-veranderlikes</dt></dl> <p>Hulle lê in <a href="/wiki/Newel#Soorte_newels" title="Newel">refleksienewels</a> en toon geleidelike toenames in hul helderheid in die omgewing van 6 magnitude, gevolg deur ’n lang fase van konstante helderheid. Oor ’n kwessie van jare verdof hulle weer met sowat 2 magnitude (ses keer dowwer). V1057 Cygni het byvoorbeeld in ’n tydperk van 11 jaar met 2,5 magnitude dowwer geword (10 keer dowwer). FU Orionis-veranderlikes is van <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">spektraaltipe A</a> tot <a href="/wiki/Sterreklassifikasie#Klas_G" title="Sterreklassifikasie">spektraaltipe G</a> en is moontlik ’n evolusiefase in die bestaan van T Tauri-sterre. </p> <div class="mw-heading mw-heading4"><h4 id="Reuse_en_superreuse">Reuse en superreuse</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=21" title="Wysig afdeling: Reuse en superreuse" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=21" title="Edit section's source code: Reuse en superreuse"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Groot sterre verloor hul materie redelik maklik. Daarom is ligwisselings vanweë uitbarstings en massaverlies redelik algemeen onder reuse en superreuse. </p> <dl><dt>Helder blou veranderlikes</dt></dl> <p>Die helderste sterre bekend behoort tot dié klas, wat ook S Doradus-veranderlikes genoem word. Voorbeelde is die <a href="/wiki/Hiperreus" title="Hiperreus">hiperreuse</a> <a href="/wiki/Eta_Carinae" title="Eta Carinae">η Carinae</a> en P Cygni. Hulle verloor permanent baie massa, maar met tussenposes van jare veroorsaak inherente pulserings dat die ster sy <a href="/wiki/Eddington-limiet" title="Eddington-limiet">Eddington-limiet</a> oorskry en dan neem die massaverlies geweldig toe. Sigbare helderheid neem toe, terwyl die algemene helderheid grootliks onveranderd bly. Reuseagtige uitbarstings wat in ’n paar van dié sterre waargeneem is, laat wel die algemene helderheid toeneem – in so ’n mate dat hulle al "vals <a href="/wiki/Supernova" title="Supernova">supernovas</a>" genoem is. Dit kan egter ’n heel ander soort voorval wees. </p> <dl><dt>Geelhiperreuse</dt></dl> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg/220px-Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg.png" decoding="async" width="220" height="158" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg/330px-Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg/440px-Rho_Cassiopeiae_Sol_VY_Canis_Majoris_-_2019-05-14.svg.png 2x" data-file-width="2696" data-file-height="1939" /></a><figcaption>Die geelhiperreus Rho Cassiopeiae, met ’n radius van <span style="white-space:nowrap">450 <a href="/wiki/Sonradius" title="Sonradius">R<sub>☉</sub></a></span> (twee van links), se grootte in vergelyking met dié van ander sterre, onder meer <a href="/wiki/Betelgeuse" title="Betelgeuse">Betelgeuse</a> (<span style="white-space:nowrap">1 000 <a href="/wiki/Sonradius" title="Sonradius">R<sub>☉</sub></a></span>, tweede van regs). Die Son kan nie op dié skaal gesien word nie.</figcaption></figure> <p>’n Geelhiperreus is ’n ster met ’n groot massa en atmosfeer, van <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">spektraaltipe laat A</a> tot <a href="/wiki/Sterreklassifikasie#Klas_K" title="Sterreklassifikasie">vroeë K</a>. Hulle het aanvanklik ’n massa van tot 20-50 <a href="/wiki/Sonmassa" title="Sonmassa">sonmassas</a> gehad, maar het al tot die helfte daarvan verloor.<sup id="cite_ref-gesicki_20-0" class="reference"><a href="#cite_note-gesicki-20"><span class="cite-bracket">[</span>20<span class="cite-bracket">]</span></a></sup> Hulle is van die sterre met die grootste <a href="/wiki/Ligsterkte" class="mw-redirect" title="Ligsterkte">ligsterkte</a>, met <a href="/wiki/Absolute_magnitude" title="Absolute magnitude">absolute magnitudes</a> van sowat <span style="white-space:nowrap">-9</span>, maar ook van die skaarsstes – daar is net ’n hand vol bekend in die <a href="/wiki/Melkweg" title="Melkweg">Melkweg</a>. Hulle word soms koel hiperreuse genoem in vergelyking met O- en B-sterre, en soms warm hiperreuse in vergelyking met rooisuperreuse.<sup id="cite_ref-cool_21-0" class="reference"><a href="#cite_note-cool-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-warm_22-0" class="reference"><a href="#cite_note-warm-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup> </p><p>Hierdie sterre is onstabiel vanweë hul besonderse helderheid en ligging bo die <a href="/wiki/Onstabiele_strook" title="Onstabiele strook">onstabiele strook</a> op die <a href="/wiki/HR-diagram" class="mw-redirect" title="HR-diagram">HR-diagram</a>, en hulle toon langsame maar soms groot fotometriese en spektroskopiese veranderings vanweë hul groot massaverlies en sporadiese groter uitbarstings. Die beste bekende voorbeeld is Rho Cassiopeiae. </p> <dl><dt>R Coronae Borealis-veranderlikes</dt></dl> <p>Hoewel hulle as uitbarstende veranderlikes geklassifiseer word, ondergaan hierdie sterre nie ’n periodieke toename in helderheid nie. Hulle is meestal op hul helderste, maar verdof met ongereelde tussenposes met 1 tot 9 magnitude (2,5 tot 4 000 keer dowwer) voordat hulle oor maande of jare na hul gewone helderheid terugkeer. Die meeste word volgens hul helderheid as geelhiperreuse geklassifiseer, hoewel hulle eintlik post-<a href="/wiki/Asimptotiese_reusetak" title="Asimptotiese reusetak">asimptotiese reuse</a> is. Daar is egter ook <a href="/wiki/Rooireus" title="Rooireus">rooi-</a> en <a href="/wiki/Bloureus" title="Bloureus">bloureuse</a> wat R CrB-sterre is. R Coronae Borealis is die prototipe-ster van dié klas. </p> <div class="mw-heading mw-heading4"><h4 id="Wolf-Rayet-veranderlikes">Wolf-Rayet-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=22" title="Wysig afdeling: Wolf-Rayet-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=22" title="Edit section's source code: Wolf-Rayet-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dd><i>Hoofartikel: <a href="/wiki/Wolf-Rayetster" title="Wolf-Rayetster">Wolf-Rayetster</a></i></dd></dl> <p><a href="/wiki/Wolf-Rayetster" title="Wolf-Rayetster">Wolf-Rayetsterre</a> is warm sterre met ’n groot massa (van meer as 20 sonmassas) wat vinnig dié massa verloor vanweë ’n sterk <a href="/wiki/Sterwind" title="Sterwind">sterwind</a>. Hulle toon soms ligwisselings, waarskynlik om verskillende redes soos <a href="/wiki/Dubbelster" title="Dubbelster">dubbelster</a>-wisselwerkings en bolle gas wat om die ster wentel. Hulle toon breë <a href="/wiki/Spektraallyn" title="Spektraallyn">emissielynspektra</a> met <a href="/wiki/Helium" title="Helium">helium-</a>, <a href="/wiki/Stikstof" title="Stikstof">stikstof-</a>, <a href="/wiki/Koolstof" title="Koolstof">koolstof-</a> en <a href="/wiki/Suurstof" title="Suurstof">suurstoflyne</a>. Wisselings in sommige sterre lyk of hulle stogasties is, terwyl ander veelvuldige periodes toon. </p> <div class="mw-heading mw-heading4"><h4 id="Gamma_Cassiopeiae-veranderlikes">Gamma Cassiopeiae-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=23" title="Wysig afdeling: Gamma Cassiopeiae-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=23" title="Edit section's source code: Gamma Cassiopeiae-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Gamma Cassiopeiae- of γ Cas-veranderlikes is <a href="/wiki/Sterreklassifikasie#Klas_B" title="Sterreklassifikasie">spektraaltipe B-sterre</a> wat nie <a href="/wiki/Superreus" title="Superreus">superreuse</a> is nie en vinnig roteer. Hul ligwisselings is onreëlmatig, met ’n omvang van tot 1,5 magnitude (vier keer so helder), vanweë die uitskiet van materie by hul ewenaars wat deur die vinnige rotasie veroorsaak word. </p> <div class="mw-heading mw-heading4"><h4 id="Opvlamsterre">Opvlamsterre</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=24" title="Wysig afdeling: Opvlamsterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=24" title="Edit section's source code: Opvlamsterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dd><i>Hoofartikel: <a href="/wiki/Opvlamster" title="Opvlamster">Opvlamster</a></i></dd></dl> <p>In hoofreekssterre is groot uitbarstende ligwisselings ongewoon. Dit is net die baie dowwe <a href="/wiki/Opvlamster" title="Opvlamster">opvlamsterre</a>, ook bekend as die UV Ceti-veranderlikes, wat gereeld opvlam. Hul ligwisselings is onvoorspelbaar en dramaties: hulle word met tot 2 magnitude (ses keer) helderder in net ’n paar sekondes, en dan verdof hulle weer binne ’n halfuur of minder tot hul normale helderheid. Opvlammings kan elke paar dae plaasvind of, soos in die geval van <a href="/wiki/Barnard_se_Ster" title="Barnard se Ster">Barnard se Ster</a>, baie minder gereeld. </p><p>Die meeste opvlamsterre is dowwe <a href="/wiki/Rooidwerg" title="Rooidwerg">rooidwergsterre</a>. Verskeie nabygeleë rooidwerge is opvlamsterre, soos Barnard se Ster en <a href="/wiki/Proxima_Centauri" title="Proxima Centauri">Proxima Centauri</a>. Die bekendste een is egter <a href="/wiki/UV_Ceti" class="mw-redirect" title="UV Ceti">UV Ceti</a>, wat in 1948 ontdek is en waarna dié klas veranderlike sterre genoem is. </p> <div class="mw-heading mw-heading4"><h4 id="RS_Canum_Venaticorum-veranderlikes">RS Canum Venaticorum-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=25" title="Wysig afdeling: RS Canum Venaticorum-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=25" title="Edit section's source code: RS Canum Venaticorum-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Hulle is dubbelsterre wat na aan mekaar geleë is en baie aktiewe chromosfere het, insluitende groot <a href="/wiki/Sonvlek" title="Sonvlek">sonvlekke</a> en opvlammings, wat waarskynlik veroorsaak word deur hul nabyheid aan mekaar. Periodes wissel van dae, wat afhang van hul wentelperiode en soms ook verduisterings, tot jare vanweë veranderings in sonvlek-aktiwiteit. Hulle word verder in vyf subklasse verdeel: reëlmatige, kortperiode-, langperiode-, opvlamster- en V471 Tau-tipe-stelsels. </p> <div class="mw-heading mw-heading3"><h3 id="Kataklismiese_veranderlikes">Kataklismiese veranderlikes</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=26" title="Wysig afdeling: Kataklismiese veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=26" title="Edit section's source code: Kataklismiese veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="mw-heading mw-heading4"><h4 id="Supernovas">Supernovas</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=27" title="Wysig afdeling: Supernovas" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=27" title="Edit section's source code: Supernovas"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dd><i>Hoofartikel: <a href="/wiki/Supernova" title="Supernova">Supernova</a></i></dd></dl> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Crab_Nebula.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/240px-Crab_Nebula.jpg" decoding="async" width="240" height="240" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/360px-Crab_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/480px-Crab_Nebula.jpg 2x" data-file-width="3864" data-file-height="3864" /></a><figcaption>Die Krap-newel.</figcaption></figure> <p><a href="/wiki/Supernova" title="Supernova">Supernovas</a> is die mees dramatiese tipe kataklismiese veranderlikes en van die verskynsels in die <a href="/wiki/Heelal" title="Heelal">heelal</a> waarby die grootste hoeveelheid <a href="/wiki/Energie" title="Energie">energie</a> betrokke is. ’n Supernova kan vir ’n ruk meer energie uitstraal as ’n hele <a href="/wiki/Sterrestelsel" title="Sterrestelsel">sterrestelsel</a> en met meer as 20 magnitude verhelder (meer as honderd miljoen keer so helder). ’n Supernova word veroorsaak deur die kern van ’n ster wat ’n sekere massadigtheidslimiet (die <a href="/wiki/Chandrasekhar-limiet" title="Chandrasekhar-limiet">Chandrasekhar-limiet</a>) bereik, wat veroorsaak dat dit in ’n breukdeel van ’n sekonde inplof. Die skokgolwe veroorsaak dat die res van die ster ontplof en ’n enorme hoeveelheid energie uitstraal. Die buitelae van die ster word teen duisende kilometers per uur weggeskiet. Dié lae kan newels vorm wat <a href="/wiki/Planet%C3%AAre_newel" title="Planetêre newel">planetêre newels</a> genoem word. ’n Bekende voorbeeld is die <a href="/wiki/Krap-newel" class="mw-redirect" title="Krap-newel">Krap-newel</a>, wat oorgebly het ná ’n supernova wat in <a href="/wiki/1054" title="1054">1054</a> in <a href="/wiki/China" class="mw-disambig" title="China">China</a> en <a href="/wiki/Noord-Amerika" title="Noord-Amerika">Noord-Amerika</a> waargeneem is. Die kern van die ster kan ’n <a href="/wiki/Neutronster" title="Neutronster">neutronster</a> (gewoonlik ’n <a href="/wiki/Pulsar" title="Pulsar">pulsar</a>) of ’n <a href="/wiki/Swartkolk" title="Swartkolk">swartkolk</a> word. </p><p>Supernovas ontstaan gewoonlik uit die dood van ’n ster met ’n enorme massa, baie keer groter as dié van die <a href="/wiki/Son" title="Son">son</a>. </p> <div class="mw-heading mw-heading4"><h4 id="Novas">Novas</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=28" title="Wysig afdeling: Novas" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=28" title="Edit section's source code: Novas"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dd><i>Hoofartikel: <a href="/wiki/Nova" title="Nova">Nova</a></i></dd></dl> <p><a href="/wiki/Nova" title="Nova">Novas</a> is ook die gevolg van ’n groot ontploffing, maar anders as met ’n supernova word ’n ster nie in die proses vernietig nie. Novas vorm in <a href="/wiki/Dubbelster" title="Dubbelster">dubbelsterstelsels</a> waarvan die een metgesel ’n <a href="/wiki/Witdwerg" title="Witdwerg">witdwerg</a> is wat die gas van die ander ster, ’n gewone ster, aantrek. Die gas bou op die oppervlak van die witdwerg op totdat dit ’n sekere limiet oorskry en ontplof. Dit kan oor tydperke van dekades of millennia plaasvind. </p><p>Novas word geklassifiseer as vinnig, stadig of baie stadig na gelang van die ligkurwe. In die onlangse geskiedenis was Nova Cygni 1975 die helderste nova, met ’n magnitude van 2. </p> <dl><dt>Dwerg-novas</dt></dl> <p>Hulle is dieselfde as novas, maar het meer gereelde en kleiner uitbarstings. Daar is drie soorte: U Geminorum-, Z Camelopardalis- en SU Ursae Majoris-veranderlikes. </p> <div class="mw-heading mw-heading2"><h2 id="Ekstrinsieke_veranderlikes">Ekstrinsieke veranderlikes</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=29" title="Wysig afdeling: Ekstrinsieke veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=29" title="Edit section's source code: Ekstrinsieke veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Daar is twee hoofgroepe ekstrinsieke veranderlikes: roterende en verduisterende sterre. </p> <div class="mw-heading mw-heading3"><h3 id="Roterende_veranderlikes">Roterende veranderlikes</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=30" title="Wysig afdeling: Roterende veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=30" title="Edit section's source code: Roterende veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Sterre met taamlike <a href="/wiki/Sonvlek" title="Sonvlek">sonvlekke</a> kan ’n aansienlike wisseling in helderheid toon namate hulle roteer en helderder gebiede van die oppervlak in die Aarde se rigting wys. Helder vlekke kom ook voor by die magnetiese pole van magnetiese sterre. Sterre met ovaal vorms kan ook verskille in helderheid ondergaan namate die dele van die oppervlak wat hulle na die waarnemer draai, van grootte verskil. </p> <div class="mw-heading mw-heading4"><h4 id="Niesferiese_sterre">Niesferiese sterre</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=31" title="Wysig afdeling: Niesferiese sterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=31" title="Edit section's source code: Niesferiese sterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dt>Ovaalvormige veranderlikes</dt></dl> <p>Hulle is <a href="/wiki/Dubbelster" title="Dubbelster">dubbelsterre</a> wat na aan mekaar geleë is. Die metgeselle is ovaalvormig vanweë hul wedersydse <a href="/wiki/Swaartekrag" title="Swaartekrag">swaartekrag</a>. Namate die sterre roteer, verander die grootte van die oppervlak wat na die Aarde wys en dit beïnvloed weer die helderheid wat die waarnemer sien. </p> <div class="mw-heading mw-heading4"><h4 id="Stervlekke">Stervlekke</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=32" title="Wysig afdeling: Stervlekke" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=32" title="Edit section's source code: Stervlekke"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Die oppervlak van ’n ster is nie oral ewe helder nie; dit het donkerder en helderder gebiede (bekend as son- of stervlekke). Die ster se chromosfeer kan ook verskille in helderheid toon. Namate die ster roteer, sien ons ligwisselings van ’n paar tiendes van ’n magnitude. </p> <dl><dt>FK Comae Berenices-veranderlikes</dt></dl> <p>Dié sterre roteer uiters vinnig (~100 km/s by die ewenaar); dus is hulle ovaalvormig. Hulle is (oënskynlik) alleenstaande <a href="/wiki/Reusester" title="Reusester">reusesterre</a> van <a href="/wiki/Sterreklassifikasie#Klas_G" title="Sterreklassifikasie">spektraaltipe G</a> en <a href="/wiki/Sterreklassifikasie#Klas_K" title="Sterreklassifikasie">spektraaltipe K</a>, en toon sterk chromosferiese <a href="/wiki/Spektraallyn" title="Spektraallyn">emissielyne</a>. Voorbeelde is FK Com, HD 199178 en UZ Lib. ’n Moontlike verduidelik vir die vinnige rotasie van FK Comae-sterre is dat hulle dubbelsterre is wat saamgesmelt het. </p> <dl><dt>BY Draconis-veranderlikes</dt></dl> <p>Die sterre in dié klas is van <a href="/wiki/Sterreklassifikasie#Klas_K" title="Sterreklassifikasie">spektraaltipe K</a> of <a href="/wiki/Sterreklassifikasie#Klas_M" title="Sterreklassifikasie">spektraaltipe M</a> en ligwisselings is minder as 0,5 magnitude (70%). </p> <div class="mw-heading mw-heading4"><h4 id="Magneetvelde">Magneetvelde</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=33" title="Wysig afdeling: Magneetvelde" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=33" title="Edit section's source code: Magneetvelde"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <dl><dt>Alpha<sup>2</sup> Canum Venaticorum-veranderlikes</dt></dl> <p>Alpha<sup>2</sup> Canum Venaticorum- of α<sup>2</sup> CVn-veranderlikes is hoofreekssterre van <a href="/wiki/Sterreklassifikasie#Klas_B" title="Sterreklassifikasie">spektraaltipe B8</a> tot <a href="/wiki/Sterreklassifikasie#Klas_A" title="Sterreklassifikasie">A7</a> wat oor ’n tydperk van 0,5 tot 160 dae ligwisselings van 0,01 tot 0,1 magnitude (1% tot 10%) toon.<sup id="cite_ref-23" class="reference"><a href="#cite_note-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup> Hulle het sterk <a href="/wiki/Magneetveld" title="Magneetveld">magneetvelde</a> en sterk <a href="/wiki/Spektraallyn" title="Spektraallyn">spektraallyne</a> van <a href="/wiki/Silikon" title="Silikon">silikon</a>, <a href="/wiki/Stronsium" title="Stronsium">stronsium</a> of <a href="/wiki/Chroom" title="Chroom">chroom</a>. </p><p>Benewens die ligskommelings is daar ook wisselings in die intensiteit en voorkoms van die spektraallyne en magneetvelde. Die periodes van hierdie wisselings is almal dieselfde en daar word geglo dit stem ooreen met die ster se rotasieperiode. Die wisselings word waarskynlik veroorsaak deur ’n ongelyke verspreiding van <a href="/wiki/Metaal_(astronomie)" class="mw-redirect" title="Metaal (astronomie)">metale</a> in die atmosfeer en daarom verskil die metale van plek tot plek namate die ster roteer.<sup id="cite_ref-24" class="reference"><a href="#cite_note-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup> </p> <dl><dt>SX Arietis-veranderlikes</dt></dl> <p>Sterre in dié klas toon ligwisselings van sowat 0,1 magnitude wat veroorsaak word deur veranderings in hul magneetvelde vanweë hul hoë rotasiespoed. Hulle is gewoonlik B-tipe-hoofreekssterre met sterk magneetvelde en sterk <a href="/wiki/Helium" title="Helium">He</a> I- en <a href="/wiki/Silikon" title="Silikon">Si</a> III-spektraallyne. </p> <dl><dt>Optiese veranderlike pulsars</dt> <dd><i>Hoofartikel: <a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></i></dd></dl> <p>’n Paar <a href="/wiki/Pulsar" title="Pulsar">pulsars</a> is waargeneem in sigbare lig. Hierdie <a href="/wiki/Neutronster" title="Neutronster">neutronsterre</a> se helderheid verander namate hulle roteer. Vanweë die vinnige rotasie is skommelings uiters vinnig, van millisekondes tot ’n paar sekondes. Die eerste en beste voorbeeld is die <a href="/wiki/Krap-pulsar" title="Krap-pulsar">Krap-pulsar</a>. </p> <div class="mw-heading mw-heading3"><h3 id="Verduisterende_dubbelsterre">Verduisterende dubbelsterre</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=34" title="Wysig afdeling: Verduisterende dubbelsterre" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=34" title="Edit section's source code: Verduisterende dubbelsterre"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/L%C3%AAer:Light_curve_of_binary_star_Kepler-16_af.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Light_curve_of_binary_star_Kepler-16_af.svg/350px-Light_curve_of_binary_star_Kepler-16_af.svg.png" decoding="async" width="350" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Light_curve_of_binary_star_Kepler-16_af.svg/525px-Light_curve_of_binary_star_Kepler-16_af.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Light_curve_of_binary_star_Kepler-16_af.svg/700px-Light_curve_of_binary_star_Kepler-16_af.svg.png 2x" data-file-width="860" data-file-height="540" /></a><figcaption>Hoe verduisterende dubbelsterre se helderheid wissel, met die primêre en sekondêre minimums aangedui.</figcaption></figure> <p>Een van die algemeenste redes vir ’n ekstrinsieke veranderlikheid is die teenwoordigheid van ’n metgesel-ster in ’n <a href="/wiki/Dubbelster" title="Dubbelster">dubbelsterstelsel</a>. Wanneer dit vanuit ’n sekere hoek beskou word, soos van die Aarde af, kan die sterre mekaar verduister wanneer hulle voor mekaar verbybeweeg en so ’n afname in helderheid veroorsaak. Een van die bekendste voorbeelde van verduisterende dubbelsterre is <a href="/wiki/Algol" title="Algol">Algol</a>, of Beta Persei (β Per). </p><p>Wanneer die sterre ook ’n spektroskopiese dubbelster is en die stelsel se <a href="/wiki/Parallaks" title="Parallaks">parallaks</a> bekend is, is hulle baie waardevol vir sterontledings.<sup id="cite_ref-25" class="reference"><a href="#cite_note-25"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> In die afgelope dekade het die meting van die basiese parameters van verduisterende dubbelsterre buite die Melkweg moontlik geword danksy 8-meter-teleskope. Die sterre kan dus gebruik word om die afstand na ander sterrestelsels regstreeks te meet, ’n proses wat meer akkuraat is as standaardmetodes.<sup id="cite_ref-wilson2008_26-0" class="reference"><a href="#cite_note-wilson2008-26"><span class="cite-bracket">[</span>26<span class="cite-bracket">]</span></a></sup> Onlangs is dié metode gebruik om die afstande na die <a href="/wiki/Groot_Magellaanse_Wolk" title="Groot Magellaanse Wolk">Groot</a> en <a href="/wiki/Klein_Magellaanse_Wolk" title="Klein Magellaanse Wolk">Klein Magellaanse Wolk</a>, <a href="/wiki/Andromeda-sterrestelsel" title="Andromeda-sterrestelsel">Andromeda</a> en die <a href="/wiki/Driehoek-sterrestelsel" class="mw-redirect" title="Driehoek-sterrestelsel">Driehoek-sterrestelsel</a> te meet tot ’n verbeterde 5%-vlak van akkuraatheid.<sup id="cite_ref-Bonanos2006_27-0" class="reference"><a href="#cite_note-Bonanos2006-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup> </p><p>Die ligkurwe van sulke sterre toon ’n lang tydperk van konstante helderheid, afgewissel deur ’n konstante periodieke verdowwing. Die verskillende groottes van die sterre in die stelsel sal die ligkurwe bepaal. As die een ster baie groter as die ander een is, sal die een verduistering algeheel wees en die ander een slegs gedeeltelik. Daar sal dus twee minimums wees van verskillende intensiteit. </p> <div class="mw-heading mw-heading4"><h4 id="Algol-veranderlikes">Algol-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=35" title="Wysig afdeling: Algol-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=35" title="Edit section's source code: Algol-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Dié sterre ondergaan verduisterings met een of twee minimums wat afgewissel word deur periodes van byna konstante lig. Die prototipe van die klas is <a href="/wiki/Algol" title="Algol">Algol</a> in die <a href="/wiki/Sterrebeeld" title="Sterrebeeld">sterrebeeld</a> <a href="/wiki/Perseus_(sterrebeeld)" title="Perseus (sterrebeeld)">Perseus</a>. </p><p>Sterre van ’n Algol-dubbelstelsel het ’n <a href="/wiki/Sfeer" title="Sfeer">sferiese</a> vorm en dit onderskei hulle van die Beta Lyrae- en W Ursae Majoris-veranderlikes. </p> <div class="mw-heading mw-heading4"><h4 id="Beta_Lyrae-veranderlikes">Beta Lyrae-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=36" title="Wysig afdeling: Beta Lyrae-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=36" title="Edit section's source code: Beta Lyrae-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Beta Lyrae- of β Lyr-veranderlikes is reuse- en superreusesterre (met ’n massa van ’n paar keer dié van die Son) wat uiters na aan mekaar lê – so naby dat hul vorm verwring word deur wedersydse <a href="/wiki/Swaartekrag" title="Swaartekrag">swaartekrag</a>. Hulle is ovaalvormig en daar is ’n groot uitruil van materie tussen die twee sterre. Die ligkurwes van die sterre verander voortdurend, en dit maak dit amper onmoontlik om die presiese begin en einde van elke verduistering te bepaal. </p> <div class="mw-heading mw-heading4"><h4 id="W_Ursae_Majoris-veranderlikes">W Ursae Majoris-veranderlikes</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=37" title="Wysig afdeling: W Ursae Majoris-veranderlikes" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=37" title="Edit section's source code: W Ursae Majoris-veranderlikes"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Die sterre in dié klas is van <a href="/wiki/Sterreklassifikasie#Klas_F" title="Sterreklassifikasie">spektraaltipe F</a>, <a href="/wiki/Sterreklassifikasie#Klas_G" title="Sterreklassifikasie">G</a> of <a href="/wiki/Sterreklassifikasie#Klas_K" title="Sterreklassifikasie">K</a> en het periodes van minder as ’n dag. Die sterre lê so na aan mekaar dat hul oppervlakke in kontak met mekaar is. Hulle word daarom kontakdubbelsterre genoem. ’n Groot hoeveelheid massa word deur ’n verbindingsbrug tussen hulle uitgeruil. </p> <div class="mw-heading mw-heading3"><h3 id="Planetêre_oorgange"><span id="Planet.C3.AAre_oorgange"></span>Planetêre oorgange</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=38" title="Wysig afdeling: Planetêre oorgange" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=38" title="Edit section's source code: Planetêre oorgange"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Sterre met <a href="/wiki/Eksoplaneet" title="Eksoplaneet">eksoplanete</a> kan ook wisselings in helderheid toon as die planete <a href="/wiki/Oorgang_(sterrekunde)" title="Oorgang (sterrekunde)">tussen hulle en die Aarde verbybeweeg</a>. Dié wisselings is baie kleiner as met ster-metgeselle en word net met baie noukeurige metings waargeneem. Voorbeelde is HD 209458 en GSC 02652-01324, asook al die planete en kandidaatplanete wat deur die <a href="/wiki/Kepler-ruimteteleskoop" title="Kepler-ruimteteleskoop">Kepler-sending</a> bespeur word. </p> <div class="mw-heading mw-heading2"><h2 id="Verwysings">Verwysings</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=39" title="Wysig afdeling: Verwysings" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=39" title="Edit section's source code: Verwysings"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="reflist columns references-column-count references-column-count-2" style="-moz-column-count: 2; -webkit-column-count: 2; column-count: 2; list-style-type: decimal;"> <ol class="references"> <li id="cite_note-1"><span class="mw-cite-backlink"><a href="#cite_ref-1">↑</a></span> <span class="reference-text"><span class="citation"> <a rel="nofollow" class="external text" href="http://www.pmodwrc.ch/pmod.php?topic=tsi/composite/SolarConstant"><i>Solar Constant</i></a>, PMOD/WRC<span class="printonly">, <a rel="nofollow" class="external free" href="http://www.pmodwrc.ch/pmod.php?topic=tsi/composite/SolarConstant">http://www.pmodwrc.ch/pmod.php?topic=tsi/composite/SolarConstant</a></span><span class="reference-accessdate">, besoek op 2009-04-27</span></span><span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Solar+Constant&rft.pub=PMOD%2FWRC&rft_id=http%3A%2F%2Fwww.pmodwrc.ch%2Fpmod.php%3Ftopic%3Dtsi%2Fcomposite%2FSolarConstant&rfr_id=info:sid/en.wikipedia.org:Veranderlike_ster"><span style="display: none;"> </span></span></span> </li> <li id="cite_note-2"><span class="mw-cite-backlink"><a href="#cite_ref-2">↑</a></span> <span class="reference-text"><style data-mw-deduplicate="TemplateStyles:r2205490">.mw-parser-output cite.citation{font-style:inherit}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .id-lock-free a,.mw-parser-output .citation .cs1-lock-free a{background-image:url("//upload.wikimedia.org/wikipedia/commons/thumb/6/65/Lock-green.svg/9px-Lock-green.svg.png");background-image:linear-gradient(transparent,transparent),url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg");background-repeat:no-repeat;background-size:9px;background-position:right .1em center}.mw-parser-output .id-lock-limited a,.mw-parser-output .id-lock-registration a,.mw-parser-output .citation .cs1-lock-limited a,.mw-parser-output .citation .cs1-lock-registration a{background-image:url("//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/Lock-gray-alt-2.svg/9px-Lock-gray-alt-2.svg.png");background-image:linear-gradient(transparent,transparent),url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg");background-repeat:no-repeat;background-size:9px;background-position:right .1em center}.mw-parser-output .id-lock-subscription a,.mw-parser-output .citation .cs1-lock-subscription a{background-image:url("//upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Lock-red-alt-2.svg/9px-Lock-red-alt-2.svg.png");background-image:linear-gradient(transparent,transparent),url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg");background-repeat:no-repeat;background-size:9px;background-position:right .1em center}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration{color:#555}.mw-parser-output .cs1-subscription span,.mw-parser-output .cs1-registration span{border-bottom:1px dotted;cursor:help}.mw-parser-output .cs1-ws-icon a{background-image:url("//upload.wikimedia.org/wikipedia/commons/thumb/4/4c/Wikisource-logo.svg/12px-Wikisource-logo.svg.png");background-image:linear-gradient(transparent,transparent),url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg");background-repeat:no-repeat;background-size:12px;background-position:right .1em center}.mw-parser-output code.cs1-code{color:inherit;background:inherit;border:inherit;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;font-size:100%}.mw-parser-output .cs1-visible-error{font-size:100%}.mw-parser-output .cs1-maint{display:none;color:#33aa33;margin-left:0.3em}.mw-parser-output .cs1-subscription,.mw-parser-output .cs1-registration,.mw-parser-output .cs1-format{font-size:95%}.mw-parser-output .cs1-kern-left,.mw-parser-output .cs1-kern-wl-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right,.mw-parser-output .cs1-kern-wl-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}</style><cite id="CITEREFPorceddu,_S.,_Jetsu,_L.,_Lyytinen,_J.,_Kajatkari,_P.,_Lehtinen,_J.,_Markkanen,_T,_Toivari-Viitala,_J.2008" class="citation journal cs1">Porceddu, S., Jetsu, L., Lyytinen, J., Kajatkari, P., Lehtinen, J., Markkanen, T, Toivari-Viitala, J. (2008). <a rel="nofollow" class="external text" href="http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=2374180">"Evidence of Periodicity in Ancient Egyptian Calendars of Lucky and Unlucky Days"</a>. <i>Cambridge Archaeological Journal</i>. <b>18</b> (3): 327–339. <a href="/wiki/Digitale_objek-identifiseerder" title="Digitale objek-identifiseerder">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1017%2FS0959774308000395">10.1017/S0959774308000395</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Cambridge+Archaeological+Journal&rft.atitle=Evidence+of+Periodicity+in+Ancient+Egyptian+Calendars+of+Lucky+and+Unlucky+Days&rft.volume=18&rft.issue=3&rft.pages=327-339&rft.date=2008&rft_id=info%3Adoi%2F10.1017%2FS0959774308000395&rft.au=Porceddu%2C+S.%2C+Jetsu%2C+L.%2C+Lyytinen%2C+J.%2C+Kajatkari%2C+P.%2C+Lehtinen%2C+J.%2C+Markkanen%2C+T%2C+Toivari-Viitala%2C+J.&rft_id=http%3A%2F%2Fjournals.cambridge.org%2Faction%2FdisplayAbstract%3FfromPage%3Donline%26aid%3D2374180&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span><span class="cs1-maint citation-comment"><code class="cs1-code">{{<a href="/wiki/Sjabloon:Cite_journal" title="Sjabloon:Cite journal">cite journal</a>}}</code>: AS1-onderhoud: meer as een naam (<a href="/wiki/Kategorie:AS1-onderhoud:_meer_as_een_naam" title="Kategorie:AS1-onderhoud: meer as een naam">link</a>)</span></span> </li> <li id="cite_note-3"><span class="mw-cite-backlink"><a href="#cite_ref-3">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFJetsu,_L.,_Porceddu,_S.,_Lyytinen,_J.,_Kajatkari,_P.,_Lehtinen,_J.,_Markkanen,_T,_Toivari-Viitala,_J.2013" class="citation journal cs1">Jetsu, L., Porceddu, S., Lyytinen, J., Kajatkari, P., Lehtinen, J., Markkanen, T, Toivari-Viitala, J. (2013). <a rel="nofollow" class="external text" href="http://adsabs.harvard.edu/abs/2013ApJ...773....1J">"Did the Ancient Egyptians Record the Period of the Eclipsing Binary Algol – The Raging One?"</a>. <i>The Astrophysical Journal</i>. <b>773</b> (1): A1 (14pp). <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="cs1-lock-free" title="Vrylik beskikbaar"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/1204.6206">1204.6206</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2013ApJ...773....1J">2013ApJ...773....1J</a>. <a href="/wiki/Digitale_objek-identifiseerder" title="Digitale objek-identifiseerder">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F0004-637X%2F773%2F1%2F1">10.1088/0004-637X/773/1/1</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=Did+the+Ancient+Egyptians+Record+the+Period+of+the+Eclipsing+Binary+Algol+%E2%80%93+The+Raging+One%3F&rft.volume=773&rft.issue=1&rft.pages=A1+%2814pp%29&rft.date=2013&rft_id=info%3Aarxiv%2F1204.6206&rft_id=info%3Adoi%2F10.1088%2F0004-637X%2F773%2F1%2F1&rft_id=info%3Abibcode%2F2013ApJ...773....1J&rft.au=Jetsu%2C+L.%2C+Porceddu%2C+S.%2C+Lyytinen%2C+J.%2C+Kajatkari%2C+P.%2C+Lehtinen%2C+J.%2C+Markkanen%2C+T%2C+Toivari-Viitala%2C+J.&rft_id=http%3A%2F%2Fadsabs.harvard.edu%2Fabs%2F2013ApJ...773....1J&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span><span class="cs1-maint citation-comment"><code class="cs1-code">{{<a href="/wiki/Sjabloon:Cite_journal" title="Sjabloon:Cite journal">cite journal</a>}}</code>: AS1-onderhoud: meer as een naam (<a href="/wiki/Kategorie:AS1-onderhoud:_meer_as_een_naam" title="Kategorie:AS1-onderhoud: meer as een naam">link</a>)</span></span> </li> <li id="cite_note-4"><span class="mw-cite-backlink"><a href="#cite_ref-4">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite class="citation web cs1 cs1-prop-foreign-lang-source"><a rel="nofollow" class="external text" href="http://www.sai.msu.su/gcvs/gcvs/iii/html/">"General Catalogue of Variable Stars: Vols I-III (the new electronic version)"</a> (in Engels). Sai.msu.su. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20191119025944/http://www.sai.msu.su/gcvs/gcvs/iii/html/">Geargiveer</a> vanaf die oorspronklike op 19 November 2019<span class="reference-accessdate">. Besoek op <span class="nowrap">1 Julie</span> 2013</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=General+Catalogue+of+Variable+Stars%3A+Vols+I-III+%28the+new+electronic+version%29&rft.pub=Sai.msu.su&rft_id=http%3A%2F%2Fwww.sai.msu.su%2Fgcvs%2Fgcvs%2Fiii%2Fhtml%2F&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-asteroseismology-5"><span class="mw-cite-backlink"><a href="#cite_ref-asteroseismology_5-0">↑</a></span> <span class="reference-text">Brown, T. M.; Gilliland, R. L. (1994). "Asteroseismology". Annual Review of Astronomy and Astrophysics 32: 37. Bibcode:1994ARA&A..32...37B. doi:10.1146/annurev.aa.32.090194.000345</span> </li> <li id="cite_note-6"><span class="mw-cite-backlink"><a href="#cite_ref-6">↑</a></span> <span class="reference-text">Cox, John P., <i>Theory of Stellar Pulsation</i>, Princeton, (1980)</span> </li> <li id="cite_note-pulsating-7"><span class="mw-cite-backlink"><a href="#cite_ref-pulsating_7-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFKilkenny" class="citation web cs1">Kilkenny, Dave. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20130123225336/http://www.star.ac.za/course-resources/local/david-buckley/var2.pdf">"Variable Stars II – Pulsating Stars"</a> <span class="cs1-format">(PDF)</span>. Geargiveer vanaf <a rel="nofollow" class="external text" href="http://www.star.ac.za/course-resources/local/david-buckley/var2.pdf">die oorspronklike</a> <span class="cs1-format">(PDF)</span> op 23 Januarie 2013<span class="reference-accessdate">. Besoek op <span class="nowrap">29 Maart</span> 2015</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Variable+Stars+II+%E2%80%93+Pulsating+Stars&rft.aulast=Kilkenny&rft.aufirst=Dave&rft_id=http%3A%2F%2Fwww.star.ac.za%2Fcourse-resources%2Flocal%2Fdavid-buckley%2Fvar2.pdf&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-spb-8"><span class="mw-cite-backlink"><a href="#cite_ref-spb_8-0">↑</a></span> <span class="reference-text">De Cat, P., "An Observational Overview of Pulsations in β Cep Stars and Slowly Pulsating B Stars", <i>Radial and Nonradial Pulsations as Probes of Stellar Physics</i>, ASP Conference Proceedings, Vol. 259. Red. Conny Aerts, Timothy R. Bedding en Jørgen Christensen-Dalsgaard. <a href="/wiki/Spesiaal:Boekbronne/1583810994" class="internal mw-magiclink-isbn">ISBN 1-58381-099-4</a></span> </li> <li id="cite_note-AAVSO-9"><span class="mw-cite-backlink">↑ <sup><a href="#cite_ref-AAVSO_9-0">9,0</a></sup> <sup><a href="#cite_ref-AAVSO_9-1">9,1</a></sup> <sup><a href="#cite_ref-AAVSO_9-2">9,2</a></sup></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFOteroWatsonWils" class="citation web cs1 cs1-prop-foreign-lang-source">Otero, S. A.; Watson, C.; Wils, P. <a rel="nofollow" class="external text" href="http://www.aavso.org/vsx/index.php?view=about.vartypes">"Variable Star Type Designations in the VSX"</a>. <i>AAVSO Website</i> (in Engels). American Association of Variable Star Observers. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20200411162004/https://www.aavso.org/vsx/index.php?view=about.vartypes">Geargiveer</a> vanaf die oorspronklike op 11 April 2020<span class="reference-accessdate">. Besoek op <span class="nowrap">11 Mei</span> 2014</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=AAVSO+Website&rft.atitle=Variable+Star+Type+Designations+in+the+VSX&rft.aulast=Otero&rft.aufirst=S.+A.&rft.au=Watson%2C+C.&rft.au=Wils%2C+P.&rft_id=http%3A%2F%2Fwww.aavso.org%2Fvsx%2Findex.php%3Fview%3Dabout.vartypes&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-Waelkens93-10"><span class="mw-cite-backlink">↑ <sup><a href="#cite_ref-Waelkens93_10-0">10,0</a></sup> <sup><a href="#cite_ref-Waelkens93_10-1">10,1</a></sup></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFWaelkens,_Christoffel1993" class="citation book cs1">Waelkens, Christoffel (1993). "Slowly Pulsating B Stars". In J. M. NEMEC (Ed), Jaymie M. Matthews (red.). <a rel="nofollow" class="external text" href="http://books.google.com.au/books?id=nP0nzUOeQ2sC&pg=PA180&lpg=PA180&dq=53+persei+variable&source=bl&ots=MMMLYVLIsb&sig=Z9Xgh1fj2_eAF9eBkdHilfLyCQk&hl=en&sa=X&ei=iXOzU73wOsXYoAS29YGYDA&ved=0CDkQ6AEwCA#v=onepage&q=53%20persei%20variable&f=false"><i>New Perspectives on Stellar Pulsation and Pulsating Variable Stars: IAU Colloquium 139</i></a>. Cambridge University Press. pp. 180–82. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Spesiaal:Boekbronne/0-521-44382-2" title="Spesiaal:Boekbronne/0-521-44382-2"><bdi>0-521-44382-2</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Slowly+Pulsating+B+Stars&rft.btitle=New+Perspectives+on+Stellar+Pulsation+and+Pulsating+Variable+Stars%3A+IAU+Colloquium+139&rft.pages=180-82&rft.pub=Cambridge+University+Press&rft.date=1993&rft.isbn=0-521-44382-2&rft.au=Waelkens%2C+Christoffel&rft_id=http%3A%2F%2Fbooks.google.com.au%2Fbooks%3Fid%3DnP0nzUOeQ2sC%26pg%3DPA180%26lpg%3DPA180%26dq%3D53%2Bpersei%2Bvariable%26source%3Dbl%26ots%3DMMMLYVLIsb%26sig%3DZ9Xgh1fj2_eAF9eBkdHilfLyCQk%26hl%3Den%26sa%3DX%26ei%3DiXOzU73wOsXYoAS29YGYDA%26ved%3D0CDkQ6AEwCA%23v%3Donepage%26q%3D53%2520persei%2520variable%26f%3Dfalse&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-Percy-11"><span class="mw-cite-backlink"><a href="#cite_ref-Percy_11-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFJohn_R._Percy2007" class="citation book cs1">John R. Percy (2007). <a rel="nofollow" class="external text" href="http://books.google.com.au/books?id=GQzCDQI3YP4C&pg=PA137&lpg=PA137&dq=slowly+pulsating+B+stars+non+radial&source=bl&ots=NIun3nErK0&sig=zNwncO4HGIK8dRWMdOTn_Ewynfg&hl=en&sa=X&ei=vKS2U4W-Is2lkQW0x4GoCw&ved=0CFYQ6AEwBw#v=onepage&q=slowly%20pulsating%20B%20stars%20non%20radial&f=false"><i>Understanding Variable Stars</i></a>. Cambridge University Press. pp. 137–38, 200–02. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Spesiaal:Boekbronne/0-521-23253-8" title="Spesiaal:Boekbronne/0-521-23253-8"><bdi>0-521-23253-8</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Understanding+Variable+Stars&rft.pages=137-38%2C+200-02&rft.pub=Cambridge+University+Press&rft.date=2007&rft.isbn=0-521-23253-8&rft.au=John+R.+Percy&rft_id=http%3A%2F%2Fbooks.google.com.au%2Fbooks%3Fid%3DGQzCDQI3YP4C%26pg%3DPA137%26lpg%3DPA137%26dq%3Dslowly%2Bpulsating%2BB%2Bstars%2Bnon%2Bradial%26source%3Dbl%26ots%3DNIun3nErK0%26sig%3DzNwncO4HGIK8dRWMdOTn_Ewynfg%26hl%3Den%26sa%3DX%26ei%3DvKS2U4W-Is2lkQW0x4GoCw%26ved%3D0CFYQ6AEwBw%23v%3Donepage%26q%3Dslowly%2520pulsating%2520B%2520stars%2520non%2520radial%26f%3Dfalse&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-Waelkens85-12"><span class="mw-cite-backlink"><a href="#cite_ref-Waelkens85_12-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite class="citation journal cs1">Waelkens, Christoffel; Rufener, Fredy (1985). "Photometric variability of mid-B stars". <i>Astronomy & Astrophysics</i>. <b>152</b> (1): 6–14. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1985A&A...152....6W">1985A&A...152....6W</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+%26+Astrophysics&rft.atitle=Photometric+variability+of+mid-B+stars&rft.volume=152&rft.issue=1&rft.pages=6-14&rft.date=1985&rft_id=info%3Abibcode%2F1985A%26A...152....6W&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span><span class="cs1-maint citation-comment"><code class="cs1-code">{{<a href="/wiki/Sjabloon:Cite_journal" title="Sjabloon:Cite journal">cite journal</a>}}</code>: AS1-onderhoud: gebruik authors-parameter (<a href="/wiki/Kategorie:AS1-onderhoud:_gebruik_authors-parameter" title="Kategorie:AS1-onderhoud: gebruik authors-parameter">link</a>)</span></span> </li> <li id="cite_note-decat07-13"><span class="mw-cite-backlink"><a href="#cite_ref-decat07_13-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFde_Cat,_P.2007" class="citation journal cs1">de Cat, P. (2007). <a rel="nofollow" class="external text" href="http://planet-austria.at/0xc1aa500d_0x0016a4f0.pdf">"Observational Asteroseismology of slowly pulsating B stars"</a> <span class="cs1-format">(PDF)</span>. <i>Comm. in Asteroseismology</i>. <b>150</b>: 167–74.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Comm.+in+Asteroseismology&rft.atitle=Observational+Asteroseismology+of+slowly+pulsating+B+stars&rft.volume=150&rft.pages=167-74&rft.date=2007&rft.au=de+Cat%2C+P.&rft_id=http%3A%2F%2Fplanet-austria.at%2F0xc1aa500d_0x0016a4f0.pdf&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-ibvs5817-14"><span class="mw-cite-backlink"><a href="#cite_ref-ibvs5817_14-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFJeffery2008" class="citation journal cs1">Jeffery, C. Simon (Maart 2008). "Variable Star Designations for Extreme Helium Stars". <i>Information Bulletin on Variable Stars</i>. <b>5817</b> (1). <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2008IBVS.5817....1J">2008IBVS.5817....1J</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Information+Bulletin+on+Variable+Stars&rft.atitle=Variable+Star+Designations+for+Extreme+Helium+Stars&rft.volume=5817&rft.issue=1&rft.date=2008-03&rft_id=info%3Abibcode%2F2008IBVS.5817....1J&rft.aulast=Jeffery&rft.aufirst=C.+Simon&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-15"><span class="mw-cite-backlink"><a href="#cite_ref-15">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFWalker,_H._J.Hill,_P._W.1985" class="citation journal cs1">Walker, H. J.; Hill, P. W. (Augustus 1985). "Radial velocities for the hydrogen-deficient star HD 168476, several helium-strong and helium-weak stars". <i>Astronomy and Astrophysics Supplement Series</i>. <b>61</b>: 303–311. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1985A&AS...61..303W">1985A&AS...61..303W</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+and+Astrophysics+Supplement+Series&rft.atitle=Radial+velocities+for+the+hydrogen-deficient+star+HD+168476%2C+several+helium-strong+and+helium-weak+stars&rft.volume=61&rft.pages=303-311&rft.date=1985-08&rft_id=info%3Abibcode%2F1985A%26AS...61..303W&rft.au=Walker%2C+H.+J.&rft.au=Hill%2C+P.+W.&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-physrev-16"><span class="mw-cite-backlink"><a href="#cite_ref-physrev_16-0">↑</a></span> <span class="reference-text">bl. 891, 895, <a rel="nofollow" class="external text" href="http://adsabs.harvard.edu/abs/1990RPPh...53..837K">Physics of white dwarf stars</a>, D. Koester en G. Chanmugam, <i>Reports on Progress in Physics</i> <b>53</b> (1990), bl. 837–915.</span> </li> <li id="cite_note-wden-17"><span class="mw-cite-backlink"><a href="#cite_ref-wden_17-0">↑</a></span> <span class="reference-text">bl. 3525, White dwarfs, Gilles Fontaine and François Wesemael, in <i>Encyclopedia of Astronomy and Astrophysics</i>, red. Paul Murdin, Bristol en Philadelphia: Institute of Physics Publishing en Londen, New York en Tokio: Nature Publishing Group, 2001. <a href="/wiki/Spesiaal:Boekbronne/0333750888" class="internal mw-magiclink-isbn">ISBN 0-333-75088-8</a>.</span> </li> <li id="cite_note-quirion-18"><span class="mw-cite-backlink"><a href="#cite_ref-quirion_18-0">↑</a></span> <span class="reference-text">§ 1.1, 1.2, <a rel="nofollow" class="external text" href="http://adsabs.harvard.edu/abs/2007ApJS..171..219Q">Mapping the Instability Domains of GW Vir Stars in the Effective Temperature-Surface Gravity Diagram</a>, Quirion, P.-O., Fontaine, G., Brassard, P., <i>Astrophysical Journal Supplement Series</i> <b>171</b> (2007), bl. 219–248.</span> </li> <li id="cite_note-19"><span class="mw-cite-backlink"><a href="#cite_ref-19">↑</a></span> <span class="reference-text">§ 1, <a rel="nofollow" class="external text" href="http://adsabs.harvard.edu/abs/2004A%26A...426L..45N">Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209</a>, T. Nagel en K. Werner, <i>Astronomy and Astrophysics</i> <b>426</b> (2004), bl. L45–L48.</span> </li> <li id="cite_note-gesicki-20"><span class="mw-cite-backlink"><a href="#cite_ref-gesicki_20-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFGesicki1992" class="citation journal cs1">Gesicki, K. (1992). "A Modelling of Circumstellar BAII Lines for the Hypergiant Rho-Cassiopeiae". <i>Astronomy and Astrophysics</i>. <b>254</b>: 280. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1992A&A...254..280G">1992A&A...254..280G</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+and+Astrophysics&rft.atitle=A+Modelling+of+Circumstellar+BAII+Lines+for+the+Hypergiant+Rho-Cassiopeiae&rft.volume=254&rft.pages=280&rft.date=1992&rft_id=info%3Abibcode%2F1992A%26A...254..280G&rft.aulast=Gesicki&rft.aufirst=K.&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-cool-21"><span class="mw-cite-backlink"><a href="#cite_ref-cool_21-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFLobelDe_JagerNieuwenhuijzen2013" class="citation journal cs1">Lobel, A.; De Jager, K.; Nieuwenhuijzen, H. (2013). "Long-term Spectroscopic Monitoring of Cool Hypergiants HR 8752, IRC+10420, and 6 Cas near the Yellow Evolutionary Void". <i>370 Years of Astronomy in Utrecht. Proceedings of a conference held 2–5 April</i>. <b>470</b>: 167. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2013ASPC..470..167L">2013ASPC..470..167L</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=370+Years+of+Astronomy+in+Utrecht.+Proceedings+of+a+conference+held+2%E2%80%935+April&rft.atitle=Long-term+Spectroscopic+Monitoring+of+Cool+Hypergiants+HR+8752%2C+IRC%2B10420%2C+and+6+Cas+near+the+Yellow+Evolutionary+Void&rft.volume=470&rft.pages=167&rft.date=2013&rft_id=info%3Abibcode%2F2013ASPC..470..167L&rft.aulast=Lobel&rft.aufirst=A.&rft.au=De+Jager%2C+K.&rft.au=Nieuwenhuijzen%2C+H.&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-warm-22"><span class="mw-cite-backlink"><a href="#cite_ref-warm_22-0">↑</a></span> <span class="reference-text"><span class="citation Journal">Humphreys, Roberta M.; Davidson, Kris; Grammer, Skyler; Kneeland, Nathan; Martin, John C.; Weis, Kerstin; Burggraf, Birgitta (2013). "Luminous and Variable Stars in M31 and M33. I. The Warm Hypergiants and Post-Red Supergiant Evolution".  [astro-ph.SR].</span><span class="Z3988" title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.btitle=Luminous+and+Variable+Stars+in+M31+and+M33.+I.+The+Warm+Hypergiants+and+Post-Red+Supergiant+Evolution&rft.atitle=&rft.aulast=Humphreys&rft.aufirst=Roberta+M.&rft.au=Humphreys%2C%26%2332%3BRoberta+M.&rft.au=Davidson%2C%26%2332%3BKris&rft.au=Grammer%2C%26%2332%3BSkyler&rft.au=Kneeland%2C%26%2332%3BNathan&rft.au=Martin%2C%26%2332%3BJohn+C.&rft.au=Weis%2C%26%2332%3BKerstin&rft.au=Burggraf%2C%26%2332%3BBirgitta&rft.date=2013&rfr_id=info:sid/en.wikipedia.org:Veranderlike_ster"><span style="display: none;"> </span></span></span> </li> <li id="cite_note-23"><span class="mw-cite-backlink"><a href="#cite_ref-23">↑</a></span> <span class="reference-text"><a rel="nofollow" class="external text" href="http://www.sai.msu.su/groups/cluster/gcvs/gcvs/iii/vartype.txt">Variability types, General Catalogue of Variable Stars</a>, Sternberg Astronomical Institute, Moscow, Russia. URL besoek op 20 Augustus 2008.</span> </li> <li id="cite_note-24"><span class="mw-cite-backlink"><a href="#cite_ref-24">↑</a></span> <span class="reference-text">bl. 83–85, <i>Variable Stars</i>, Michel Petit, Chichester, VK: John Wiley & Sons, 1987, <a href="/wiki/Spesiaal:Boekbronne/0471909203" class="internal mw-magiclink-isbn">ISBN 0-471-90920-3</a>.</span> </li> <li id="cite_note-25"><span class="mw-cite-backlink"><a href="#cite_ref-25">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFBruton" class="citation web cs1 cs1-prop-foreign-lang-source">Bruton, D. <a rel="nofollow" class="external text" href="http://www.physics.sfasu.edu/astro/ebstar/ebstar.html">"Eclipsing Binary Stars"</a> (in Engels). Stephen F. Austin-staatsuniversiteit. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20190916161010/http://www.physics.sfasu.edu/astro/ebstar/ebstar.html">Geargiveer</a> vanaf die oorspronklike op 16 September 2019<span class="reference-accessdate">. Besoek op <span class="nowrap">2 April</span> 2015</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Eclipsing+Binary+Stars&rft.pub=Stephen+F.+Austin-staatsuniversiteit&rft.aulast=Bruton&rft.aufirst=D.&rft_id=http%3A%2F%2Fwww.physics.sfasu.edu%2Fastro%2Febstar%2Febstar.html&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-wilson2008-26"><span class="mw-cite-backlink"><a href="#cite_ref-wilson2008_26-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFWilson,_R.E.2008" class="citation journal cs1">Wilson, R.E. (1 Januarie 2008). "Eclipsing Binary Solutions in Physical Units and Direct Distance Estimation". <i>The Astrophysical Journal</i>. <b>672</b> (1). <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2008ApJ...672..575W">2008ApJ...672..575W</a>. <a href="/wiki/Digitale_objek-identifiseerder" title="Digitale objek-identifiseerder">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F523634">10.1086/523634</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=Eclipsing+Binary+Solutions+in+Physical+Units+and+Direct+Distance+Estimation&rft.volume=672&rft.issue=1&rft.date=2008-01-01&rft_id=info%3Adoi%2F10.1086%2F523634&rft_id=info%3Abibcode%2F2008ApJ...672..575W&rft.au=Wilson%2C+R.E.&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> <li id="cite_note-Bonanos2006-27"><span class="mw-cite-backlink"><a href="#cite_ref-Bonanos2006_27-0">↑</a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r2205490"><cite id="CITEREFBonanos,_Alceste_Z.2006" class="citation journal cs1">Bonanos, Alceste Z. (2006). "Eclipsing Binaries: Tools for Calibrating the Extragalactic Distance Scale". <i>Proceedings of the International Astronomical Union</i>. <b>2</b>. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="cs1-lock-free" title="Vrylik beskikbaar"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0610923">astro-ph/0610923</a></span>. <a href="/wiki/Digitale_objek-identifiseerder" title="Digitale objek-identifiseerder">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1017%2FS1743921307003845">10.1017/S1743921307003845</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Proceedings+of+the+International+Astronomical+Union&rft.atitle=Eclipsing+Binaries%3A+Tools+for+Calibrating+the+Extragalactic+Distance+Scale&rft.volume=2&rft.date=2006&rft_id=info%3Aarxiv%2Fastro-ph%2F0610923&rft_id=info%3Adoi%2F10.1017%2FS1743921307003845&rft.au=Bonanos%2C+Alceste+Z.&rfr_id=info%3Asid%2Faf.wikipedia.org%3AVeranderlike+ster" class="Z3988"></span></span> </li> </ol></div> <div class="mw-heading mw-heading2"><h2 id="Eksterne_skakels">Eksterne skakels</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Veranderlike_ster&veaction=edit&section=40" title="Wysig afdeling: Eksterne skakels" class="mw-editsection-visualeditor"><span>wysig</span></a><span class="mw-editsection-divider"> | </span><a href="/w/index.php?title=Veranderlike_ster&action=edit&section=40" title="Edit section's source code: Eksterne skakels"><span>wysig bron</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a rel="nofollow" class="external text" href="http://www.aavso.org/">The American Association of Variable Star Observers</a></li> <li><a rel="nofollow" class="external text" href="http://www.sai.msu.su/gcvs/gcvs/iii/vartype.txt">GCVS Variability Types</a></li> <li><a rel="nofollow" class="external text" href="http://www.popastro.com/sections/vs.htm">Society for Popular Astronomy – Variable Star Section</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20080421150843/http://www.popastro.com/sections/vs.htm">Geargiveer</a> 21 April 2008 op <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a></li></ul> <ul><li><span class="noviewer" typeof="mw:File"><a href="/wiki/L%C3%AAer:Commons-logo.svg" class="mw-file-description" title="Wikimedia Commons logo"><img alt="Wikimedia Commons logo" src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/12px-Commons-logo.svg.png" decoding="async" width="12" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/18px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/24px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></a></span> <a href="/wiki/Wikimedia_Commons" title="Wikimedia Commons">Wikimedia Commons</a> het meer media in die kategorie <a href="https://commons.wikimedia.org/wiki/Category:Variable_stars" class="extiw" title="commons:Category:Variable stars">Veranderlike ster</a>.</li> <li><span typeof="mw:File"><a href="/wiki/L%C3%AAer:Crystal_txt.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Crystal_txt.png/15px-Crystal_txt.png" decoding="async" width="15" height="15" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/Crystal_txt.png/23px-Crystal_txt.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/83/Crystal_txt.png/30px-Crystal_txt.png 2x" data-file-width="64" data-file-height="64" /></a></span> Hierdie artikel is vertaal uit die <a href="https://en.wikipedia.org/wiki/Variable_star" class="extiw" title="en:Variable star">Engelse Wikipedia</a></li></ul> <div role="navigation" class="navbox" aria-labelledby="Soorte_sterre_en_sterregroepe" style="padding:3px"><table class="nowraplinks mw-collapsible expanded navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="3" style="background:#CEDAF2;"><div class="plainlinks hlist navbar mini"><ul><li class="nv-lees"><a href="/wiki/Sjabloon:Sterre" title="Sjabloon:Sterre"><abbr title="Lees hierdie sjabloon" style=";background:#CEDAF2;;background:none transparent;color:inherit;border:none;-moz-box-shadow:none;-webkit-box-shadow:none;box-shadow:none; padding:0;">l</abbr></a></li><li class="nv-bespreek"><a href="/wiki/Sjabloonbespreking:Sterre" title="Sjabloonbespreking:Sterre"><abbr title="Bespreek hierdie sjabloon" style=";background:#CEDAF2;;background:none transparent;color:inherit;border:none;-moz-box-shadow:none;-webkit-box-shadow:none;box-shadow:none; padding:0;">b</abbr></a></li><li class="nv-wysig"><a class="external text" href="https://af.wikipedia.org/w/index.php?title=Sjabloon:Sterre&action=edit"><abbr title="Wysig hierdie sjabloon" style=";background:#CEDAF2;;background:none transparent;color:inherit;border:none;-moz-box-shadow:none;-webkit-box-shadow:none;box-shadow:none; padding:0;">w</abbr></a></li></ul></div><div id="Soorte_sterre_en_sterregroepe" class="vcard" style="font-size:114%;margin:0 4em">Soorte sterre en sterregroepe</div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%;background:none; text-align:left; vertical-align: top; padding-left: 0.5em; padding-right: 0.5em; text-align: right;">Sterre</th><td class="navbox-list navbox-odd hlist" style="text-align:left;border-left-width:2px;border-left-style:solid;width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/Ster" title="Ster">Ster</a></li> <li><a href="/wiki/Hoofreeks" title="Hoofreeks">Dwerg-/hoofreeksster</a></li> <li><a href="/wiki/Rooidwerg" title="Rooidwerg">Rooidwerg</a></li> <li><a href="/wiki/Geeldwerg" title="Geeldwerg">Geeldwerg</a></li> <li><a href="/wiki/Bruindwerg" title="Bruindwerg">Bruindwerg</a></li> <li><a href="/wiki/Witdwerg" title="Witdwerg">Witdwerg</a></li> <li><a href="/wiki/Bloudwerg_(rooidwergstadium)" title="Bloudwerg (rooidwergstadium)">Bloudwerg</a></li> <li><a href="/wiki/Swartdwerg" title="Swartdwerg">Swartdwerg</a></li> <li><a href="/wiki/Subdwergster" title="Subdwergster">Subdwerg</a></li> <li><a href="/wiki/Reusester" title="Reusester">Reusester</a></li> <li><a href="/wiki/Helder_reus" title="Helder reus">Helder reus</a></li> <li><a href="/wiki/Superreus" title="Superreus">Superreus</a></li> <li><a href="/wiki/Hiperreus" title="Hiperreus">Hiperreus</a></li> <li><a href="/wiki/Subreusester" title="Subreusester">Subreus</a></li> <li><a href="/wiki/Rooireus" title="Rooireus">Rooireus</a></li> <li><a href="/wiki/Bloureus" title="Bloureus">Bloureus</a></li> <li><a href="/wiki/Neutronster" title="Neutronster">Neutronster</a></li> <li><a href="/wiki/Kwarkster" title="Kwarkster">Kwarkster</a></li> <li><a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></li> <li><a href="/wiki/Bloudwaalster" title="Bloudwaalster">Bloudwaalster</a></li> <li><a href="/wiki/Cephe%C3%AFed" title="Cepheïed">Cepheïed</a></li> <li><a class="mw-selflink selflink">Veranderlike ster</a></li> <li><a href="/wiki/Opvlamster" title="Opvlamster">Opvlamster</a></li> <li><a href="/wiki/RR_Lyrae-ster" title="RR Lyrae-ster">RR Lyrae-ster</a></li> <li><a href="/wiki/Wolf-Rayetster" title="Wolf-Rayetster"><span style="white-space:nowrap">Wolf-Rayetster</span></a></li> <li><a href="/wiki/Poolster" title="Poolster">Poolster</a></li> <li><a href="/wiki/Skilster" title="Skilster">Skilster</a></li> <li><a href="/wiki/Be-ster" title="Be-ster">Be-ster</a></li> <li><a href="/wiki/O-tipe_ster" class="mw-redirect" title="O-tipe ster"><span style="white-space:nowrap">O-tipe ster</span></a></li> <li><a href="/wiki/B-tipe_ster" class="mw-redirect" title="B-tipe ster"><span style="white-space:nowrap">B-tipe ster</span></a></li> <li><a href="/wiki/A-tipe_ster" class="mw-redirect" title="A-tipe ster"><span style="white-space:nowrap">A-tipe ster</span></a></li> <li><a href="/wiki/F-tipe_ster" class="mw-redirect" title="F-tipe ster"><span style="white-space:nowrap">F-tipe ster</span></a></li> <li><a href="/wiki/G-tipe_ster" class="mw-redirect" title="G-tipe ster"><span style="white-space:nowrap">G-tipe ster</span></a></li> <li><a href="/wiki/K-tipe_ster" class="mw-redirect" title="K-tipe ster"><span style="white-space:nowrap">K-tipe ster</span></a></li> <li><a href="/wiki/M-tipe_ster" class="mw-redirect" title="M-tipe ster"><span style="white-space:nowrap">M-tipe ster</span></a></li> <li><a href="/wiki/Luside" title="Luside">Luside</a></li> <li><a href="/wiki/Sterevolusie" title="Sterevolusie">Sterevolusie</a></li> <li><a href="/wiki/Jong_stervoorwerp" title="Jong stervoorwerp">Jong stervoorwerp</a></li> <li><a href="/wiki/Voorhoofreeksster" title="Voorhoofreeksster">Voorhoofreeksster</a></li> <li><a href="/wiki/T_Tauri-ster" title="T Tauri-ster">T Tauri-ster</a></li> <li><a href="/wiki/Herbig_Ae/Be-ster" title="Herbig Ae/Be-ster">Herbig Ae/Be-ster</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="3" style="width:1px;padding:0px 0px 0px 2px"><div><span typeof="mw:File"><a href="/wiki/L%C3%AAer:HD_820.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/7a/HD_820.jpg/160px-HD_820.jpg" decoding="async" width="160" height="150" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/7a/HD_820.jpg/240px-HD_820.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/7a/HD_820.jpg/320px-HD_820.jpg 2x" data-file-width="2000" data-file-height="1869" /></a></span></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;background:none; text-align:left; vertical-align: top; padding-left: 0.5em; padding-right: 0.5em; text-align: right;">Sterregroepe</th><td class="navbox-list navbox-even hlist" style="text-align:left;border-left-width:2px;border-left-style:solid;width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/Dubbelster" title="Dubbelster">Dubbelster</a></li> <li><a href="/wiki/X-straaldubbelster" title="X-straaldubbelster">X-straaldubbelster</a></li> <li><a href="/wiki/Veelvoudige_ster" title="Veelvoudige ster">Veelvoudige ster</a></li> <li><a href="/wiki/Sterreswerm" title="Sterreswerm">Sterreswerm</a></li> <li><a href="/wiki/Sterkinematika" title="Sterkinematika">Kinematiese groep</a></li> <li><a href="/wiki/Sterassosiasie" title="Sterassosiasie">Sterassosiasie</a></li> <li><a href="/wiki/Bewegingsgroep" title="Bewegingsgroep">Bewegingsgroep</a></li> <li><a href="/wiki/Sterrestroom" title="Sterrestroom">Sterrestroom</a></li> <li><a href="/wiki/Sterrestelsel" title="Sterrestelsel">Sterrestelsel</a></li> <li><a href="/wiki/Melkweg" title="Melkweg">Melkweg</a></li> <li><a href="/wiki/Sterrestelselswerm" title="Sterrestelselswerm">Sterrestelselswerm</a></li> <li><a href="/wiki/Superswerm" title="Superswerm">Superswerm</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;background:none; text-align:left; vertical-align: top; padding-left: 0.5em; padding-right: 0.5em; text-align: right;">Verwante voorwerpe</th><td class="navbox-list navbox-odd hlist" style="text-align:left;border-left-width:2px;border-left-style:solid;width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/Nova" title="Nova">Nova</a></li> <li><a href="/wiki/Supernova" title="Supernova">Supernova</a></li> <li><a href="/wiki/Supernova-oorblyfsel" title="Supernova-oorblyfsel">Supernova-oorblyfsel</a></li> <li><a href="/wiki/Hipernova" title="Hipernova">Hipernova</a></li> <li><a href="/wiki/Newel" title="Newel">Newel</a></li> <li><a href="/wiki/Protoplanet%C3%AAre_skyf" title="Protoplanetêre skyf">Protoplanetêre skyf</a></li> <li><a href="/wiki/Messier-katalogus" title="Messier-katalogus">Messier-voorwerp</a></li> <li><a href="/wiki/Sterrebeeld" title="Sterrebeeld">Sterrebeeld</a> • <a href="/wiki/Sterrepatroon" title="Sterrepatroon">Asterisme</a></li> <li><a href="/wiki/Supermassiewe_swartkolk" title="Supermassiewe swartkolk">Supermassiewe swartkolk</a></li> <li><a href="/wiki/Kwasar" title="Kwasar">Kwasar</a></li> <li><a href="/wiki/Superholte" title="Superholte">Superholte</a></li> <li><a href="/wiki/Molekul%C3%AAre_wolk" title="Molekulêre wolk">Molekulêre wolk</a></li></ul> </div></td></tr></tbody></table></div> <div style="display:none; right:10px;" class="metadata topicon nopopups" id="featured-star"><span typeof="mw:File"><a href="/wiki/Wikipedia:Voorbladartikel" title="Hierdie artikel is gekies as 'n voorbladartikel. 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