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title="我们推荐您创建账号并登录，但这不是强制性的"><span class="vector-icon mw-ui-icon-userAdd mw-ui-icon-wikimedia-userAdd"></span> <span>创建账号</span></a></li><li id="pt-login" class="user-links-collapsible-item mw-list-item"><a href="/w/index.php?title=Special:%E7%94%A8%E6%88%B7%E7%99%BB%E5%BD%95&returnto=%E6%98%9F%E5%86%95" title="建议你登录，尽管并非必须。[o]" accesskey="o"><span class="vector-icon mw-ui-icon-logIn mw-ui-icon-wikimedia-logIn"></span> <span>登录</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"> 未登录编辑者的页面 <a href="/wiki/Help:%E6%96%B0%E6%89%8B%E5%85%A5%E9%97%A8" aria-label="了解有关编辑的更多信息"><span>了解详情</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/Special:%E6%88%91%E7%9A%84%E8%B4%A1%E7%8C%AE" title="来自此IP地址的编辑列表[y]" accesskey="y"><span>贡献</span></a></li><li id="pt-anontalk" class="mw-list-item"><a href="/wiki/Special:%E6%88%91%E7%9A%84%E8%AE%A8%E8%AE%BA%E9%A1%B5" title="对于来自此IP地址编辑的讨论[n]" accesskey="n"><span>讨论</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="站点"> <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="目录" 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">目录</h2> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-pin-button" data-event-name="pinnable-header.vector-toc.pin">移至侧栏</button> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-unpin-button" data-event-name="pinnable-header.vector-toc.unpin">隐藏</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">序言</div> </a> </li> <li id="toc-歷史" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#歷史"> <div class="vector-toc-text"> <span class="vector-toc-numb">1</span> <span>歷史</span> </div> </a> <button aria-controls="toc-歷史-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>开关歷史子章节</span> </button> <ul id="toc-歷史-sublist" class="vector-toc-list"> <li id="toc-歷史上的理論" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#歷史上的理論"> <div class="vector-toc-text"> <span class="vector-toc-numb">1.1</span> <span>歷史上的理論</span> </div> </a> <ul id="toc-歷史上的理論-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-物理性質" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#物理性質"> <div class="vector-toc-text"> <span class="vector-toc-numb">2</span> <span>物理性質</span> </div> </a> <button aria-controls="toc-物理性質-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>开关物理性質子章节</span> </button> <ul id="toc-物理性質-sublist" class="vector-toc-list"> <li id="toc-活躍區" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#活躍區"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1</span> <span>活躍區</span> </div> </a> <ul id="toc-活躍區-sublist" class="vector-toc-list"> <li id="toc-冕環" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#冕環"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1.1</span> <span>冕環</span> </div> </a> <ul id="toc-冕環-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-大型結構" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#大型結構"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1.2</span> <span>大型結構</span> </div> </a> <ul id="toc-大型結構-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-活躍區互連" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#活躍區互連"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1.3</span> <span>活躍區互連</span> </div> </a> <ul id="toc-活躍區互連-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-長絲腔" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#長絲腔"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1.4</span> <span>長絲腔</span> </div> </a> <ul id="toc-長絲腔-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-亮點" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#亮點"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1.5</span> <span>亮點</span> </div> </a> <ul id="toc-亮點-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-冕洞" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#冕洞"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.2</span> <span>冕洞</span> </div> </a> <ul id="toc-冕洞-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-寧靜太陽" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#寧靜太陽"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.3</span> <span>寧靜太陽</span> </div> </a> <ul id="toc-寧靜太陽-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-日冕的變異性" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#日冕的變異性"> <div class="vector-toc-text"> <span class="vector-toc-numb">3</span> <span>日冕的變異性</span> </div> </a> <button aria-controls="toc-日冕的變異性-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>开关日冕的變異性子章节</span> </button> <ul id="toc-日冕的變異性-sublist" class="vector-toc-list"> <li id="toc-閃焰" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#閃焰"> <div class="vector-toc-text"> <span class="vector-toc-numb">3.1</span> <span>閃焰</span> </div> </a> <ul id="toc-閃焰-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-瞬變" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#瞬變"> <div class="vector-toc-text"> <span class="vector-toc-numb">3.2</span> <span>瞬變</span> </div> </a> <ul id="toc-瞬變-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-星冕" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#星冕"> <div class="vector-toc-text"> <span class="vector-toc-numb">4</span> <span>星冕</span> </div> </a> <ul id="toc-星冕-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-日冕的物理" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#日冕的物理"> <div class="vector-toc-text"> <span class="vector-toc-numb">5</span> <span>日冕的物理</span> </div> </a> <button aria-controls="toc-日冕的物理-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>开关日冕的物理子章节</span> </button> <ul id="toc-日冕的物理-sublist" class="vector-toc-list"> <li id="toc-輻射" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#輻射"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1</span> <span>輻射</span> </div> </a> <ul id="toc-輻射-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-熱傳導" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#熱傳導"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2</span> <span>熱傳導</span> </div> </a> <ul id="toc-熱傳導-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-日冕地震學" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#日冕地震學"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3</span> <span>日冕地震學</span> </div> </a> <ul id="toc-日冕地震學-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-日冕加熱問題" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#日冕加熱問題"> <div class="vector-toc-text"> <span class="vector-toc-numb">6</span> <span>日冕加熱問題</span> </div> </a> <button aria-controls="toc-日冕加熱問題-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>开关日冕加熱問題子章节</span> </button> <ul id="toc-日冕加熱問題-sublist" class="vector-toc-list"> <li id="toc-波加熱理論" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#波加熱理論"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.1</span> <span>波加熱理論</span> </div> </a> <ul id="toc-波加熱理論-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-磁重聯理論" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#磁重聯理論"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.2</span> <span>磁重聯理論</span> </div> </a> <ul id="toc-磁重聯理論-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-針狀體（第二型）" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#針狀體（第二型）"> <div class="vector-toc-text"> <span class="vector-toc-numb">6.3</span> <span>針狀體（第二型）</span> </div> </a> <ul id="toc-針狀體（第二型）-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-相關條目" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#相關條目"> <div class="vector-toc-text"> <span class="vector-toc-numb">7</span> <span>相關條目</span> </div> </a> <ul id="toc-相關條目-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-參考資料" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#參考資料"> <div class="vector-toc-text"> <span class="vector-toc-numb">8</span> <span>參考資料</span> </div> </a> <ul id="toc-參考資料-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-進階讀物" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#進階讀物"> <div class="vector-toc-text"> <span class="vector-toc-numb">9</span> <span>進階讀物</span> </div> </a> <ul id="toc-進階讀物-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-外部連結" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#外部連結"> <div class="vector-toc-text"> <span class="vector-toc-numb">10</span> <span>外部連結</span> </div> </a> <ul id="toc-外部連結-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="目录" 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="开关目录" > <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">开关目录</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">星冕</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="前往另一种语言写成的文章。9种语言可用" > <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-9" 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">9种语言</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%87%D8%A7%D9%84%D8%A9_%D9%86%D8%AC%D9%85%D9%8A%D8%A9" title="هالة نجمية – 阿拉伯语" lang="ar" hreflang="ar" data-title="هالة نجمية" data-language-autonym="العربية" data-language-local-name="阿拉伯语" class="interlanguage-link-target"><span>العربية</span></a></li><li class="interlanguage-link interwiki-en mw-list-item"><a href="https://en.wikipedia.org/wiki/Stellar_corona" title="Stellar corona – 英语" lang="en" hreflang="en" data-title="Stellar corona" data-language-autonym="English" data-language-local-name="英语" class="interlanguage-link-target"><span>English</span></a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%AA%D8%A7%D8%AC_%D8%B3%D8%AA%D8%A7%D8%B1%D9%87%E2%80%8C%D8%A7%DB%8C" title="تاج ستاره‌ای – 波斯语" lang="fa" hreflang="fa" data-title="تاج ستاره‌ای" data-language-autonym="فارسی" data-language-local-name="波斯语" class="interlanguage-link-target"><span>فارسی</span></a></li><li class="interlanguage-link interwiki-ig mw-list-item"><a href="https://ig.wikipedia.org/wiki/Okpueze_kpakpando" title="Okpueze kpakpando – 伊博语" lang="ig" hreflang="ig" data-title="Okpueze kpakpando" data-language-autonym="Igbo" data-language-local-name="伊博语" class="interlanguage-link-target"><span>Igbo</span></a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%85%D0%B2%D0%B5%D0%B7%D0%B4%D0%B5%D0%BD%D0%B0_%D0%BA%D0%BE%D1%80%D0%BE%D0%BD%D0%B0" title="Ѕвездена корона – 马其顿语" lang="mk" hreflang="mk" data-title="Ѕвездена корона" data-language-autonym="Македонски" data-language-local-name="马其顿语" class="interlanguage-link-target"><span>Македонски</span></a></li><li class="interlanguage-link interwiki-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Coroa_estelar" title="Coroa estelar – 葡萄牙语" lang="pt" hreflang="pt" data-title="Coroa estelar" data-language-autonym="Português" data-language-local-name="葡萄牙语" class="interlanguage-link-target"><span>Português</span></a></li><li class="interlanguage-link interwiki-ru mw-list-item"><a href="https://ru.wikipedia.org/wiki/%D0%97%D0%B2%D1%91%D0%B7%D0%B4%D0%BD%D0%B0%D1%8F_%D0%BA%D0%BE%D1%80%D0%BE%D0%BD%D0%B0" title="Звёздная корона – 俄语" lang="ru" hreflang="ru" data-title="Звёздная корона" data-language-autonym="Русский" data-language-local-name="俄语" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-sw mw-list-item"><a href="https://sw.wikipedia.org/wiki/Kitanga_cha_nyota" title="Kitanga cha nyota – 斯瓦希里语" lang="sw" hreflang="sw" data-title="Kitanga cha nyota" data-language-autonym="Kiswahili" data-language-local-name="斯瓦希里语" 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%B5%E0%AE%BF%E0%AE%A3%E0%AF%8D%E0%AE%AE%E0%AF%80%E0%AE%A9%E0%AF%8D_%E0%AE%AA%E0%AF%81%E0%AE%B1%E0%AE%A3%E0%AE%BF" title="விண்மீன் புறணி – 泰米尔语" lang="ta" hreflang="ta" data-title="விண்மீன் புறணி" data-language-autonym="தமிழ்" data-language-local-name="泰米尔语" class="interlanguage-link-target"><span>தமிழ்</span></a></li> </ul> <div class="after-portlet after-portlet-lang"><span class="wb-langlinks-edit wb-langlinks-link"><a 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class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/cd/Zh_conversion_icon_m.svg/53px-Zh_conversion_icon_m.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/cd/Zh_conversion_icon_m.svg/70px-Zh_conversion_icon_m.svg.png 2x" data-file-width="32" data-file-height="20" /></span></span></div></div> </div> <div id="siteSub" class="noprint">维基百科，自由的百科全书</div> </div> <div id="contentSub"><div id="mw-content-subtitle"></div></div> <div id="mw-content-text" class="mw-body-content"><div class="mw-content-ltr mw-parser-output" lang="zh" dir="ltr"><div id="noteTA-3696a9fc" class="noteTA"><div class="noteTA-group"><div data-noteta-group-source="module" data-noteta-group="Astronomy"></div></div></div> <style data-mw-deduplicate="TemplateStyles:r84833064">.mw-parser-output .hatnote{font-size:small}.mw-parser-output div.hatnote{padding-left:2em;margin-bottom:0.8em;margin-top:0.8em}.mw-parser-output .hatnote-notice-img::after{content:"\202f \202f \202f \202f "}.mw-parser-output .hatnote-notice-img-small::after{content:"\202f \202f "}.mw-parser-output .hatnote+link+.hatnote{margin-top:-0.5em}body.skin-minerva .mw-parser-output .hatnote-notice-img,body.skin-minerva .mw-parser-output .hatnote-notice-img-small{display:none}@media print{body.ns-0 .mw-parser-output .hatnote{display:none!important}}</style><div role="note" class="hatnote navigation-not-searchable"><span typeof="mw:File"><a href="/wiki/Wikipedia:%E6%B6%88%E6%AD%A7%E4%B9%89" title="Wikipedia:消歧义"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/Disambig_gray.svg/25px-Disambig_gray.svg.png" decoding="async" width="25" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/Disambig_gray.svg/38px-Disambig_gray.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5f/Disambig_gray.svg/50px-Disambig_gray.svg.png 2x" data-file-width="220" data-file-height="168" /></a></span><style data-mw-deduplicate="TemplateStyles:r74069148">body:not(.skin-minerva) .mw-parser-output .ifmobile>.mobile{display:none}body.skin-minerva .mw-parser-output .ifmobile>.nomobile{display:inherit;display:initial}</style><span class="ifmobile"><span class="nomobile">  </span><span class="mobile"></span></span>此條目介紹的是天文學項目。关于其它用法，请见「<b><a href="/wiki/%E5%86%95_(%E6%B6%88%E6%AD%A7%E7%BE%A9)" class="mw-disambig" title="冕 (消歧義)">冕 (消歧義)</a></b>」。</div> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:Solar_eclipse_1999_4.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Solar_eclipse_1999_4.jpg/220px-Solar_eclipse_1999_4.jpg" decoding="async" width="220" height="217" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Solar_eclipse_1999_4.jpg/330px-Solar_eclipse_1999_4.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Solar_eclipse_1999_4.jpg/440px-Solar_eclipse_1999_4.jpg 2x" data-file-width="3543" data-file-height="3489" /></a><figcaption>在1999年8月11日的日全食影像。在全食階段，可以用<a href="/wiki/%E8%82%89%E7%9C%BC" title="肉眼">肉眼</a>看見日冕和凸出於太陽邊緣的<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a>。</figcaption></figure> <p><b>星冕</b>或<b>冕</b>是環繞<a href="/wiki/%E6%81%86%E6%98%9F" class="mw-redirect" title="恆星">恆星</a>周圍的<a href="/wiki/%E7%AD%89%E9%9B%A2%E5%AD%90%E9%AB%94" class="mw-redirect" title="等離子體">電漿</a>光環，環繞<a href="/wiki/%E5%A4%AA%E9%99%BD" class="mw-redirect" title="太陽">太陽</a>的稱為<b>日冕</b>。太陽的日冕在每一次的<a href="/wiki/%E6%97%A5%E9%A3%9F" title="日食">日全食</a>中都很容易看到；平時也可以透過<a href="/wiki/%E6%97%A5%E5%86%95%E4%BB%AA" title="日冕仪">日冕儀</a>觀測。英文的<i>冕</i> （<i>corona</i>）這個詞源自<a href="/wiki/%E6%8B%89%E4%B8%81%E6%96%87" class="mw-redirect" title="拉丁文">拉丁文</a>的<i>crown</i>，意思是<i>冠</i>，再追溯則為<a href="/wiki/%E5%8F%A4%E5%B8%8C%E8%87%98" class="mw-redirect" title="古希臘">古希臘</a>的κορώνη（korōnè，意思為“花環<i>、</i>花冠”）。 </p><p><a href="/wiki/%E5%A4%AA%E9%99%BD" class="mw-redirect" title="太陽">太陽</a>的日冕位於<a href="/wiki/%E8%89%B2%E7%90%83%E5%B1%82" class="mw-redirect" title="色球层">色球層</a>上方，延伸到外層空間數百萬公里。<a href="/wiki/%E5%85%89%E8%AD%9C" class="mw-redirect" title="光譜">光譜</a>測量表明日冕中的溫度超過<span style="white-space:nowrap">1<span style="margin-left:0.25em">000</span><span style="margin-left:0.25em">000 <a href="/wiki/%E7%86%B1%E5%8A%9B%E5%AD%B8%E6%BA%AB%E6%A8%99" class="mw-redirect" title="熱力學溫標">K</a></span></span>，是強<a href="/wiki/%E9%9B%BB%E9%9B%A2" class="mw-redirect" title="電離">電離</a>的電漿<sup id="cite_ref-Aschwanden_1-0" class="reference"><a href="#cite_note-Aschwanden-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup>，比被稱為太陽表面的<a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球</a>熱得多。 </p><p>來自日冕的光有三個主要的來源，而且都來自空間中相同的區域。 </p><p>K冕：源自德語的<i>kontinuierlich</i>，意思是<i>連續</i>，它是陽光經由自由<a href="/wiki/%E9%9B%BB%E5%AD%90" class="mw-redirect" title="電子">電子</a>的<a href="/wiki/%E6%B9%AF%E5%A7%86%E6%A3%AE%E6%95%A3%E5%B0%84" class="mw-redirect" title="湯姆森散射">湯姆森散射</a>造成的。來自光球層的可見光，在日冕中被電漿吸收產生的<a href="/wiki/%E8%AD%9C%E7%B7%9A" title="譜線">吸收譜線</a>，因為強大的<a href="/wiki/%E5%A4%9A%E6%99%AE%E5%8B%92%E8%87%B4%E5%AE%BD" class="mw-redirect" title="多普勒致宽">都卜勒致寬</a>的擴散，使被反射的光球層吸收線完全被遮蔽掉，造成光譜的外觀呈現沒有吸收譜線的連續光譜。 </p><p>F冕：因<a href="/wiki/%E7%B4%84%E7%91%9F%E5%A4%AB%C2%B7%E5%A4%AB%E6%9C%97%E5%92%8C%E6%96%90" class="mw-redirect" title="約瑟夫·夫朗和斐">約瑟夫·夫朗和斐</a>而得名，是由被塵埃反射的太陽光所產生，並且可以被觀測到。因為它的光包含了在原始的陽光中可以看到的夫朗和斐吸收譜線而得名。它從太陽延伸到非常大的<a href="/wiki/%E8%B7%9D%E8%A7%92" title="距角">離日度</a>，就會被稱為<a href="/wiki/%E9%BB%83%E9%81%93%E5%85%89" title="黃道光">黃道光</a>。 </p><p>E冕：也稱為發射冕（E為發射），是由存在日冕電漿中的<a href="/wiki/%E9%9B%A2%E5%AD%90" class="mw-redirect" title="離子">離子</a>產生的光譜發射線。它可以被觀測到是寬譜線、<a href="/wiki/%E7%A6%81%E7%B7%9A" class="mw-redirect" title="禁線">禁線</a>或是熱<a href="/wiki/%E8%AD%9C%E7%B7%9A" title="譜線">發射線</a>，並且是日冕成分的主要資訊來源<sup id="cite_ref-Corfield_2-0" class="reference"><a href="#cite_note-Corfield-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup>。 </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="歷史"><span id=".E6.AD.B7.E5.8F.B2"></span>歷史</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=1" title="编辑章节：歷史"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Solar_eclipse_1806Jun16-Corona-Ferrer.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Solar_eclipse_1806Jun16-Corona-Ferrer.png/220px-Solar_eclipse_1806Jun16-Corona-Ferrer.png" decoding="async" width="220" height="218" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Solar_eclipse_1806Jun16-Corona-Ferrer.png/330px-Solar_eclipse_1806Jun16-Corona-Ferrer.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/6f/Solar_eclipse_1806Jun16-Corona-Ferrer.png/440px-Solar_eclipse_1806Jun16-Corona-Ferrer.png 2x" data-file-width="1405" data-file-height="1395" /></a><figcaption><span class="ilh-all" data-orig-title="何塞·华金·德费雷尔" data-lang-code="en" data-lang-name="英语" data-foreign-title="José Joaquín de Ferrer"><span class="ilh-page"><a href="/w/index.php?title=%E4%BD%95%E5%A1%9E%C2%B7%E5%8D%8E%E9%87%91%C2%B7%E5%BE%B7%E8%B4%B9%E9%9B%B7%E5%B0%94&action=edit&redlink=1" class="new" title="何塞·华金·德费雷尔（页面不存在）">何塞·华金·德费雷尔</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Jos%C3%A9_Joaqu%C3%ADn_de_Ferrer" class="extiw" title="en:José Joaquín de Ferrer"><span lang="en" dir="auto">José Joaquín de Ferrer</span></a></span>）</span></span>於<a href="/wiki/1806%E5%B9%B46%E6%9C%8816%E6%97%A5%E6%97%A5%E9%A3%9F" title="1806年6月16日日食">1806年6月16日日食</a>在紐約<a href="/wiki/%E9%87%91%E5%BE%B7%E8%83%A1%E5%85%8B" title="金德胡克">金德胡克</a>素描的日冕。</figcaption></figure> <p>在1724年，法-義天文學家<span class="ilh-all" data-orig-title="詹姆斯·馬拉爾迪" data-lang-code="en" data-lang-name="英语" data-foreign-title="Giacomo F. Maraldi"><span class="ilh-page"><a href="/w/index.php?title=%E8%A9%B9%E5%A7%86%E6%96%AF%C2%B7%E9%A6%AC%E6%8B%89%E7%88%BE%E8%BF%AA&action=edit&redlink=1" class="new" title="詹姆斯·馬拉爾迪（页面不存在）">詹姆斯·馬拉爾迪</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Giacomo_F._Maraldi" class="extiw" title="en:Giacomo F. Maraldi"><span lang="en" dir="auto">Giacomo F. Maraldi</span></a></span>）</span></span>認識到在<a href="/wiki/%E6%97%A5%E9%A3%9F" title="日食">日食</a>期間可見的光環屬於<a href="/wiki/%E5%A4%AA%E9%99%BD" class="mw-redirect" title="太陽">太陽</a>，而不是<a href="/wiki/%E6%9C%88%E7%90%83" title="月球">月球</a><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>。在1809年，西班牙天文學家<span class="ilh-all" data-orig-title="何塞·华金·德费雷尔" data-lang-code="en" data-lang-name="英语" data-foreign-title="José Joaquín de Ferrer"><span class="ilh-page"><a href="/w/index.php?title=%E4%BD%95%E5%A1%9E%C2%B7%E5%8D%8E%E9%87%91%C2%B7%E5%BE%B7%E8%B4%B9%E9%9B%B7%E5%B0%94&action=edit&redlink=1" class="new" title="何塞·华金·德费雷尔（页面不存在）">何塞·华金·德费雷尔</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Jos%C3%A9_Joaqu%C3%ADn_de_Ferrer" class="extiw" title="en:José Joaquín de Ferrer"><span lang="en" dir="auto">José Joaquín de Ferrer</span></a></span>）</span></span>創造了<b>日冕</b>一詞<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>。1806年，德費雷爾依據自己在紐約<a href="/wiki/%E9%87%91%E5%BE%B7%E8%83%A1%E5%85%8B" title="金德胡克">金德胡克</a>的觀測，也提出日冕是太陽的一部分，而不是月球的一部分。英國天文學家<a href="/wiki/%E7%BA%A6%E7%91%9F%E5%A4%AB%C2%B7%E8%AF%BA%E6%9B%BC%C2%B7%E6%B4%9B%E5%85%8B%E8%80%B6" title="约瑟夫·诺曼·洛克耶">约瑟夫·诺曼·洛克耶</a>確定太陽色球中有一種地球上未知的元素，現在該元素被稱為<a href="/wiki/%E6%B0%A6" title="氦">氦</a>。法國天文學家<a href="/wiki/%E7%9A%AE%E5%9F%83%E5%B0%94%C2%B7%E8%AE%A9%E6%A3%AE" title="皮埃尔·让森">皮埃尔·让森</a>指出，日冕的大小和形狀會隨著<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽黑子週期</a>的變化而變化<sup id="cite_ref-5" class="reference"><a href="#cite_note-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup>。在1930年，<a href="/wiki/%E8%B2%9D%E7%88%BE%E7%B4%8D%C2%B7%E8%B2%BB%E8%BF%AA%E5%8D%97%C2%B7%E6%9D%8E%E5%A5%A7" title="貝爾納·費迪南·李奧">伯納德·李奧特</a>發明了<a href="/wiki/%E6%97%A5%E5%86%95%E4%BB%AA" title="日冕仪">日冕儀</a>，能夠在沒有日全食的情況下看見日冕。在1952年，美國天文學家<a href="/wiki/%E5%B0%A4%E9%87%91%C2%B7%E6%B4%BE%E5%85%8B" title="尤金·派克">尤金·派克</a>認為太陽的日冕可能是被類似閃焰，但覆蓋在整個太陽表面，微型、明亮且無以計數的<i>納米閃焰</i>加熱。 </p> <div class="mw-heading mw-heading3"><h3 id="歷史上的理論"><span id=".E6.AD.B7.E5.8F.B2.E4.B8.8A.E7.9A.84.E7.90.86.E8.AB.96"></span>歷史上的理論</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=2" title="编辑章节：歷史上的理論"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>太陽日冕的高溫給了它不尋常的<a href="/wiki/%E5%85%89%E8%AD%9C" class="mw-redirect" title="光譜">光譜</a>特徵，導致在19世紀認為它包含一種以前未知的元素：<a href="/wiki/%F0%B0%9B%82" title="𰛂"><span class="inline-unihan" style="border-bottom: 1px dotted; font-variant: normal;cursor: help; font-family: sans-serif, 'FZSongS-Extended', 'FZSongS-Extended(SIP)', 'WenQuanYi Zen Hei Mono', 'BabelStone Han', 'HanaMinB', 'FZSong-Extended', 'Arial Unicode MS', Code2002, DFSongStd, 'STHeiti SC', unifont, SimSun-ExtB, TH-Tshyn-P0, TH-Tshyn-P1, TH-Tshyn-P2, Jigmo3, Jigmo2, Jigmo, ZhongHuaSongPlane15, ZhongHuaSongPlane02, ZhongHuaSongPlane00, 'Plangothic P1', 'Plangothic P2';" title="字符描述：⿹气免 
※如果您看到空白、方塊或問號，代表您的系統無法顯示此字元。">𰛂</span></a> (<i><span lang="en">coronium</span></i>)。實際上，這些譜線特徵後來被解釋為<a href="/wiki/%E9%AB%98%E7%94%B5%E8%8D%B7%E6%80%81%E7%A6%BB%E5%AD%90" title="高电荷态离子">高電荷態離子</a><a href="/wiki/%E9%90%B5" class="mw-redirect" title="鐵">鐵</a>（Fe-XIV或Fe<sup>13+</sup>）。<span class="ilh-all" data-orig-title="約翰·埃德倫" data-lang-code="en" data-lang-name="英语" data-foreign-title="Bengt Edlén"><span class="ilh-page"><a href="/w/index.php?title=%E7%B4%84%E7%BF%B0%C2%B7%E5%9F%83%E5%BE%B7%E5%80%AB&action=edit&redlink=1" class="new" title="約翰·埃德倫（页面不存在）">約翰·埃德倫</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Bengt_Edl%C3%A9n" class="extiw" title="en:Bengt Edlén"><span lang="en" dir="auto">Bengt Edlén</span></a></span>）</span></span>，繼Grotrian（1939年）之後，在1940年（觀測始於1869年）首次確認了日冕的譜線，是從高度電離的<a href="/wiki/%E4%BA%9A%E7%A8%B3%E6%80%81" class="mw-redirect" title="亚稳态">亚稳态</a>回到低能階的基態（綠色的5303 Å 線是來自Fe<sup>13+</sup>，Fe-XIV；紅色的6374 Å 來自Fe<sup> 9 + </sup>,Fe-X）<sup id="cite_ref-Aschwanden_1-1" class="reference"><a href="#cite_note-Aschwanden-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading2"><h2 id="物理性質"><span id=".E7.89.A9.E7.90.86.E6.80.A7.E8.B3.AA"></span>物理性質</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=3" title="编辑章节：物理性質"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Twistedflux.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/2a/Twistedflux.png/220px-Twistedflux.png" decoding="async" width="220" height="149" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/2/2a/Twistedflux.png/330px-Twistedflux.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/2/2a/Twistedflux.png/440px-Twistedflux.png 2x" data-file-width="541" data-file-height="367" /></a><figcaption>展示太陽週期中太陽磁流結構的繪圖。</figcaption></figure> <p>太陽的日冕比可見的太陽表面要熱得多（150至450倍）：<a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球</a>的平均<a href="/wiki/%E6%BA%AB%E5%BA%A6" class="mw-redirect" title="溫度">溫度</a>是5,800<a href="/wiki/%E7%86%B1%E5%8A%9B%E5%AD%B8%E6%BA%AB%E6%A8%99" class="mw-redirect" title="熱力學溫標">K</a>，而日冕的是100萬至300萬K。但是，日冕的密度是光球密度的10 <sup>-12 </sup>倍，因此產生的可見光約只是光球的百萬分之一。日冕和光球被相對較薄的一層<a href="/wiki/%E8%89%B2%E7%90%83" title="色球">色球</a>分隔開來。日冕加熱的確實機制仍然是有爭論的議題，其可能的機制包括後面將論述的太陽<a href="/wiki/%E7%A3%81%E5%A0%B4" title="磁場">磁場</a>和<a href="/wiki/%E7%A3%81%E6%B5%81%E9%AB%94%E5%8A%9B%E5%AD%B8" class="mw-redirect" title="磁流體力學">磁流體力學</a>。由於磁場是開放的，日冕外緣不斷的流失，從而產生<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%A2%A8" class="mw-redirect" title="太陽風">太陽風</a>。 </p><p>日冕在太陽表面的分布並不總是平均的。在寧靜的時期，日冕或多或少的局限在<a href="/wiki/%E8%B5%A4%E9%81%93" title="赤道">赤道</a>的區域，<a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a>覆蓋在<a href="/wiki/%E5%9C%B0%E7%90%86%E6%A5%B5%E9%BB%9E" title="地理極點">極區</a>的區域。然而，在活躍的時期，雖然最突出的是<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%BB%91%E5%AD%90" class="mw-redirect" title="太陽黑子">太陽黑子</a>活躍區，但日冕均勻的分佈在赤道和極區。<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽週期</a>從<a href="/wiki/%E5%A4%AA%E9%99%BD%E6%A5%B5%E5%B0%8F%E6%9C%9F" title="太陽極小期">太陽極小期</a>到下個極小期,大約跨越11年。由於太陽的赤道自轉的比極區快（<a href="/wiki/%E8%BC%83%E5%B7%AE%E8%87%AA%E8%BD%89" class="mw-redirect" title="較差自轉">較差自轉</a>），太陽的磁場不斷的隨著物質紐攪，在<a href="/wiki/%E5%A4%AA%E9%99%BD%E6%A5%B5%E5%A4%A7%E6%9C%9F" title="太陽極大期">太陽極大期</a>時，<a href="/wiki/%E7%A3%81%E5%A0%B4" title="磁場">磁場</a>受到的糾結最為強烈，太陽黑子的活動也最為明顯。與太陽黑子相關的<a href="/wiki/%E5%86%95%E7%92%B0" title="冕環">冕環</a>，<a href="/wiki/%E7%A3%81%E9%80%9A%E9%87%8F" title="磁通量">磁通量</a>的迴路，是來自太陽內部的上升流。這些磁通量將較熱的光球推向旁邊，曝露出下面較冷的電漿，從而產生相對較暗的太陽黑子。 </p><p>由於<a href="/wiki/%E5%A4%A9%E7%A9%BA%E5%AE%9E%E9%AA%8C%E5%AE%A4" title="天空实验室">天空實驗室</a>於1973年在光譜的X射線波段上拍攝到高解析的日冕，並且之後的<a href="/wiki/%E9%99%BD%E5%85%89%E8%A1%9B%E6%98%9F" class="mw-redirect" title="陽光衛星">陽光衛星</a>和後續的其它太空儀器也都拍攝到，因此人們才知道日冕的結構千變萬化，而且複雜：不同的區域在分類上有不同的冕盤<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-7" class="reference"><a href="#cite_note-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-8" class="reference"><a href="#cite_note-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup>。天文學家通常會分出的區域<sup id="cite_ref-Gibson_9-0" class="reference"><a href="#cite_note-Gibson-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup>，如下所述。 </p> <div class="mw-heading mw-heading3"><h3 id="活躍區"><span id=".E6.B4.BB.E8.BA.8D.E5.8D.80"></span>活躍區</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=4" title="编辑章节：活躍區"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E6%B4%BB%E8%BA%8D%E5%8D%80" title="活躍區">活躍區</a></div> <p><b>活躍區</b>是光球中連接相反磁極點的迴路，即所謂的<a href="/wiki/%E5%86%95%E7%92%B0" title="冕環">冕環</a>結構的集合。 </p><p>它們通常分布在兩個活躍區，而這兩個活躍區與太陽赤道大致上是平行的。平均溫度在200萬至400萬K之間，而密度從每立方公分10 <sup> 9 </sup>到10 <sup> 10 </sup>個顆粒。 </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Prominence_(PSF).png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/03/Prominence_%28PSF%29.png/220px-Prominence_%28PSF%29.png" decoding="async" width="220" height="88" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/03/Prominence_%28PSF%29.png/330px-Prominence_%28PSF%29.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/03/Prominence_%28PSF%29.png/440px-Prominence_%28PSF%29.png 2x" data-file-width="3636" data-file-height="1452" /></a><figcaption><a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">太陽日珥</a>和<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%BB%91%E5%AD%90" class="mw-redirect" title="太陽黑子">太陽黑子</a>的圖解。</figcaption></figure> <p>活躍區涉及與磁場直接相關的所有現象，在太陽表面上不同高度的磁場引發不同的現象<sup id="cite_ref-Gibson_9-1" class="reference"><a href="#cite_note-Gibson-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup>：<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%BB%91%E5%AD%90" class="mw-redirect" title="太陽黑子">太陽黑子</a>和<a href="/wiki/%E5%85%89%E6%96%91" title="光斑">光斑</a>發生在<a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球</a>中，<a href="/wiki/%E9%87%9D%E7%8B%80%E9%AB%94" title="針狀體">針狀體</a>、<a href="/wiki/H-%CE%B1" title="H-α">Hα</a>、<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">暗條</a>、和<a href="/wiki/%E8%AD%9C%E6%96%91" title="譜斑">譜斑</a>在色球中，<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a>從色球穿越過度區，<a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a>和<a href="/wiki/%E6%97%A5%E5%86%95%E7%89%A9%E8%B3%AA%E6%8B%8B%E5%B0%84" class="mw-redirect" title="日冕物質拋射">日冕物質拋射</a>發生在日冕和色球。如果閃焰非常猛烈，還會干擾到色球，並且產生<a href="/wiki/%E8%8E%AB%E7%88%BE%E9%A0%93%E6%B3%A2" title="莫爾頓波">莫爾頓波</a>。相對的，靜態日珥是在太陽盤面上被觀察到的黑色、蛇形的Hα絲帶（看起來像暗條），是巨大、較低溫的誌密結構。它們的溫度約為5,000至8,000K，因而通常被認為是色球的特徵。 </p><p>在2013年，來自<span class="ilh-all" data-orig-title="高解析度日冕成像儀" data-lang-code="en" data-lang-name="英语" data-foreign-title="High Resolution Coronal Imager"><span class="ilh-page"><a href="/w/index.php?title=%E9%AB%98%E8%A7%A3%E6%9E%90%E5%BA%A6%E6%97%A5%E5%86%95%E6%88%90%E5%83%8F%E5%84%80&action=edit&redlink=1" class="new" title="高解析度日冕成像儀（页面不存在）">高解析度日冕成像儀</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/High_Resolution_Coronal_Imager" class="extiw" title="en:High Resolution Coronal Imager"><span lang="en" dir="auto">High Resolution Coronal Imager</span></a></span>）</span></span>的圖像揭露了這些活躍區的外層內有所未知的電漿“磁性辮子”<sup id="cite_ref-10" class="reference"><a href="#cite_note-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading4"><h4 id="冕環"><span id=".E5.86.95.E7.92.B0"></span>冕環</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=5" title="编辑章节：冕環"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E5%86%95%E7%92%B0" title="冕環">冕環</a></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Traceimage.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/93/Traceimage.jpg/220px-Traceimage.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/93/Traceimage.jpg/330px-Traceimage.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/93/Traceimage.jpg/440px-Traceimage.jpg 2x" data-file-width="768" data-file-height="768" /></a><figcaption>TRACE 171Å 的冕環</figcaption></figure> <p><a href="/wiki/%E5%86%95%E7%92%B0" title="冕環">冕環</a>是磁性太陽日冕的基本結構。這些環圈的是封閉性磁通量，和在<a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a>區中發現的開放性磁通量的<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%A2%A8" class="mw-redirect" title="太陽風">太陽風</a>是堂兄弟。由太陽內部產生的磁通量環圈充滿了炙熱的太陽電漿<sup id="cite_ref-11" class="reference"><a href="#cite_note-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup>。由於這些冕環區域的磁活性增強，通常是<a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a>和<a href="/wiki/%E6%97%A5%E5%86%95%E7%89%A9%E8%B3%AA%E6%8B%8B%E5%B0%84" class="mw-redirect" title="日冕物質拋射">日冕物質拋射</a>（CME）的前兆。 </p><p>這些餵飽冕環的太陽電漿，從溫度低於6000K的光球，經過過渡區進入日冕時，已經被加熱至10<sup>6</sup>K。通常情況下，這些電漿會因為壓力差從一個點，稱為足點（<a href="/wiki/%E8%99%B9%E5%90%B8" title="虹吸">虹吸</a><sup id="cite_ref-12" class="reference"><a href="#cite_note-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup>或由於其它因素驅動的不對稱流），排放至另一個點。 </p><p>當電漿由足點上升到環圈頂端時，就像緻密的閃焰初始階段總會發生的那樣，被定義為色球<a href="/wiki/%E8%92%B8%E7%99%BC" class="mw-redirect" title="蒸發">蒸發</a>。當電漿迅速冷卻並落回光球時，它被稱為色球<a href="/wiki/%E5%87%9D%E7%B5%90" title="凝結">凝聚區</a>。也可能有從兩個足點<a href="/wiki/%E5%B0%8D%E7%A8%B1" title="對稱">對稱</a>的流動，造成物質在環圈結構中的累積。電漿可能在這樣的區域迅速冷卻（因為熱不穩定），它黑暗的<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">暗條</a>與太陽盤面或<a href="/wiki/%E5%91%A8%E9%82%8A%E6%98%8F%E6%9A%97" title="周邊昏暗">邊緣</a>的<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a>形成明顯的對比。 </p><p>冕環的生命期可能能以秒（在閃焰事件的情況下）、分鐘、小時或天的等級來排序。當冕環的能量來源和支出能平衡的情況下，冕環可以持續很長的時間並被稱為<i><a href="/wiki/%E7%A9%A9%E6%85%8B_(%E7%B3%BB%E7%B5%B1)" title="穩態 (系統)">穩態 (系統)</a></i>或<i><a href="https://zh.wiktionary.org/wiki/quiescent" class="extiw" title="wikt:quiescent">靜止</a></i>冕環（<a href="/wiki/File:Energyfig.png" title="File:Energyfig.png">例子</a>）。 </p><p>冕環對我們理解當前的<i>日冕加熱問題</i>非常重要。冕環是電漿的高度輻射源，因此<i><a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">TRACE</a></i>等儀器很容易觀察到。但因為這些都是在遠端觀測，結構都有模糊之處（即沿<a href="/wiki/%E8%A6%96%E7%B7%9A%E5%82%B3%E6%92%AD" class="mw-redirect" title="視線傳播">視線傳播</a>貢獻的輻射），因此日冕加熱的解釋仍然有問題存在。<i><a href="/wiki/In_situ" title="In situ">現場</a></i>的測量是必要的，只有這樣才能得到明確的答案。但由於日冕電漿的高溫，"現場"測量在目前是不可能的。目前NASA進行的<a href="/wiki/%E6%B4%BE%E5%85%8B%E5%A4%AA%E9%99%BD%E6%8E%A2%E6%B8%AC%E5%99%A8" title="派克太陽探測器">派克太陽探測器</a>將更密切的接近太陽，也只能夠在較接近的距離進行觀測。 </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Coronal_Hole_Magnetic_Field_Lines.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/09/Coronal_Hole_Magnetic_Field_Lines.svg/220px-Coronal_Hole_Magnetic_Field_Lines.svg.png" decoding="async" width="220" height="398" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/09/Coronal_Hole_Magnetic_Field_Lines.svg/330px-Coronal_Hole_Magnetic_Field_Lines.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/09/Coronal_Hole_Magnetic_Field_Lines.svg/440px-Coronal_Hole_Magnetic_Field_Lines.svg.png 2x" data-file-width="151" data-file-height="273" /></a><figcaption>(A)是冕環連接相對的磁極；(B)是單一磁極的冕洞區域。</figcaption></figure> <div class="mw-heading mw-heading4"><h4 id="大型結構"><span id=".E5.A4.A7.E5.9E.8B.E7.B5.90.E6.A7.8B"></span>大型結構</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=6" title="编辑章节：大型結構"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p><b>大型結構</b>是非常長的弧線，可以跨越四分之一以上的太陽盤面，但包含的電漿密度低於活躍區域的冕環。 </p><p>它們最早是在1968年6月8日的火箭飛行期間的閃焰觀測中被發現的<sup id="cite_ref-Giacconi_13-0" class="reference"><a href="#cite_note-Giacconi-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup>。 </p><p>日冕的大型結構在11年的<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽週期</a>間會發生變化，在太陽磁場幾乎類似雙極結構（加上四極成分）的極小期時，變得特別簡單。 </p> <div class="mw-heading mw-heading4"><h4 id="活躍區互連"><span id=".E6.B4.BB.E8.BA.8D.E5.8D.80.E4.BA.92.E9.80.A3"></span>活躍區互連</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=7" title="编辑章节：活躍區互連"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p><b> 活躍區互連 </b>是不同活躍區域的相對磁場的弧形連接區。這些結構的重大變化往往是在閃焰發生之後看到的<style data-mw-deduplicate="TemplateStyles:r83946278">.mw-parser-output .template-facttext{background-color:var(--background-color-neutral,#eaecf0);color:inherit;margin:-.3em 0;padding:.3em 0}</style><sup class="noprint Template-Fact"><a href="/wiki/Wikipedia:%E5%88%97%E6%98%8E%E6%9D%A5%E6%BA%90" title="Wikipedia:列明来源"><span style="white-space: nowrap;" title="来源请求。">[來源請求]</span></a></sup>。 </p><p>類似的其他特徵是<a href="/wiki/%E7%9B%94%E7%8B%80%E6%B5%81" title="盔狀流">盔狀流</a> －大型的類似冠狀結構日冕，具有長的尖峰，通常覆蓋著太陽黑子和活躍區域。冕流被認為是慢速<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%A2%A8" class="mw-redirect" title="太陽風">太陽風</a>的來源<sup id="cite_ref-14" class="reference"><a href="#cite_note-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading4"><h4 id="長絲腔"><span id=".E9.95.B7.E7.B5.B2.E8.85.94"></span>長絲腔</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=8" title="编辑章节：長絲腔"><span>编辑</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/File:Crackling_with_Solar_Flares.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Crackling_with_Solar_Flares.jpg/220px-Crackling_with_Solar_Flares.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Crackling_with_Solar_Flares.jpg/330px-Crackling_with_Solar_Flares.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c6/Crackling_with_Solar_Flares.jpg/440px-Crackling_with_Solar_Flares.jpg 2x" data-file-width="2048" data-file-height="2048" /></a><figcaption><a href="/wiki/%E5%A4%AA%E9%99%BD%E5%8B%95%E5%8A%9B%E5%AD%B8%E5%A4%A9%E6%96%87%E5%8F%B0" title="太陽動力學天文台">SDO</a>在2010年10月16日拍攝的圖像。在太陽的南半球可以看到一個很長的長絲腔。</figcaption></figure> <p><b>長絲腔</b>是在X射線中看起來很暗的區域，位於色球中觀察到的<a href="/wiki/H-%CE%B1" title="H-α">hα</a>長絲區域之上。是在1970年的兩次火箭飛行中首次觀察到的，這次的火箭飛行也觀測到了<i>冕洞</i><sup id="cite_ref-Giacconi_13-1" class="reference"><a href="#cite_note-Giacconi-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup>。 </p><p>長絲腔是由磁力懸浮在太陽表面上方較冷的氣體雲（電漿）。這些區域是強磁場區，因為沒有熱電漿，在圖像中看起來很暗。事實上，<span class="ilh-all" data-orig-title="磁壓" data-lang-code="en" data-lang-name="英语" data-foreign-title="Magnetic pressure"><span class="ilh-page"><a href="/w/index.php?title=%E7%A3%81%E5%A3%93&action=edit&redlink=1" class="new" title="磁壓（页面不存在）">磁壓</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Magnetic_pressure" class="extiw" title="en:Magnetic pressure"><span lang="en" dir="auto">Magnetic pressure</span></a></span>）</span></span>和電漿壓力的總和在太陽圈上的任何地方都必須是恆定的，有一個平衡的配置：在磁壓高的地方，電漿必須較冷或密度較低。電漿壓力可以透過理想氣體的<a href="/wiki/%E7%8A%B6%E6%80%81%E6%96%B9%E7%A8%8B" title="状态方程">狀態方程</a>計算<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle p=nK_{B}T}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>p</mi> <mo>=</mo> <mi>n</mi> <msub> <mi>K</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> <mi>T</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle p=nK_{B}T}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/d5ca46d8dd7a2d075b38e1d039c28459a0c56716" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; margin-left: -0.089ex; width:10.841ex; height:2.509ex;" alt="{\displaystyle p=nK_{B}T}"></span>，此處的<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle n}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>n</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle n}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/a601995d55609f2d9f5e233e36fbe9ea26011b3b" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.395ex; height:1.676ex;" alt="{\displaystyle n}"></span>是<a href="/wiki/%E7%B2%92%E5%AD%90%E6%95%B8" title="粒子數">粒子數</a>，, <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle K_{B}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>K</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle K_{B}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/041770ed83382d595875532cc29acd938c39a74b" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:3.453ex; height:2.509ex;" alt="{\displaystyle K_{B}}"></span>是<a href="/wiki/%E6%B3%A2%E8%8C%B2%E6%9B%BC%E5%B8%B8%E6%95%B8" title="波茲曼常數">波茲曼常數</a>，和<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle T}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>T</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle T}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/ec7200acd984a1d3a3d7dc455e262fbe54f7f6e0" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.636ex; height:2.176ex;" alt="{\displaystyle T}"></span>是電漿的溫度。從方程，當電漿溫度相對於周圍區域的溫度降低，或強磁場區清空時，電漿壓力會降低。同樣的物理效應使<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%BB%91%E5%AD%90" class="mw-redirect" title="太陽黑子">太陽黑子</a>在<a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球</a>中顯得黑暗。 </p> <div class="mw-heading mw-heading4"><h4 id="亮點"><span id=".E4.BA.AE.E9.BB.9E"></span>亮點</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=9" title="编辑章节：亮點"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p><b>亮點</b>是在太陽盤面上發現的小活躍區域。在1969年4月8日的一次火箭飛行中首次探測到X射限亮點<sup id="cite_ref-Giacconi_13-2" class="reference"><a href="#cite_note-Giacconi-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup>。 </p><p>亮點覆蓋在太陽表面的百分比隨<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽週期</a>的不同而變化，與磁場的小雙極區域有關。其平均溫度範圍從1.1x10<sup>6</sup> K至3.4x10<sup>6</sup> K，溫度的變化通常與X射線輻射的變化有關<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> <div class="mw-heading mw-heading3"><h3 id="冕洞"><span id=".E5.86.95.E6.B4.9E"></span>冕洞</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=10" title="编辑章节：冕洞"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a></div> <p><b><a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a></b>因為不會輻射出太多的X射線，在X射線中看起來是很暗的極地區域<sup id="cite_ref-16" class="reference"><a href="#cite_note-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup>。它們是太陽上的廣闊區域，那裡的磁場是向行星際空間開放的單極。高速<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%A2%A8" class="mw-redirect" title="太陽風">太陽風</a>主要來自這些區域。 </p><p>在冕洞的紫外線影像中，一些類似於拉長氣泡的小結構經常看起來像是懸浮在太陽風中。這些是冕<b>羽流</b>，更確切的說，它們是從太陽的南北兩極向外投射出來的細長絲帶<sup id="cite_ref-17" class="reference"><a href="#cite_note-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading3"><h3 id="寧靜太陽"><span id=".E5.AF.A7.E9.9D.9C.E5.A4.AA.E9.99.BD"></span>寧靜太陽</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=11" title="编辑章节：寧靜太陽"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>不屬於活躍區域和冕洞的太陽區域通常被認定是<b>寧靜太陽</b>。 </p><p>赤道區域自轉的比極區快，這種<a href="/wiki/%E8%BC%83%E5%B7%AE%E8%87%AA%E8%BD%89" class="mw-redirect" title="較差自轉">較差自轉</a>的結果是活躍區域總是成對的出現在與赤道平行的區帶中。它們在每個<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽週期</a>的極大期間擴展與增加，而在極小期時幾乎消失不見。因此，寧靜太陽總是與赤道區重合，其表面在太陽活動的極大期間也不太活躍。接近太陽週期（也稱為蝴蝶週期）的極小期時，寧靜太陽的範圍會擴展與增加，直到覆蓋整個太陽盤面，但是要排除半球上的那些亮點和有冕洞的極區。 </p> <div class="mw-heading mw-heading2"><h2 id="日冕的變異性"><span id=".E6.97.A5.E5.86.95.E7.9A.84.E8.AE.8A.E7.95.B0.E6.80.A7"></span>日冕的變異性</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=12" title="编辑章节：日冕的變異性"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>對日冕主要結構特徵的動態分析指出，日冕的特徵是多樣化的，在它們之間主要結構的演變也非常不同。研究日冕變化的複雜性很不容易，因為不同結構的演化時間就會有很大的差異：從秒到數個月都有。日冕事件發生區域的典型大小也有相同方式的變化，如下表所示。 </p> <table class="wikitable" title="可觀測到的日冕特徵的典型長度"> <tbody><tr> <th><b>日冕事件</b></th> <th><b>典型的時間尺度</b></th> <th><b>典型的長度尺度（Mm）</b> </th></tr> <tr> <td>活躍區<a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a></td> <td>10至10,000秒</td> <td>10–100 </td></tr> <tr> <td>X射線亮點</td> <td>數分鐘</td> <td>1–10 </td></tr> <tr> <td>大型結構中的瞬變</td> <td>從數分鐘至數小時</td> <td>〜100 </td></tr> <tr> <td>互連弧中的瞬變</td> <td>從數分鐘至數小時</td> <td>〜100 </td></tr> <tr> <td>寧靜太陽</td> <td>從數小時到數月</td> <td>100–1,000 </td></tr> <tr> <td><a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a></td> <td>數次自轉</td> <td>100–1,000 </td></tr></tbody></table> <div class="mw-heading mw-heading3"><h3 id="閃焰"><span id=".E9.96.83.E7.84.B0"></span>閃焰</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=13" title="编辑章节：閃焰"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg/220px-Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg" decoding="async" width="220" height="124" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg/330px-Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/e3/Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg/440px-Magnificent_CME_Erupts_on_the_Sun_-_August_31.jpg 2x" data-file-width="1920" data-file-height="1080" /></a><figcaption>一直在太陽外大氣層中盤旋的物質，日冕，在2012年美國東部時間下午4:36的爆發。</figcaption></figure> <p>閃焰發生在活躍地區，其特徵是來自日冕小地區發射的通量突然增加。它們是非常複雜的現象，在許多的波段中都可以觀察到；它們涉及太陽大氣的好幾個區域和許多物理效應：熱和非熱的，有時會有廣泛的磁重連和物質排出。 </p><p>閃焰是脈衝現象，平均的持續時間約為15分鐘，但能量最強的事件可以持續數小時。閃焰會產生快速的密度增加和高溫。 </p><p>白光閃焰很少發生和被觀測到：通常的情況下，閃焰只在極紫外線和X射線的波段被觀測到，是典型的色球和日冕發射。 </p><p>在日冕中，閃焰的型態是由紫外線、軟和硬X射線以及<a href="/wiki/H-%CE%B1" title="H-α">hα</a>波長的觀測來描述，並且非常複雜。但是，可以區分出兩種基本結構<sup id="cite_ref-18" class="reference"><a href="#cite_note-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup>： </p> <ul><li><b>緻密型閃焰</b>：當事件發生時，兩個拱弧之一會保持其形態。在沒有顯著結構變化的情況下，能觀察到排放的增加。發射能量的數量極約為10<sup>22</sup>至 10<sup>23</sup>焦耳。</li> <li><b>持續長時間閃焰</b>：與<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a>的爆發、白光和<i>雙帶閃焰</i>的瞬變有關<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>。在這種情況下，磁環會在事件其間更改其配置。這些閃焰發出的能量很高，可以達到10<sup>25</sup>焦耳。</li></ul> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Solar-filament.gif" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/b4/Solar-filament.gif/220px-Solar-filament.gif" decoding="async" width="220" height="157" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/b4/Solar-filament.gif/330px-Solar-filament.gif 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/b4/Solar-filament.gif/440px-Solar-filament.gif 2x" data-file-width="669" data-file-height="478" /></a><figcaption>在閃焰期間噴發的長絲。是<a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">TRACE</a>以EUV波長觀測到的。</figcaption></figure> <p>至於時間動力學，通常區分三個不同的階段，其持續時間是不可比較的。這些週期的持續時間取決於用於觀察事件的波長範圍： </p> <ul><li><b>初始脈衝階段</b>：其持續時間約為數分鐘，即使在微波、EUV波長、和硬X射線頻率中，也經常能觀測到強能量的發射。</li> <li><b>極大階段</b></li> <li><b>衰減階段</b>：可能會持續數小時。.</li></ul> <p>有時在閃焰發生之前也有一個階段可以被觀測到，通常稱為"預閃焰"階段。 </p> <div class="mw-heading mw-heading3"><h3 id="瞬變"><span id=".E7.9E.AC.E8.AE.8A"></span>瞬變</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=14" title="编辑章节：瞬變"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E6%97%A5%E5%86%95%E7%89%A9%E8%B3%AA%E6%8A%9B%E5%B0%84" class="mw-redirect" title="日冕物質抛射">日冕物質抛射</a></div> <p>伴隨著<a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a>或大型<a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a>，有時也會釋出<b>"日冕瞬變"</b>（也稱為<a href="/wiki/%E6%97%A5%E5%86%95%E7%89%A9%E8%B3%AA%E6%8B%8B%E5%B0%84" class="mw-redirect" title="日冕物質拋射">日冕物質拋射</a>）。這些是日冕物質的巨量回圈，以超過100萬公里的時速從太陽向外傳播，其所釋出的能量大約是閃焰或伴隨它們的日珥能量的10倍。一些更巨大的拋射可以每小時150萬公里的速度將數億噸的物質拋進太空。 </p> <div class="mw-heading mw-heading2"><h2 id="星冕"><span id=".E6.98.9F.E5.86.95"></span>星冕</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=15" title="编辑章节：星冕"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>星冕對在<a href="/wiki/%E8%B5%AB%E7%BE%85%E5%9C%96" title="赫羅圖">赫羅圖</a>低溫區部分的<a href="/wiki/%E6%81%86%E6%98%9F" class="mw-redirect" title="恆星">恆星</a>是無處不在的,可以用<a href="/wiki/X%E5%B0%84%E7%B7%9A%E6%9C%9B%E9%81%A0%E9%8F%A1" class="mw-redirect" title="X射線望遠鏡">X射線望遠鏡</a>檢測到這些星冕。有些星冕，特別是年輕的恆星，比太陽的明亮許多。例如，<a href="/wiki/%E8%AE%8A%E6%98%9F" title="變星">變星</a>中的<span class="ilh-all" data-orig-title="后髮座FK型變星" data-lang-code="en" data-lang-name="英语" data-foreign-title="Variable star"><span class="ilh-page"><a href="/w/index.php?title=%E5%90%8E%E9%AB%AE%E5%BA%A7FK%E5%9E%8B%E8%AE%8A%E6%98%9F&action=edit&redlink=1" class="new" title="后髮座FK型變星（页面不存在）">后髮座FK型變星</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Variable_star" class="extiw" title="en:Variable star"><span lang="en" dir="auto">Variable star</span></a></span>）</span></span>的原型，<a href="/wiki/%E5%90%8E%E9%AB%AE%E5%BA%A7FK" title="后髮座FK">后髮座FK</a>變星。這些是有異常高速自轉和極端活動跡象，光譜類型為G和K的巨星。它們的星冕X射線是最明亮的（<i>L</i><sub>x</sub> ≥ 10<sup>32</sup> 爾格·秒<sup>−1</sup>或10<sup>25</sup>瓦），並且是已知最熱的，主體溫度高達400萬K<sup id="cite_ref-Gudel_20-0" class="reference"><a href="#cite_note-Gudel-20"><span class="cite-bracket">[</span>20<span class="cite-bracket">]</span></a></sup>。 </p><p>朱塞佩·瓦伊亞納和他的小組與使用<a href="/wiki/%E7%88%B1%E5%9B%A0%E6%96%AF%E5%9D%A6%E5%8D%AB%E6%98%9F" title="爱因斯坦卫星">愛因斯坦天文台</a>進行的天文觀測計畫<sup id="cite_ref-Vaianaetal81_21-0" class="reference"><a href="#cite_note-Vaianaetal81-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup>顯示F、G、K、和M恆星都有色球，並且有和太陽很像的星冕。 </p><p>表面沒有對流層的<i>O-B恆星</i>，具有很強的X射線發射。然而，這些恆星沒有星冕，但因為快速移動的氣體團塊存在著熱不穩定性，在這樣的衝擊下導致恆星外層發射出X射線。另外，A型恆星也沒有對流層的，但是它們不會發射出紫外和X射線的波長。因此，他們既沒有色球，也沒有星冕。 </p> <div class="mw-heading mw-heading2"><h2 id="日冕的物理"><span id=".E6.97.A5.E5.86.95.E7.9A.84.E7.89.A9.E7.90.86"></span>日冕的物理</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=16" title="编辑章节：日冕的物理"><span>编辑</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/File:171879main_LimbFlareJan12_lg.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/d/da/171879main_LimbFlareJan12_lg.jpg/220px-171879main_LimbFlareJan12_lg.jpg" decoding="async" width="220" height="154" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/d/da/171879main_LimbFlareJan12_lg.jpg/330px-171879main_LimbFlareJan12_lg.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/d/da/171879main_LimbFlareJan12_lg.jpg/440px-171879main_LimbFlareJan12_lg.jpg 2x" data-file-width="1014" data-file-height="712" /></a><figcaption>這張圖片是<a href="/wiki/%E6%97%A5%E5%87%BA%E8%99%9F" class="mw-redirect" title="日出號">日出號</a>衛星在2007年1月12日拍攝的影像，揭露了日冕的絲狀性質。</figcaption></figure> <p>太陽大氣外部的物質大部分都是<a href="/wiki/%E9%9B%BB%E6%BC%BF" class="mw-redirect" title="電漿">電漿</a>的狀態，處於非常高的溫度（數百萬K的高溫）和非常低的密度（約10 <sup> 15 </sup>粒子/m<sup>3</sup>）。 </p><p>根據電漿的定義，它是一個準中性粒子集合表現出的一種集體行為。 </p><p>這種成分與太陽內部的組成相似，主要是氫，但電離程度遠遠高於光球中發現的。較重的金屬，如部分電離的鐵，且失去了大部分的電子。化學元素的電離狀態嚴格取決於溫度，並由最低層大氣中的<a href="/wiki/%E8%90%A8%E5%93%88%E7%94%B5%E7%A6%BB%E6%96%B9%E7%A8%8B" title="萨哈电离方程">薩哈方程</a>調節，但要由低光薄日冕中的碰撞來平衡。從歷史上看，由於存在高度電離狀態鐵原子發射的明線光譜，可以確定日冕電漿的高溫，而且日冕明顯的比內部的色球要熱得多。 </p><p>日冕的行為就像一種非常熱又非常輕的氣體：在活躍區域，日冕中的壓力通常只有.01到.06帕；而在地球上，大氣壓力通常是1,000百帕，大約比太陽表面高了約100萬倍。然而，它並不是氣體，而是以不同速度運動的自由帶電粒子（基本上是電子和質子）組成。假設它們具有相同的平均動能（依據<a href="/wiki/%E8%83%BD%E9%87%8F%E5%9D%87%E5%88%86%E5%AE%9A%E7%90%86" title="能量均分定理">能量均分定理</a>），電子的質量大約是質子的1,800分之一，因此它們獲得更高的速度，而金屬離子總是較慢。這一事實對輻射的過程（與光球輻射過程大不相同）或熱傳導都會產生相關的物理結果。此外，電荷的存在會導致電流和高磁場的產生。磁流體力學波（MHD波）也可以在電漿中傳播<sup id="cite_ref-Jeffrey_22-0" class="reference"><a href="#cite_note-Jeffrey-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup>，然而還不清楚它們適合在日冕中生成和傳輸。 </p> <div class="mw-heading mw-heading3"><h3 id="輻射"><span id=".E8.BC.BB.E5.B0.84"></span>輻射</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=17" title="编辑章节：輻射"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<span class="ilh-all" data-orig-title="Coronal radiative losses" data-lang-code="en" data-lang-name="英语" data-foreign-title="Coronal radiative losses"><span class="ilh-page"><a href="/w/index.php?title=Coronal_radiative_losses&action=edit&redlink=1" class="new" title="Coronal radiative losses（页面不存在）">Coronal radiative losses</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Coronal_radiative_losses" class="extiw" title="en:Coronal radiative losses"><span lang="en" dir="auto">Coronal radiative losses</span></a></span>）</span></span></div> <p>日冕的輻射主要是X射線，但只能在太空中觀測到。 </p><p>電漿對自身和下層的輻射是透明的，因此我們說它是"光學薄"的。事實上，氣體本身也非常稀薄，光子的平均自由路徑超越了包括日冕特徵的典型大小等一切的尺度。 </p><p>由於電漿粒子之間的兩兩互撞過程，發生輻射的地方不同，而與光子的交互作用則來自下層；這是非常罕見的。 </p><p>因為發射是源自電子和離子之間的碰撞，所以單位時間中在單位體積內因碰撞所釋放的能量與單位體積中粒子的平方數成正比，或者更確切的說，是與電子密度和質子密度的乘積成正比<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>。 </p> <div class="mw-heading mw-heading3"><h3 id="熱傳導"><span id=".E7.86.B1.E5.82.B3.E5.B0.8E"></span>熱傳導</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=18" title="编辑章节：熱傳導"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:STEREO-A_first_images.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c8/STEREO-A_first_images.jpg/220px-STEREO-A_first_images.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c8/STEREO-A_first_images.jpg/330px-STEREO-A_first_images.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c8/STEREO-A_first_images.jpg/440px-STEREO-A_first_images.jpg 2x" data-file-width="2700" data-file-height="2700" /></a><figcaption><a href="/wiki/%E6%97%A5%E5%9C%B0%E5%85%B3%E7%B3%BB%E5%A4%A9%E6%96%87%E5%8F%B0" title="日地关系天文台">STEREO</a>在2006年12月4日以及紫外線拍攝的馬賽克影像。這些假色影像顯示出不同溫度範圍的太陽大氣。從左上角順時針依序為：100萬°C（171 Å—藍色）、150萬度(195 Å—綠色）、60,000–80,000 °C（304 Å—紅色）、和250萬°C (286 Å—黃色)。.</figcaption></figure> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:STEREO-A_first_images_slow_anim.gif" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/STEREO-A_first_images_slow_anim.gif/220px-STEREO-A_first_images_slow_anim.gif" decoding="async" width="220" height="219" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/e3/STEREO-A_first_images_slow_anim.gif/330px-STEREO-A_first_images_slow_anim.gif 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/e3/STEREO-A_first_images_slow_anim.gif/440px-STEREO-A_first_images_slow_anim.gif 2x" data-file-width="1423" data-file-height="1418" /></a><figcaption><a href="/wiki/%E6%97%A5%E5%9C%B0%E5%85%B3%E7%B3%BB%E5%A4%A9%E6%96%87%E5%8F%B0" title="日地关系天文台">STEREO</a>– 第一張慢動作動畫。</figcaption></figure> <p>日冕的<a href="/wiki/%E7%86%B1%E5%82%B3%E5%B0%8E" class="mw-redirect" title="熱傳導">熱傳導</a>是外部較熱的大氣像內部冷卻層方向進行，負責熱傳導過程的是電子。如上所述，它們比離子輕得多，移動速度更快。 </p><p>當存在磁場時，電漿的<a href="/wiki/%E7%86%B1%E5%B0%8E%E7%8E%87" title="熱導率">熱導率</a>是在與場線平行的方向上，而不是在垂直方向上<sup id="cite_ref-Spitzer_24-0" class="reference"><a href="#cite_note-Spitzer-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup>。在垂直於磁場線方向上運動的帶電粒子受到<a href="/wiki/%E6%B4%9B%E4%BC%A6%E5%85%B9%E5%8A%9B" title="洛伦兹力">洛伦兹力</a>的影響，該粒子的運動平面與速度和磁場各自所在的平面是正交的。這個力彎曲了粒子的路徑。一般情況下，由於粒子沿磁場方向也有速度分量，<a href="/wiki/%E6%B4%9B%E4%BC%A6%E5%85%B9%E5%8A%9B" title="洛伦兹力">洛伦兹力</a>限制它們<a href="/wiki/%E5%9B%9E%E6%97%8B%E5%8A%A0%E9%80%9F%E5%99%A8" title="回旋加速器">迴旋加速器</a>的頻率下沿著磁場線彎曲和呈螺旋移動。 </p><p>如果粒子之間的碰撞非常頻繁，它們就會分散在各個方向。這種情況發生在光球中，電漿在其運動中攜帶著磁場。相對的，在日冕中的平均自由路徑大約為數公里甚至更長，因此每顆電子在被碰撞散射之前，能進行一段螺旋的運動。因此，沿著磁場線的熱傳導得到增強，而在垂直方向上受到抑制。 </p><p>在磁場的縱向方向上，日冕的<a href="/wiki/%E5%AF%BC%E7%83%AD%E7%B3%BB%E6%95%B0" class="mw-redirect" title="导热系数">導熱係數</a>是<sup id="cite_ref-Spitzer_24-1" class="reference"><a href="#cite_note-Spitzer-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup> </p><p><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle k=20\left({\frac {2}{\pi }}\right)^{3/2}{\frac {\left(k_{B}T\right)^{5/2}k_{B}}{m_{e}^{1/2}e^{4}\ln \Lambda }}\approx 1.8~10^{-10}~{\frac {T^{5/2}}{\ln \Lambda }}~Wm^{-1}K^{-1}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>k</mi> <mo>=</mo> <mn>20</mn> <msup> <mrow> <mo>(</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mn>2</mn> <mi>π</mi> </mfrac> </mrow> <mo>)</mo> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>3</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mn>2</mn> </mrow> </msup> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <msup> <mrow> <mo>(</mo> <mrow> <msub> <mi>k</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> <mi>T</mi> </mrow> <mo>)</mo> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>5</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mn>2</mn> </mrow> </msup> <msub> <mi>k</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> </mrow> <mrow> <msubsup> <mi>m</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>e</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>1</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mn>2</mn> </mrow> </msubsup> <msup> <mi>e</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>4</mn> </mrow> </msup> <mi>ln</mi> <mo>⁡</mo> <mi mathvariant="normal">Λ</mi> </mrow> </mfrac> </mrow> <mo>≈</mo> <mn>1.8</mn> <mtext> </mtext> <msup> <mn>10</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>10</mn> </mrow> </msup> <mtext> </mtext> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <msup> <mi>T</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>5</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mn>2</mn> </mrow> </msup> <mrow> <mi>ln</mi> <mo>⁡</mo> <mi mathvariant="normal">Λ</mi> </mrow> </mfrac> </mrow> <mtext> </mtext> <mi>W</mi> <msup> <mi>m</mi> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> <msup> <mi>K</mi> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle k=20\left({\frac {2}{\pi }}\right)^{3/2}{\frac {\left(k_{B}T\right)^{5/2}k_{B}}{m_{e}^{1/2}e^{4}\ln \Lambda }}\approx 1.8~10^{-10}~{\frac {T^{5/2}}{\ln \Lambda }}~Wm^{-1}K^{-1}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/6af9dfaf211e939f64dc7a79f80b4cf89d3a11de" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -3.171ex; width:57.065ex; height:7.509ex;" alt="{\displaystyle k=20\left({\frac {2}{\pi }}\right)^{3/2}{\frac {\left(k_{B}T\right)^{5/2}k_{B}}{m_{e}^{1/2}e^{4}\ln \Lambda }}\approx 1.8~10^{-10}~{\frac {T^{5/2}}{\ln \Lambda }}~Wm^{-1}K^{-1}}"></span> </p><p>此處的<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle k_{B}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>k</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle k_{B}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/70f38f7b73e53fd7b5d9ca64bec3a1438cc0eade" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:2.691ex; height:2.509ex;" alt="{\displaystyle k_{B}}"></span>是<a href="/wiki/%E6%B3%A2%E8%8C%B2%E6%9B%BC%E5%B8%B8%E6%95%B8" title="波茲曼常數">波茲曼常數</a>， <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle T}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>T</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle T}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/ec7200acd984a1d3a3d7dc455e262fbe54f7f6e0" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.636ex; height:2.176ex;" alt="{\displaystyle T}"></span>是絕對溫度， <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle m_{e}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>m</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>e</mi> </mrow> </msub> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle m_{e}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/8303b668e94e02d8f3db8c5b3ebd069ca5da9ba5" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:3.039ex; height:2.009ex;" alt="{\displaystyle m_{e}}"></span>是電子質量， <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle e}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>e</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle e}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/cd253103f0876afc68ebead27a5aa9867d927467" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.083ex; height:1.676ex;" alt="{\displaystyle e}"></span>電子的電量， </p><p><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle \ln \Lambda =\ln \left(12\pi n\lambda _{D}^{3}\right)}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>ln</mi> <mo>⁡</mo> <mi mathvariant="normal">Λ</mi> <mo>=</mo> <mi>ln</mi> <mo>⁡</mo> <mrow> <mo>(</mo> <mrow> <mn>12</mn> <mi>π</mi> <mi>n</mi> <msubsup> <mi>λ</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>D</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>3</mn> </mrow> </msubsup> </mrow> <mo>)</mo> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \ln \Lambda =\ln \left(12\pi n\lambda _{D}^{3}\right)}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/5383af7812f34dd14c8c1c739729fbbd81092b00" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -1.005ex; width:19.107ex; height:3.176ex;" alt="{\displaystyle \ln \Lambda =\ln \left(12\pi n\lambda _{D}^{3}\right)}"></span> </p><p>庫倫對數，和 </p><p><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle \lambda _{D}={\sqrt {\frac {k_{B}T}{4\pi ne^{2}}}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>λ</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>D</mi> </mrow> </msub> <mo>=</mo> <mrow class="MJX-TeXAtom-ORD"> <msqrt> <mfrac> <mrow> <msub> <mi>k</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>B</mi> </mrow> </msub> <mi>T</mi> </mrow> <mrow> <mn>4</mn> <mi>π</mi> <mi>n</mi> <msup> <mi>e</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mrow> </mfrac> </msqrt> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \lambda _{D}={\sqrt {\frac {k_{B}T}{4\pi ne^{2}}}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/3053dea2c53672bac0210c27b644659e7eacf2f5" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -2.505ex; width:15.233ex; height:6.343ex;" alt="{\displaystyle \lambda _{D}={\sqrt {\frac {k_{B}T}{4\pi ne^{2}}}}}"></span> </p><p>與電漿粒子密度相關的<a href="/w/index.php?title=%E5%BE%97%E6%8B%9C%E5%B8%B8%E6%95%B8&action=edit&redlink=1" class="new" title="得拜常數（页面不存在）">得拜常數</a><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle n}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>n</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle n}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/a601995d55609f2d9f5e233e36fbe9ea26011b3b" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.395ex; height:1.676ex;" alt="{\displaystyle n}"></span>。 </p><p>在平均溫度100萬K，密度為10<sup>15</sup>粒子/m<sup>3</sup>的日冕，庫倫對數<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle \ln \Lambda }"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>ln</mi> <mo>⁡</mo> <mi mathvariant="normal">Λ</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \ln \Lambda }</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/28b8691dd99b06547958f2cf02eed02fdb8744e0" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:3.939ex; height:2.176ex;" alt="{\displaystyle \ln \Lambda }"></span>大約是20；溫度約為10萬K，粒子密度為10<sup>18</sup>粒子/m<sup>3</sup>的色球，庫倫對數大約是10，。在實務中可以假定它是常數。 </p><p>如果我們用<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle q}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>q</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle q}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/06809d64fa7c817ffc7e323f85997f783dbdf71d" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:1.07ex; height:2.009ex;" alt="{\displaystyle q}"></span>取代J m<sup>−3</sup>表示單位體積的熱量，那麼導熱的傅立葉方程就只能沿著場線的方向<span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle x}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>x</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle x}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/87f9e315fd7e2ba406057a97300593c4802b53e4" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.33ex; height:1.676ex;" alt="{\displaystyle x}"></span>計算，變成 </p><p><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle {\frac {\partial q}{\partial t}}=0.9~10^{-11}~{\frac {\partial ^{2}T^{7/2}}{\partial x^{2}}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mi mathvariant="normal">∂</mi> <mi>q</mi> </mrow> <mrow> <mi mathvariant="normal">∂</mi> <mi>t</mi> </mrow> </mfrac> </mrow> <mo>=</mo> <mn>0.9</mn> <mtext> </mtext> <msup> <mn>10</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>11</mn> </mrow> </msup> <mtext> </mtext> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <msup> <mi mathvariant="normal">∂</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> <msup> <mi>T</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>7</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mn>2</mn> </mrow> </msup> </mrow> <mrow> <mi mathvariant="normal">∂</mi> <msup> <mi>x</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mrow> </mfrac> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle {\frac {\partial q}{\partial t}}=0.9~10^{-11}~{\frac {\partial ^{2}T^{7/2}}{\partial x^{2}}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/fe8073f9da413b7ee59f46082fed0fa24ed06455" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -2.171ex; width:23.587ex; height:6.009ex;" alt="{\displaystyle {\frac {\partial q}{\partial t}}=0.9~10^{-11}~{\frac {\partial ^{2}T^{7/2}}{\partial x^{2}}}}"></span>. </p><p>數值計算表明，日冕的導熱係數與銅相當。 </p> <div class="mw-heading mw-heading3"><h3 id="日冕地震學"><span id=".E6.97.A5.E5.86.95.E5.9C.B0.E9.9C.87.E5.AD.B8"></span>日冕地震學</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=19" title="编辑章节：日冕地震學"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<span class="ilh-all" data-orig-title="日冕地震學" data-lang-code="en" data-lang-name="英语" data-foreign-title="Coronal seismology"><span class="ilh-page"><a href="/w/index.php?title=%E6%97%A5%E5%86%95%E5%9C%B0%E9%9C%87%E5%AD%B8&action=edit&redlink=1" class="new" title="日冕地震學（页面不存在）">日冕地震學</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Coronal_seismology" class="extiw" title="en:Coronal seismology"><span lang="en" dir="auto">Coronal seismology</span></a></span>）</span></span></div> <p><b>日冕地震學</b>是使用<a href="/wiki/%E7%A3%81%E6%B5%81%E9%AB%94%E5%8A%9B%E5%AD%B8" class="mw-redirect" title="磁流體力學">磁流體動力學</a>波研究日冕<a href="/wiki/%E9%9B%BB%E6%BC%BF" class="mw-redirect" title="電漿">電漿</a>的新方法。磁流體力學研究的是<a href="/wiki/%E9%9B%BB%E5%B0%8E%E7%8E%87" title="電導率">導電</a><a href="/wiki/%E6%B5%81%E9%AB%94" class="mw-redirect" title="流體">流體</a>的<a href="/wiki/%E5%8B%95%E5%8A%9B%E5%AD%B8" title="動力學">動力學</a> －在這種情況下，流體是日冕電漿。就哲學而言，日冕地震學類似於地球的<a href="/wiki/%E5%9C%B0%E9%9C%87%E5%AD%B8" class="mw-redirect" title="地震學">地震學</a>、太陽的<a href="/wiki/%E6%97%A5%E9%9C%87%E5%AD%B8" title="日震學">日震學</a>、和實驗室電漿體的MHD光譜。在所有的這些方法中，用各種的波來探測介質。日冕地震學在估計日冕磁場、密度、<a href="/wiki/%E5%A4%A7%E6%B0%A3%E6%A8%99%E9%AB%98" title="大氣標高">大氣標高</a>、<a href="/wiki/%E7%B2%BE%E7%B4%B0%E7%B5%90%E6%A7%8B" title="精細結構">精細結構</a>和加熱等方面的潛力，已被不同的研究小組證實。 </p> <div class="mw-heading mw-heading2"><h2 id="日冕加熱問題"><span id=".E6.97.A5.E5.86.95.E5.8A.A0.E7.86.B1.E5.95.8F.E9.A1.8C"></span>日冕加熱問題</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=20" title="编辑章节：日冕加熱問題"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r82655521">.mw-parser-output .side-box{margin:4px 0;box-sizing:border-box;border:1px solid #aaa;font-size:88%;line-height:1.25em;background-color:#f9f9f9;display:flow-root}.mw-parser-output .side-box-abovebelow,.mw-parser-output .side-box-text{padding:0.25em 0.9em}.mw-parser-output .side-box-image{padding:2px 0 2px 0.9em;text-align:center}.mw-parser-output .side-box-imageright{padding:2px 0.9em 2px 0;text-align:center}@media(min-width:500px){.mw-parser-output .side-box-flex{display:flex;align-items:center}.mw-parser-output .side-box-text{flex:1}}@media(min-width:720px){.mw-parser-output .side-box{width:238px}.mw-parser-output .side-box-right{clear:right;float:right;margin-left:1em}.mw-parser-output .side-box-left{margin-right:1em}}</style><div class="side-box side-box-right" style="width: 250px;"><style data-mw-deduplicate="TemplateStyles:r82655520">.mw-parser-output .plainlist ol,.mw-parser-output .plainlist ul{line-height:inherit;list-style:none;margin:0;padding:0}.mw-parser-output .plainlist ol li,.mw-parser-output .plainlist ul li{margin-bottom:0}</style> <div class="side-box-flex"> <div class="side-box-text plainlist"><b><a href="/wiki/%E6%9C%AA%E8%A7%A3%E6%B1%BA%E7%9A%84%E7%89%A9%E7%90%86%E5%AD%B8%E5%95%8F%E9%A1%8C" title="未解決的物理學問題">未解決的物理學問題</a>：</b>太陽的日冕為何會比表面熱那麼多？</div> <div class="side-box-imageright"><span typeof="mw:File"><a href="/wiki/File:Question_mark2.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/b0/Question_mark2.svg/40px-Question_mark2.svg.png" decoding="async" width="40" height="52" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/b0/Question_mark2.svg/60px-Question_mark2.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/b0/Question_mark2.svg/80px-Question_mark2.svg.png 2x" data-file-width="71" data-file-height="92" /></a></span></div></div> </div> <figure class="mw-default-size" typeof="mw:File/Thumb"><span><video id="mwe_player_0" poster="//upload.wikimedia.org/wikipedia/commons/thumb/b/b6/Van_Gogh_Sun.ogv/220px--Van_Gogh_Sun.ogv.jpg" controls="" preload="none" data-mw-tmh="" class="mw-file-element" width="220" height="124" data-durationhint="127" data-mwtitle="Van_Gogh_Sun.ogv" data-mwprovider="wikimediacommons" resource="/wiki/File:Van_Gogh_Sun.ogv"><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b6/Van_Gogh_Sun.ogv/Van_Gogh_Sun.ogv.480p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="480p.vp9.webm" data-width="854" data-height="480" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b6/Van_Gogh_Sun.ogv/Van_Gogh_Sun.ogv.720p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="720p.vp9.webm" data-width="1280" data-height="720" /><source src="//upload.wikimedia.org/wikipedia/commons/b/b6/Van_Gogh_Sun.ogv" type="video/ogg; codecs="theora, vorbis"" data-width="1280" data-height="720" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b6/Van_Gogh_Sun.ogv/Van_Gogh_Sun.ogv.240p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="240p.vp9.webm" data-width="426" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b6/Van_Gogh_Sun.ogv/Van_Gogh_Sun.ogv.360p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="360p.vp9.webm" data-width="640" data-height="360" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b6/Van_Gogh_Sun.ogv/Van_Gogh_Sun.ogv.360p.webm" type="video/webm; codecs="vp8, vorbis"" data-transcodekey="360p.webm" data-width="640" data-height="360" /></video></span><figcaption>一種新的視覺化技術可以為日冕加熱問題提供線索。</figcaption></figure> <p><a href="/wiki/%E5%A4%AA%E9%99%BD%E7%89%A9%E7%90%86%E5%AD%B8" class="mw-redirect" title="太陽物理學">太陽物理學</a>的日冕加熱問題與為什麼日冕的溫度比表面高數百萬K有關。因為<a href="/wiki/%E7%86%B1%E5%8A%9B%E5%AD%B8%E7%AC%AC%E4%BA%8C%E5%AE%9A%E5%BE%8B" class="mw-redirect" title="熱力學第二定律">熱力學第二定律</a>阻止熱量直接從只有5,800K太陽光球（表面）流向溫度高達100萬K〜300萬K的日冕（部分可達1,000萬K），因此日冕的高溫需要能量通過非熱過程從太陽的內部輸送。 </p><p>在光球和日冕之間，有一個稱為<a href="/wiki/%E9%81%8E%E6%B8%A1%E5%8D%80" title="過渡區">過渡區</a>的薄層，是溫度升高的區域。它的厚度只有數十至數百公里不等。因為不能違反<a href="/wiki/%E7%86%B1%E5%8A%9B%E5%AD%B8%E7%AC%AC%E4%BA%8C%E5%AE%9A%E5%BE%8B" class="mw-redirect" title="熱力學第二定律">熱力學第二定律</a>，能量不能通過常規從較冷的光球轉移到日冕傳送。一個類比的例子是燈泡，會把周圍的溫度提升到比玻璃表面還要高的溫度。因此，在日冕的加熱過程中，還必須考慮到其它的能量傳遞方式。 </p><p>加熱太陽日冕所需要的功率可以很容易地計算為<span class="ilh-all" data-orig-title="日冕輻射損耗" data-lang-code="en" data-lang-name="英语" data-foreign-title="Coronal radiative losses"><span class="ilh-page"><a href="/w/index.php?title=%E6%97%A5%E5%86%95%E8%BC%BB%E5%B0%84%E6%90%8D%E8%80%97&action=edit&redlink=1" class="new" title="日冕輻射損耗（页面不存在）">日冕輻射損耗</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Coronal_radiative_losses" class="extiw" title="en:Coronal radiative losses"><span lang="en" dir="auto">Coronal radiative losses</span></a></span>）</span></span>與以熱傳導從<a href="/wiki/%E8%89%B2%E7%90%83" title="色球">色球</a>通過過渡區之間的差。這大約是在色球上每米平方1千瓦，或是從太陽表面逃逸光能量的1/40,000。 </p><p>許多日冕加熱的理論曾經被提出來<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>，但是只有兩種理論是最有可能的候選者：波加熱和<a href="/wiki/%E7%A3%81%E9%87%8D%E8%81%94" title="磁重联">磁重聯</a>（或<a href="/wiki/%E6%AF%AB%E5%BE%AE%E9%96%83%E7%84%B0" title="毫微閃焰">毫微閃焰</a>）<sup id="cite_ref-26" class="reference"><a href="#cite_note-26"><span class="cite-bracket">[</span>26<span class="cite-bracket">]</span></a></sup>。然而，在過去50年的大部分時間裡，這兩種理論都未能解釋極端的日冕溫度。 </p><p>在2012年，高解析（<0.2”）的<a href="/wiki/%E8%BD%AFX%E5%B0%84%E7%BA%BF" class="mw-redirect" title="软X射线">軟X射線</a>影像與<a href="/wiki/%E6%8E%A2%E7%A9%BA%E7%81%AB%E7%AE%AD" title="探空火箭">探空火箭</a>的<span class="ilh-all" data-orig-title="高解析度日冕成像儀" data-lang-code="en" data-lang-name="英语" data-foreign-title="High Resolution Coronal Imager"><span class="ilh-page"><a href="/w/index.php?title=%E9%AB%98%E8%A7%A3%E6%9E%90%E5%BA%A6%E6%97%A5%E5%86%95%E6%88%90%E5%83%8F%E5%84%80&action=edit&redlink=1" class="new" title="高解析度日冕成像儀（页面不存在）">高解析度日冕成像儀</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/High_Resolution_Coronal_Imager" class="extiw" title="en:High Resolution Coronal Imager"><span lang="en" dir="auto">High Resolution Coronal Imager</span></a></span>）</span></span>揭示了日冕中有緊密纏繞的辮子。這被推測認為辮子的解開和重新連結可以做為活躍太陽日冕加熱至高達400萬K的主要能量來源。在寧靜日冕（150萬K）的主要熱源被認為來自<a href="/wiki/%E7%A3%81%E6%B5%81%E9%AB%94%E5%8A%9B%E5%AD%B8" class="mw-redirect" title="磁流體力學">MHD波</a> <sup id="cite_ref-Cirtain2013_27-0" class="reference"><a href="#cite_note-Cirtain2013-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup>。 </p><p><a href="/wiki/%E7%BE%8E%E5%9B%BD%E5%9B%BD%E5%AE%B6%E8%88%AA%E7%A9%BA%E8%88%AA%E5%A4%A9%E5%B1%80" title="美国国家航空航天局">NASA</a>的<a href="/wiki/%E6%B4%BE%E5%85%8B%E5%A4%AA%E9%99%BD%E6%8E%A2%E6%B8%AC%E5%99%A8" title="派克太陽探測器">派克太陽探測器</a>任務打算接近太陽制約9.5太陽半徑的距離，以研究日冕加熱和太陽風的起源。它已於2018年8月12日成功發射，目前已經離開地球並飛掠過金星，進入第一階段的軌道<sup id="cite_ref-28" class="reference"><a href="#cite_note-28"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup>。 </p> <table class="wikitable" style="margin: 1em auto 1em auto"> <caption><b>相互競爭的加熱機制</b> </caption> <tbody><tr> <th colspan="3">加熱模式 </th></tr> <tr> <th>流體力學 </th> <th colspan="2">磁 </th></tr> <tr> <td rowspan="2"> <ul><li>無磁場</li> <li>緩慢旋轉的恆星</li></ul> </td> <th><a href="/wiki/%E7%9B%B4%E6%B5%81%E9%9B%BB" title="直流電">DC</a> (<i>重連結</i>) </th> <th><a href="/wiki/%E4%BA%A4%E6%B5%81%E9%9B%BB" title="交流電">AC</a> (<i>波</i>) </th></tr> <tr> <td> <ul><li>磁場應力</li> <li>重連結事件</li> <li><a href="/wiki/%E9%96%83%E7%84%B0" class="mw-redirect" title="閃焰">閃焰</a>-<a href="/wiki/%E6%AF%AB%E5%BE%AE%E9%96%83%E7%84%B0" title="毫微閃焰">毫微閃焰</a></li> <li><i>均勻的加熱率</i></li></ul> </td> <td> <ul><li>光球足點<i>滑移</i></li> <li>MHD波傳播</li> <li>高阿爾文波流</li> <li><i>不均勻的加熱率</i></li></ul> </td></tr> <tr> <th> </th> <th colspan="2">競爭的理論 </th></tr></tbody></table> <div class="mw-heading mw-heading3"><h3 id="波加熱理論"><span id=".E6.B3.A2.E5.8A.A0.E7.86.B1.E7.90.86.E8.AB.96"></span>波加熱理論</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=21" title="编辑章节：波加熱理論"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>波加熱理論是<span class="ilh-all" data-orig-title="葉夫裡·沙茨曼" data-lang-code="en" data-lang-name="英语" data-foreign-title="Evry Schatzman"><span class="ilh-page"><a href="/w/index.php?title=%E8%91%89%E5%A4%AB%E8%A3%A1%C2%B7%E6%B2%99%E8%8C%A8%E6%9B%BC&action=edit&redlink=1" class="new" title="葉夫裡·沙茨曼（页面不存在）">葉夫裡·沙茨曼</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Evry_Schatzman" class="extiw" title="en:Evry Schatzman"><span lang="en" dir="auto">Evry Schatzman</span></a></span>）</span></span>在1949年提出的，他認為波攜帶能量從太陽內部傳遞至色球和日冕。太陽是由<a href="/wiki/%E9%9B%BB%E6%BC%BF" class="mw-redirect" title="電漿">電漿</a>，而不是普通的物質組成的，因此他支援幾種類似於空氣中<a href="/wiki/%E8%81%B2%E6%B3%A2" class="mw-redirect" title="聲波">聲波</a>的波。最重要的波是<a href="/wiki/%E7%A3%81%E8%81%B2%E6%B3%A2" class="mw-redirect" title="磁聲波">磁聲波</a>和<a href="/wiki/%E9%98%BF%E7%88%BE%E6%96%87%E6%B3%A2" class="mw-redirect" title="阿爾文波">阿爾文波</a>這兩種類型<sup id="cite_ref-29" class="reference"><a href="#cite_note-29"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup>。磁聲波是因應磁場的存在而修改的聲波，阿爾文波類似於<a href="/wiki/%E8%B6%85%E4%BD%8E%E9%A0%BB" title="超低頻">超低頻</a><a href="/wiki/%E7%84%A1%E7%B7%9A%E9%9B%BB%E6%B3%A2" class="mw-redirect" title="無線電波">無線電波</a>，這是經過修改的聲波，能通過與電漿中<a href="/wiki/%E7%89%A9%E8%B3%AA" class="mw-redirect" title="物質">物質</a>的交互作用而傳播。這兩種類型的波都可以通過光球層的<a href="/wiki/%E7%B1%B3%E7%B2%92%E7%B5%84%E7%B9%94" class="mw-redirect" title="米粒組織">米粒組織</a>和<a href="/wiki/%E8%B6%85%E7%B1%B3%E7%B2%92%E7%B5%84%E7%B9%94" title="超米粒組織">超米粒組織</a>的湍流來發射，並且在在成為<a href="/wiki/%E6%BF%80%E6%B3%A2" title="激波">激波</a>將能量以熱的形式釋放之前，通過太陽大氣層的一段距離。 </p><p>波加熱的一個問題是如何將熱量傳遞到適當的地方。因為色球中存在的低壓，磁聲波不能攜帶足夠的能量到日冕，以及它們往往會被<a href="/wiki/%E5%8F%8D%E5%B0%84" class="mw-disambig" title="反射">反射</a>回光球。阿爾文波可以攜帶足夠的能量，但一旦進入日冕，就不能足夠迅速地耗散能量。眾所周知，在電漿中的波很難理解、描述和分析，但由湯瑪斯·柏格丹和他的同事們在2003年進行的電腦模擬，似乎表明阿爾文波可以轉化為日冕底部其他模式的波。這提供了一個通道，可以通過色球和過渡區從光球攜帶大量能量進入日冕，最後在日冕以熱的形式耗散能量。 </p><p>波加熱的另一個問題是，直到20世紀90年代的末期，還沒有任何直接的證據顯示波可以在日冕中傳播。第一個直接觀測到波在日冕中傳播的是<a href="/wiki/%E5%A4%AA%E9%99%BD%E5%92%8C%E5%A4%AA%E9%99%BD%E5%9C%88%E6%8E%A2%E6%B8%AC%E5%99%A8" title="太陽和太陽圈探測器">太陽和太陽圈探測器</a>，在1997年使用<a href="/wiki/%E7%B4%AB%E5%A4%96%E7%B7%9A" class="mw-redirect" title="紫外線">及紫外線</a>完成的。<a href="/wiki/%E5%A4%AA%E9%99%BD%E5%92%8C%E5%A4%AA%E9%99%BD%E5%9C%88%E6%8E%A2%E6%B8%AC%E5%99%A8" title="太陽和太陽圈探測器">太陽和太陽圈探測器</a>是能在太空中承擔長時間穩定[[光度測定 (天文學)]測光]]的平台。這個波是頻率約為1<a href="/wiki/%E8%B5%AB%E8%8C%B2" class="mw-redirect" title="赫茲">毫赫茲</a>（MHz相當週期1,000秒），但只攜帶日冕所需能量的10%左右。現在已經觀測到存在許多局部的波，例如閃焰發射的阿爾文波。但這些現象都是瞬態的，不能解釋均勻的日冕高熱。 </p><p>目前還不清楚需要多少的波才能加熱日冕。使用<a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">太陽過渡區與日冕探測器</a>（TRACE）在2004年公布的結果，似乎顯示太陽大氣中存在頻率高達100mHz（週期10秒）的波。使用<a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">太陽過渡區與日冕探測器</a>的超紫外線日冕儀（UVCS，UltraViolet Coronagraph SpectrometerMeasurements）測量<a href="/wiki/%E5%A4%AA%E9%99%BD%E9%A2%A8" class="mw-redirect" title="太陽風">太陽風</a>中不同<a href="/wiki/%E9%9B%A2%E5%AD%90" class="mw-redirect" title="離子">離子</a>的溫度，提供了有力的間接證據，證明有200Hz到人耳聽力範圍頻率的波存在。這些波在正常情況下很難被探測到，但來自<a href="/wiki/%E5%A8%81%E5%BB%89%E5%A3%AB%E5%AD%B8%E9%99%A2" class="mw-redirect" title="威廉士學院">威廉士學院</a>的研究小組在日食期間收集的證據表明，存在1-10Hz範圍的這種波。 </p><p>最近，在較低的太陽大氣中發現了阿爾文波的運動<sup id="cite_ref-30" class="reference"><a href="#cite_note-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-31" class="reference"><a href="#cite_note-31"><span class="cite-bracket">[</span>31<span class="cite-bracket">]</span></a></sup>，並且使用<a href="/wiki/%E5%A4%AA%E9%99%BD%E5%8B%95%E5%8A%9B%E5%AD%B8%E5%A4%A9%E6%96%87%E5%8F%B0" title="太陽動力學天文台">太陽動力學天文台</a>的大氣成像組件（Atmospheric Imaging Assembly，AIA）在寧靜太陽、冕動和活躍區都觀測到<sup id="cite_ref-32" class="reference"><a href="#cite_note-32"><span class="cite-bracket">[</span>32<span class="cite-bracket">]</span></a></sup>。這些阿爾文振盪有很大的力量，似乎與早先<a href="/wiki/%E6%97%A5%E5%87%BA%E8%99%9F" class="mw-redirect" title="日出號">日出號</a>報告的色球阿爾文振盪有所關聯<sup id="cite_ref-33" class="reference"><a href="#cite_note-33"><span class="cite-bracket">[</span>33<span class="cite-bracket">]</span></a></sup>。 </p><p><span class="ilh-all" data-orig-title="風 (太空船)" data-lang-code="en" data-lang-name="英语" data-foreign-title="WIND (spacecraft)"><span class="ilh-page"><a href="/w/index.php?title=%E9%A2%A8_(%E5%A4%AA%E7%A9%BA%E8%88%B9)&action=edit&redlink=1" class="new" title="風 (太空船)（页面不存在）">風 (太空船)</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/WIND_(spacecraft)" class="extiw" title="en:WIND (spacecraft)"><span lang="en" dir="auto">WIND (spacecraft)</span></a></span>）</span></span>最近的太陽風觀測證據，也支持阿爾文循環耗散理論導致局部離子加熱<sup id="cite_ref-34" class="reference"><a href="#cite_note-34"><span class="cite-bracket">[</span>34<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading3"><h3 id="磁重聯理論"><span id=".E7.A3.81.E9.87.8D.E8.81.AF.E7.90.86.E8.AB.96"></span>磁重聯理論</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=22" title="编辑章节：磁重聯理論"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84833064"><div role="note" class="hatnote navigation-not-searchable">主条目：<a href="/wiki/%E7%A3%81%E9%87%8D%E8%81%94" title="磁重联">磁重联</a></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Arcing_Active_Region.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Arcing_Active_Region.jpg/220px-Arcing_Active_Region.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Arcing_Active_Region.jpg/330px-Arcing_Active_Region.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/9c/Arcing_Active_Region.jpg/440px-Arcing_Active_Region.jpg 2x" data-file-width="800" data-file-height="800" /></a><figcaption><a href="/wiki/%E5%A4%AA%E9%99%BD%E5%8B%95%E5%8A%9B%E5%AD%B8%E5%A4%A9%E6%96%87%E5%8F%B0" title="太陽動力學天文台">太陽動力學天文台</a>拍攝的活躍區弧。</figcaption></figure> <p><a href="/wiki/%E7%A3%81%E9%87%8D%E8%81%94" title="磁重联">磁重聯</a>理論依賴太陽磁場在日冕中產生電流<sup id="cite_ref-35" class="reference"><a href="#cite_note-35"><span class="cite-bracket">[</span>35<span class="cite-bracket">]</span></a></sup>。隨後，電流突然崩潰，釋放出能量成為日冕中的熱量和波能量。因為磁場在電漿（或任何導電流體，如<a href="/wiki/%E6%B1%9E" title="汞">汞</a>或<a href="/wiki/%E6%B5%B7%E6%B0%B4" title="海水">海水</a>）的特殊行為，此一過程稱為"重聯"。在電漿中，<a href="/wiki/%E7%A3%81%E5%A0%B4%E7%B7%9A" class="mw-redirect" title="磁場線">磁場線</a>通常與單個物質塊相連，因此磁場的<a href="/wiki/%E6%8B%93%E6%A8%B8" class="mw-redirect" title="拓樸">拓樸</a>保持不變：如果一個特定的南北<a href="/w/index.php?title=%E5%A4%A9%E9%AB%94%E6%A5%B5&action=edit&redlink=1" class="new" title="天體極（页面不存在）">磁極</a>由一條單線連結，那麼即使電漿被攪動或著磁體被移動，該場線將繼續連接這些特定的極點。聯結由電漿中產生的電流維持。在一定的條件下，電流會崩潰，讓磁場"重聯"到其它的磁極，並載此過程中釋放熱量和波能量。 </p><p><a href="/wiki/%E7%A3%81%E9%87%8D%E8%81%94" title="磁重联">磁重聯</a>被假設為太陽系中最大的爆炸，太陽閃焰背後的機制。此外，太陽表面覆蓋著數以百萬計，尺度在50-1,000公里的小磁化區域。這些小磁極是不斷攪動和衝撞的米粒組織。太陽日冕中的磁場必須經過幾乎恆定的重聯，以匹配這些"磁性地毯"的運動，因此重聯釋放的能量是四免加熱最自然的候選物質，也許是一系列的"微閃焰"，各自提供很少的能量，但整體累積得到所需的能量。 </p><p><a href="/wiki/%E5%B0%A4%E9%87%91%C2%B7%E6%B4%BE%E5%85%8B" title="尤金·派克">尤金·派克</a>在20世紀的80年代提出<a href="/wiki/%E6%AF%AB%E5%BE%AE%E9%96%83%E7%84%B0" title="毫微閃焰">奈米閃焰</a>可能會加熱日冕，但仍有爭議。特別是，<a href="/wiki/%E7%B4%AB%E5%A4%96%E7%B7%9A" class="mw-redirect" title="紫外線">紫外線</a>望遠鏡，如<a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">太陽過渡區與日冕探測器</a>和<a href="/w/index.php?title=%E5%A4%AA%E9%99%BD%E5%92%8C%E6%97%A5%E5%85%89%E5%B1%A4%E5%A4%A9%E6%96%87%E5%8F%B0&action=edit&redlink=1" class="new" title="太陽和日光層天文台（页面不存在）">太陽和日光層天文台</a>/EIT可以在級紫外線下觀察到單個微閃焰的亮光但這些事件似乎太少<sup id="cite_ref-36" class="reference"><a href="#cite_note-36"><span class="cite-bracket">[</span>36<span class="cite-bracket">]</span></a></sup>，但這些事件似乎太少，無法解釋釋放至日冕中的能量。這沒有考慮到可以由波能量來彌補額外的能量，也可以由比微閃焰更平穩釋放能量的磁重聯來彌補，因此在<a href="/wiki/%E5%A4%AA%E9%98%B3%E8%BF%87%E6%B8%A1%E5%8C%BA%E4%B8%8E%E6%97%A5%E5%86%95%E6%8E%A2%E6%B5%8B%E5%99%A8" title="太阳过渡区与日冕探测器">太陽過渡區與日冕探測器</a>的資料中不會好好地呈現出來。用其它機制來改變微閃焰磁場或釋放能量，是2005年積極研究的課題。 </p> <div class="mw-heading mw-heading3"><h3 id="針狀體（第二型）"><span id=".E9.87.9D.E7.8B.80.E9.AB.94.EF.BC.88.E7.AC.AC.E4.BA.8C.E5.9E.8B.EF.BC.89"></span>針狀體（第二型）</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=23" title="编辑章节：針狀體（第二型）"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>幾十年來，研究人員認為<a href="/wiki/%E9%87%9D%E7%8B%80%E9%AB%94" title="針狀體">針狀體</a>可以將熱量送入日冕。然而，經過20世紀80年代的觀測，發現針狀體電漿沒有達到日冕的溫度，因此這個理論不受重視。 </p><p>靠著在<a href="/wiki/%E7%A7%91%E7%BE%85%E6%8B%89%E5%A4%9A%E5%B7%9E" title="科羅拉多州">科羅拉多州</a>的"國家大氣研究中心"與"洛克希德·馬丁的太陽和天體物理實驗室"（LMSAL）和<a href="/wiki/%E5%A5%A5%E6%96%AF%E9%99%86%E5%A4%A7%E5%AD%A6" title="奥斯陆大学">奧斯陸大學</a>的"理論天體物理學院"在2007年發現一種新型的針狀體（第二型）。它的速度更快（100Km/s），壽命更短，在2010年的研究可以解釋這個問題<sup id="cite_ref-37" class="reference"><a href="#cite_note-37"><span class="cite-bracket">[</span>37<span class="cite-bracket">]</span></a></sup>。這些噴射將炙熱的電漿插入太陽外部的大氣中。 </p><p>因此，從今以後可以預期對日冕有更多的了解，對太陽隊地球高層大氣微妙影響的瞭解也會得到改善。在美國國家航空暨太空總署（NASA）最近發射的<a href="/wiki/%E5%A4%AA%E9%99%BD%E5%8B%95%E5%8A%9B%E5%AD%B8%E5%A4%A9%E6%96%87%E5%8F%B0" title="太陽動力學天文台">太陽動力學天文台</a>上的大氣成像組件，是接續NASA在日本<a href="/wiki/%E6%97%A5%E5%87%BA%E8%99%9F" class="mw-redirect" title="日出號">日出號</a>衛星上的太陽光學望遠鏡配置的焦平面機組，用來測試這種假設。新的儀器有較高的空間和瞬態解析度揭示了這種日冕物質的供應。 </p><p>這些觀測揭示了加熱到數百萬度的電漿與插入日冕的針狀體間一對一的聯繫<sup id="cite_ref-38" class="reference"><a href="#cite_note-38"><span class="cite-bracket">[</span>38<span class="cite-bracket">]</span></a></sup>。 </p> <div class="mw-heading mw-heading2"><h2 id="相關條目"><span id=".E7.9B.B8.E9.97.9C.E6.A2.9D.E7.9B.AE"></span>相關條目</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=24" title="编辑章节：相關條目"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <div role="navigation" aria-label="Portals" class="noprint portal plainlist tright" style="margin:0.5em 0 0.5em 1em;border:solid #aaa 1px"> <ul 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ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Supra-arcade_downflows" class="extiw" title="en:Supra-arcade downflows"><span lang="en" dir="auto">Supra-arcade downflows</span></a></span>）</span></span></li> <li><span class="ilh-all" data-orig-title="風 (太空船)" data-lang-code="en" data-lang-name="英语" data-foreign-title="WIND (spacecraft)"><span class="ilh-page"><a href="/w/index.php?title=%E9%A2%A8_(%E5%A4%AA%E7%A9%BA%E8%88%B9)&action=edit&redlink=1" class="new" title="風 (太空船)（页面不存在）">風 (太空船)</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/WIND_(spacecraft)" class="extiw" title="en:WIND (spacecraft)"><span lang="en" dir="auto">WIND (spacecraft)</span></a></span>）</span></span></li> <li><a href="/wiki/X%E5%B0%84%E7%BA%BF%E5%A4%A9%E6%96%87%E5%AD%A6" title="X射线天文学">X射线天文学</a></li> <li><a href="/wiki/%E7%81%AB%E5%B1%B1%E5%99%B4%E7%99%BC%E9%A1%9E%E5%9E%8B" title="火山噴發類型">火山噴發類型</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="參考資料"><span id=".E5.8F.83.E8.80.83.E8.B3.87.E6.96.99"></span>參考資料</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=25" title="编辑章节：參考資料"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="reflist columns references-column-width" style="-moz-column-width: 30em; -webkit-column-width: 30em; column-width: 30em; list-style-type: decimal;"> <ol class="references"> <li id="cite_note-Aschwanden-1"><span class="mw-cite-backlink">^ <a href="#cite_ref-Aschwanden_1-0"><sup><b>1.0</b></sup></a> <a href="#cite_ref-Aschwanden_1-1"><sup><b>1.1</b></sup></a></span> <span class="reference-text"><cite class="citation book">Aschwanden, Markus J. Physics of the Solar Corona: An Introduction with Problems and Solutions. Chichester, UK: Praxis Publishing. 2005. <a href="/wiki/Special:%E7%BD%91%E7%BB%9C%E4%B9%A6%E6%BA%90/978-3-540-22321-4" title="Special:网络书源/978-3-540-22321-4"><span title="国际标准书号">ISBN</span> 978-3-540-22321-4</a>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.aufirst=Markus+J.&rft.aulast=Aschwanden&rft.btitle=Physics+of+the+Solar+Corona%3A+An+Introduction+with+Problems+and+Solutions&rft.date=2005&rft.genre=book&rft.isbn=978-3-540-22321-4&rft.place=Chichester%2C+UK&rft.pub=Praxis+Publishing&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-Corfield-2"><span class="mw-cite-backlink"><b><a href="#cite_ref-Corfield_2-0">^</a></b></span> <span class="reference-text"><cite class="citation book">Corfield, Richard. <a rel="nofollow" class="external text" href="https://archive.org/details/livesofplanetsna00corf">Lives of the Planets</a>. Basic Books. 2007. <a href="/wiki/Special:%E7%BD%91%E7%BB%9C%E4%B9%A6%E6%BA%90/978-0-465-01403-3" title="Special:网络书源/978-0-465-01403-3"><span title="国际标准书号">ISBN</span> 978-0-465-01403-3</a>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.aufirst=Richard&rft.aulast=Corfield&rft.btitle=Lives+of+the+Planets&rft.date=2007&rft.genre=book&rft.isbn=978-0-465-01403-3&rft.pub=Basic+Books&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Flivesofplanetsna00corf&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-3"><span class="mw-cite-backlink"><b><a href="#cite_ref-3">^</a></b></span> <span class="reference-text"><cite class="citation book">Hall, Graham; Elliott, Ian; Joeveer, Mihkel; Bònoli, Fabrizio; Langermann, Y. Tzvi; Casulleras, Josep; Sarma, Ke Ve; Bell, Trudy E.; Gurshtein, Alexander A. Maraldi, Giacomo Filippo. Hockey, Thomas (编). <a rel="nofollow" class="external text" href="http://link.springer.com/10.1007/978-0-387-30400-7_899">The Biographical Encyclopedia of Astronomers</a>. New York, NY: Springer New York. 2007: 736–736. <a href="/wiki/Special:%E7%BD%91%E7%BB%9C%E4%B9%A6%E6%BA%90/978-0-387-31022-0" title="Special:网络书源/978-0-387-31022-0"><span title="国际标准书号">ISBN</span> 978-0-387-31022-0</a>. <a rel="nofollow" class="external text" href="https://doi.org/10.1007%2F978-0-387-30400-7_899"><span title="數位物件識別號">doi:10.1007/978-0-387-30400-7_899</span></a> <span style="font-family: sans-serif; cursor: default; color:var(--color-subtle, #54595d); font-size: 0.8em; bottom: 0.1em; font-weight: bold;" title="连接到英语网页">（英语）</span>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.atitle=Maraldi%2C+Giacomo+Filippo&rft.au=B%C3%B2noli%2C+Fabrizio&rft.au=Bell%2C+Trudy+E.&rft.au=Casulleras%2C+Josep&rft.au=Elliott%2C+Ian&rft.au=Gurshtein%2C+Alexander+A.&rft.au=Joeveer%2C+Mihkel&rft.au=Langermann%2C+Y.+Tzvi&rft.au=Sarma%2C+Ke+Ve&rft.aufirst=Graham&rft.aulast=Hall&rft.btitle=The+Biographical+Encyclopedia+of+Astronomers&rft.date=2007&rft.genre=bookitem&rft.isbn=978-0-387-31022-0&rft.pages=736-736&rft.place=New+York%2C+NY&rft.pub=Springer+New+York&rft_id=http%3A%2F%2Flink.springer.com%2F10.1007%2F978-0-387-30400-7_899&rft_id=info%3Adoi%2F10.1007%2F978-0-387-30400-7_899&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-4"><span class="mw-cite-backlink"><b><a href="#cite_ref-4">^</a></b></span> <span class="reference-text"><cite class="citation book">de Ferrer, José Joaquín. Observations of the eclipse of the sun June 16th 1806 made at Kinderhook in the State of New York.. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20220417053712/https://books.google.co.in/books?id=DbkAAAAAYAAJ&pg=PA264">Transactions of the American Philosophical Society</a>. American Philosophical Society. 1809: 264 <span class="reference-accessdate"> [<span class="nowrap">2022-04-17</span>]</span>. （<a rel="nofollow" class="external text" href="https://books.google.co.in/books?id=DbkAAAAAYAAJ&pg=PA264">原始内容</a>存档于2022-04-17） <span style="font-family: sans-serif; cursor: default; color:var(--color-subtle, #54595d); font-size: 0.8em; bottom: 0.1em; font-weight: bold;" title="连接到英语网页">（英语）</span>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.atitle=Observations+of+the+eclipse+of+the+sun+June+16th+1806+made+at+Kinderhook+in+the+State+of+New+York.&rft.aufirst=Jos%C3%A9+Joaqu%C3%ADn&rft.aulast=de+Ferrer&rft.btitle=Transactions+of+the+American+Philosophical+Society&rft.date=1809&rft.genre=bookitem&rft.pages=264&rft.pub=American+Philosophical+Society&rft_id=https%3A%2F%2Fbooks.google.co.in%2Fbooks%3Fid%3DDbkAAAAAYAAJ%26pg%3DPA264&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-5"><span class="mw-cite-backlink"><b><a href="#cite_ref-5">^</a></b></span> <span class="reference-text"><cite class="citation web">Espenak, Fred. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20150405095618/http://mreclipse.com/Totality2/TotalityApH.html">Chronology of Discoveries about the Sun</a>. 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Astronomy & Astrophysics. 2002-04, <b>385</b> (3): 1073–1077. <a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2002A&A...385.1073P"><span title="Bibcode">Bibcode:2002A&A...385.1073P</span></a>. <a rel="nofollow" class="external text" href="//www.worldcat.org/issn/0004-6361"><span title="国际标准连续出版物号">ISSN 0004-6361</span></a>. <a rel="nofollow" class="external text" href="https://doi.org/10.1051%2F0004-6361%3A20020151"><span title="數位物件識別號">doi:10.1051/0004-6361:20020151</span></a>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.atitle=Intermittent+behavior+in+the+transition+region+and+the+low+corona+of+the+quiet+Sun&rft.au=Vial%2C+J.-C.&rft.aufirst=S.&rft.aulast=Patsourakos&rft.date=2002-04&rft.genre=article&rft.issn=0004-6361&rft.issue=3&rft.jtitle=Astronomy+%26+Astrophysics&rft.pages=1073-1077&rft.volume=385&rft_id=http%3A%2F%2Fwww.aanda.org%2F10.1051%2F0004-6361%3A20020151&rft_id=info%3Abibcode%2F2002A%26A...385.1073P&rft_id=info%3Adoi%2F10.1051%2F0004-6361%3A20020151&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-37"><span class="mw-cite-backlink"><b><a href="#cite_ref-37">^</a></b></span> <span class="reference-text"><cite class="citation web"><a rel="nofollow" class="external text" href="http://www.rediff.com/news/slide-show/slide-show-1-mystery-of-suns-hot-outer-atmosphere-solved/20110107.htm">Mystery of Sun's hot outer atmosphere 'solved' – Rediff.com News</a>. Rediff.com. 2011-01-07 <span class="reference-accessdate"> [<span class="nowrap">2012-05-21</span>]</span>. （原始内容<a rel="nofollow" class="external text" href="https://web.archive.org/web/20120415111049/http://www.rediff.com/news/slide-show/slide-show-1-mystery-of-suns-hot-outer-atmosphere-solved/20110107.htm">存档</a>于2012-04-15）.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.btitle=Mystery+of+Sun%27s+hot+outer+atmosphere+%27solved%27+%E2%80%93+Rediff.com+News&rft.date=2011-01-07&rft.genre=unknown&rft.pub=Rediff.com&rft_id=http%3A%2F%2Fwww.rediff.com%2Fnews%2Fslide-show%2Fslide-show-1-mystery-of-suns-hot-outer-atmosphere-solved%2F20110107.htm&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook" class="Z3988"><span style="display:none;"> </span></span></span> </li> <li id="cite_note-38"><span class="mw-cite-backlink"><b><a href="#cite_ref-38">^</a></b></span> <span class="reference-text"><cite class="citation journal">De Pontieu, B.; McIntosh, S. W.; Carlsson, M.; Hansteen, V. H.; Tarbell, T. D.; Boerner, P.; Martinez-Sykora, J.; Schrijver, C. J.; Title, A. M. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20220417053521/https://www.science.org/doi/10.1126/science.1197738">The Origins of Hot Plasma in the Solar Corona</a>. Science. 2011-01-07, <b>331</b> (6013): 55–58 <span class="reference-accessdate"> [<span class="nowrap">2022-04-17</span>]</span>. <a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2011Sci...331...55D"><span title="Bibcode">Bibcode:2011Sci...331...55D</span></a>. <a rel="nofollow" class="external text" href="//www.worldcat.org/issn/0036-8075"><span title="国际标准连续出版物号">ISSN 0036-8075</span></a>. <a rel="nofollow" class="external text" href="//www.ncbi.nlm.nih.gov/pubmed/21212351"><span title="公共医学识别码">PMID 21212351</span></a>. <a rel="nofollow" class="external text" href="https://doi.org/10.1126%2Fscience.1197738"><span title="數位物件識別號">doi:10.1126/science.1197738</span></a>. （<a rel="nofollow" class="external text" href="https://www.science.org/doi/10.1126/science.1197738">原始内容</a>存档于2022-04-17） <span style="font-family: sans-serif; cursor: default; color:var(--color-subtle, #54595d); font-size: 0.8em; bottom: 0.1em; font-weight: bold;" title="连接到英语网页">（英语）</span>.</cite><span title="ctx_ver=Z39.88-2004&rfr_id=info%3Asid%2Fzh.wikipedia.org%3A%E6%98%9F%E5%86%95&rft.atitle=The+Origins+of+Hot+Plasma+in+the+Solar+Corona&rft.au=Boerner%2C+P.&rft.au=Carlsson%2C+M.&rft.au=Hansteen%2C+V.+H.&rft.au=Martinez-Sykora%2C+J.&rft.au=McIntosh%2C+S.+W.&rft.au=Schrijver%2C+C.+J.&rft.au=Tarbell%2C+T.+D.&rft.au=Title%2C+A.+M.&rft.aufirst=B.&rft.aulast=De+Pontieu&rft.date=2011-01-07&rft.genre=article&rft.issn=0036-8075&rft.issue=6013&rft.jtitle=Science&rft.pages=55-58&rft.volume=331&rft_id=https%3A%2F%2Fwww.science.org%2Fdoi%2F10.1126%2Fscience.1197738&rft_id=info%3Abibcode%2F2011Sci...331...55D&rft_id=info%3Adoi%2F10.1126%2Fscience.1197738&rft_id=info%3Apmid%2F21212351&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal" class="Z3988"><span style="display:none;"> </span></span></span> </li> </ol></div> <div class="mw-heading mw-heading2"><h2 id="進階讀物"><span id=".E9.80.B2.E9.9A.8E.E8.AE.80.E7.89.A9"></span>進階讀物</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=26" title="编辑章节：進階讀物"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li>Thorsten Dambeck: <i><a rel="nofollow" class="external text" href="http://www.mpg.de/english/illustrationsDocumentation/multimedia/mpResearch/2008/heft02/011/pdf13.pdf">Seething Cauldron in the Suns's Furnace</a><sup class="noprint Inline-Template"><span style="white-space: nowrap;">[<a href="/wiki/Wikipedia:%E5%A4%B1%E6%95%88%E9%93%BE%E6%8E%A5" title="Wikipedia:失效链接"><span title="">失效連結</span></a>]</span></sup></i>, MaxPlanckResearch, 2/2008, p. 28–33</li> <li>B. N. Dwivedi and A. K. Srivastava <a rel="nofollow" class="external text" href="http://www.ias.ac.in/currsci/10feb2010/295.pdf">Coronal heating by Alfvén waves</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20200721115823/http://www.ias.ac.in/currsci/10feb2010/295.pdf">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>） CURRENT 296 SCIENCE, VOL. 98, NO. 3, 10 FEBRUARY 2010, pp. 295–296</li></ul> <div class="mw-heading mw-heading2"><h2 id="外部連結"><span id=".E5.A4.96.E9.83.A8.E9.80.A3.E7.B5.90"></span>外部連結</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=%E6%98%9F%E5%86%95&action=edit&section=27" title="编辑章节：外部連結"><span>编辑</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r82655521"><div class="side-box side-box-right plainlinks sistersitebox" style="font-size:small;"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r82655520"> <div class="side-box-flex"> <div class="side-box-image"><span class="noviewer" typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/30px-Commons-logo.svg.png" decoding="async" width="30" height="40" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/45px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Commons-logo.svg/59px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></span></span></div> <div class="side-box-text plainlist"><a href="/wiki/%E7%BB%B4%E5%9F%BA%E5%85%B1%E4%BA%AB%E8%B5%84%E6%BA%90" title="维基共享资源">维基共享资源</a>上的相关多媒体资源：<a href="https://commons.wikimedia.org/wiki/Category:Solar_corona" class="extiw" title="commons:Category:Solar corona"><span style="font-weight:bold;">星冕</span></a></div></div> </div> <ul><li><a rel="nofollow" class="external text" href="https://web.archive.org/web/20100223073835/http://solarscience.msfc.nasa.gov/corona.shtml">NASA description of the solar corona</a></li> <li><a rel="nofollow" class="external text" href="http://www.innovations-report.com/html/reports/physics_astronomy/report-33153.html">Coronal heating problem at Innovation Reports</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20081227114327/http://www.innovations-report.com/html/reports/physics_astronomy/report-33153.html">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="https://imagine.gsfc.nasa.gov/docs/science/mysteries_l1/corona.html">NASA/GSFC description of the coronal heating problem</a>（<a rel="nofollow" class="external text" href="//web.archive.org/web/20120213234040/http://imagine.gsfc.nasa.gov/docs/science/mysteries_l1/corona.html">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="http://solar-center.stanford.edu/FAQ/Qcorona.html">FAQ about coronal heating</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20100301054309/http://solar-center.stanford.edu/FAQ/Qcorona.html">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="https://sohowww.nascom.nasa.gov">Solar and Heliospheric Observatory, including near-real-time images of the solar corona</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20110224201848/http://sohowww.nascom.nasa.gov/">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="http://xrt.cfa.harvard.edu/">Coronal x-ray images from the Hinode XRT</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20100311012022/http://xrt.cfa.harvard.edu/">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="https://antwrp.gsfc.nasa.gov/apod/ap090726.html">nasa.gov Astronomy Picture of the Day July 26, 2009</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20101213132307/http://antwrp.gsfc.nasa.gov/apod/ap090726.html">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>） – a combination of thirty-three photographs of the sun's corona that were digitally processed to highlight faint features of a total eclipse that occurred in March 2006</li> <li><a rel="nofollow" class="external text" href="http://alienworlds.southwales.ac.uk/sunStructure.html#/corona">Animated explanation of the core of the Sun</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20151116133527/http://alienworlds.southwales.ac.uk/sunStructure.html#/corona">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>） (University of South Wales)</li> <li><a rel="nofollow" class="external text" href="http://alienworlds.southwales.ac.uk/sunStructure.html#/coronatemp">Animated explanation of the temperature of the Corona</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20151116133527/http://alienworlds.southwales.ac.uk/sunStructure.html#/coronatemp">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>） (University of South Wales)</li> <li><a rel="nofollow" class="external text" href="https://web.archive.org/web/20161203143607/https://sites.google.com/site/ecanrio/Home/referencias/ETMV-Libro_new.pdf?attredirects=0yd=1">Space,time,matter and vacuum: The Solar Corona. A sign of Quantum Gravity?(Spanish)</a></li> <li><a rel="nofollow" class="external text" href="https://web.archive.org/web/20110710155828/http://blogs.physicstoday.org/update/2009/03/alfven-waves-may-heat-the-suns.html">Alfvén waves may heat the Sun's corona</a></li> <li><a rel="nofollow" class="external text" href="http://news.discovery.com/space/sun-heat-mystery-110106.html">New Clue May Solve Solar Mystery</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20121121183413/http://news.discovery.com/space/sun-heat-mystery-110106.html">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="http://www.sciencemag.org/content/331/6013/55.abstract?sid=18d15db8-169c-4ebf-a391-dc1ad55f0fa9">The Origins of Hot Plasma in the Solar Corona</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20150924160815/http://www.sciencemag.org/content/331/6013/55.abstract?sid=18d15db8-169c-4ebf-a391-dc1ad55f0fa9">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li> <li><a rel="nofollow" class="external text" href="https://www.youtube.com/watch?v=o-v9kLLiK4s">Solar Interface Region – Bart de Pontieu (SETI Talks) Video</a> （<a rel="nofollow" class="external text" href="//web.archive.org/web/20201019153156/https://www.youtube.com/watch?v=o-v9kLLiK4s">页面存档备份</a>，存于<a href="/wiki/%E4%BA%92%E8%81%94%E7%BD%91%E6%A1%A3%E6%A1%88%E9%A6%86" title="互联网档案馆">互联网档案馆</a>）</li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r84265675">.mw-parser-output .hlist dl,.mw-parser-output .hlist ol,.mw-parser-output .hlist ul{margin:0;padding:0}.mw-parser-output .hlist dd,.mw-parser-output .hlist dt,.mw-parser-output .hlist li{margin:0;display:inline}.mw-parser-output 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.navbar-brackets::before{margin-right:-0.125em;content:"[ "}.mw-parser-output .navbar-brackets::after{margin-left:-0.125em;content:" ]"}.mw-parser-output .navbar li{word-spacing:-0.125em}.mw-parser-output .navbar a>span,.mw-parser-output .navbar a>abbr{text-decoration:inherit}.mw-parser-output .navbar-mini abbr{font-variant:small-caps;border-bottom:none;text-decoration:none;cursor:inherit}.mw-parser-output .navbar-ct-full{font-size:110%;margin:0 8em}.mw-parser-output .navbar-ct-mini{font-size:110%;margin:0 5em}html.skin-theme-clientpref-night .mw-parser-output .navbar li a abbr{color:var(--color-base)!important}@media(prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .navbar li a abbr{color:var(--color-base)!important}}@media print{.mw-parser-output .navbar{display:none!important}}</style><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:%E5%A4%AA%E9%98%B3" title="Template:太阳"><abbr 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title="差旋層">差旋層</a></li> <li><a href="/wiki/%E5%B0%8D%E6%B5%81%E5%B1%A4_(%E6%81%86%E6%98%9F)" title="對流層 (恆星)">對流層</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="5" style="width:1px;padding:0px 0px 0px 2px"><div><figure class="mw-halign-right mw-image-border" typeof="mw:File"><a href="/wiki/File:The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/b4/The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg/155px-The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg" decoding="async" width="155" height="148" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/b4/The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg/233px-The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/b4/The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg/310px-The_Sun_by_the_Atmospheric_Imaging_Assembly_of_NASA%27s_Solar_Dynamics_Observatory_-_20100819.jpg 2x" data-file-width="4044" data-file-height="3860" /></a><figcaption></figcaption></figure></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%"><a href="/wiki/%E6%81%86%E6%98%9F%E5%A4%A7%E6%B0%A3%E5%B1%A4" title="恆星大氣層">大氣層</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E8%B6%85%E7%B1%B3%E7%B2%92%E7%B5%84%E7%B9%94" title="超米粒組織">超米粒組織</a></li> <li><a href="/wiki/%E7%B1%B3%E7%B2%92%E7%BB%84%E7%BB%87" title="米粒组织">米粒组织</a></li> <li><a href="/wiki/%E5%85%89%E6%96%91" title="光斑">光斑</a></li> <li><a href="/wiki/%E5%A4%AA%E9%98%B3%E9%BB%91%E5%AD%90" title="太阳黑子">太阳黑子</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E8%89%B2%E7%90%83" title="色球">色球</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E8%AD%9C%E6%96%91" title="譜斑">譜斑</a></li> <li><a href="/wiki/%E9%87%9D%E7%8B%80%E9%AB%94" title="針狀體">針狀體</a></li> <li><a href="/wiki/%E8%8E%AB%E7%88%BE%E9%A0%93%E6%B3%A2" title="莫爾頓波">莫爾頓波</a></li> <li><a href="/wiki/%E8%80%80%E6%96%91" title="耀斑">耀斑</a></li> <li><a href="/wiki/%E6%97%A5%E7%8F%A5" title="日珥">日珥</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a class="mw-selflink selflink">日冕</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E9%81%8E%E6%B8%A1%E5%8D%80" title="過渡區">過渡區</a></li> <li><a href="/wiki/%E5%86%95%E6%B4%9E" title="冕洞">冕洞</a></li> <li><a href="/wiki/%E5%86%95%E7%92%B0" title="冕環">冕環</a></li> <li><a href="/wiki/%E6%97%A5%E5%86%95%E5%B7%A8%E9%87%8F%E5%99%B4%E7%99%BC" title="日冕巨量噴發">日冕物質抛射</a></li> <li><a href="/wiki/%E7%9B%94%E7%8B%80%E6%B5%81" title="盔狀流">盔狀流</a></li> <li><a href="/wiki/%E8%B2%BB%E7%B1%B3%E8%BC%9D%E5%85%89" title="費米輝光">費米輝光</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%"><a href="/wiki/%E5%A4%AA%E9%98%B3%E6%B4%BB%E5%8A%A8" title="太阳活动">活動</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F" title="太陽週期">太陽週期</a> <ul><li><a href="/wiki/%E5%A4%AA%E9%99%BD%E9%80%B1%E6%9C%9F%E8%A1%A8" title="太陽週期表">太陽週期表</a></li></ul></li> <li><a href="/wiki/%E5%A4%AA%E9%99%BD%E6%A5%B5%E5%A4%A7%E6%9C%9F" title="太陽極大期">太陽極大期</a></li> <li><a href="/wiki/%E5%A4%AA%E9%99%BD%E6%A5%B5%E5%B0%8F%E6%9C%9F" title="太陽極小期">太陽極小期</a></li> <li><a href="/wiki/%E6%B2%83%E5%A4%AB%E6%95%B8" title="沃夫數">沃夫數</a></li> <li><a href="/wiki/%E8%80%80%E6%96%91" title="耀斑">耀斑</a></li> <li><a href="/wiki/%E6%AF%AB%E5%BE%AE%E9%96%83%E7%84%B0" title="毫微閃焰">毫微閃焰</a></li> <li><a href="/wiki/%E6%97%A5%E9%9C%87" title="日震">日震</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%"><a href="/wiki/%E5%A4%AA%E9%99%BD%E5%9C%88" title="太陽圈">太陽圈</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E5%A4%AA%E9%98%B3%E9%A3%8E" title="太阳风">太阳风</a> <ul><li><a href="/wiki/%E5%A4%AA%E9%99%BD%E5%9C%88%E9%9B%BB%E6%B5%81%E7%89%87" title="太陽圈電流片">電流片</a></li></ul></li> <li><a href="/wiki/%E7%BB%88%E7%AB%AF%E6%BF%80%E6%B3%A2" title="终端激波">终端激波</a></li> <li><a href="/wiki/%E6%97%A5%E9%9E%98" title="日鞘">日鞘</a></li> <li><a href="/wiki/%E6%97%A5%E7%90%83%E5%B1%A4%E9%A0%82" title="日球層頂">日球層頂</a></li> <li><a href="/wiki/%E5%BC%93%E5%BD%A2%E9%9C%87%E6%B3%A2" title="弓形震波">弓形激波</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%">相關條目</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"><span class="nowrap"><a href="/wiki/%E5%A4%AA%E9%98%B3%E6%B4%BB%E5%8A%A8" title="太阳活动">太阳活动</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%99%BD%E5%A4%A9%E6%96%87%E5%AD%B8" title="太陽天文學">太陽天文學</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%99%BD%E7%99%BC%E9%9B%BB%E6%A9%9F" title="太陽發電機">太陽發電機</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%99%BD%E6%9C%9B%E9%81%A0%E9%8F%A1" title="太陽望遠鏡">太陽望遠鏡</a> ·</span> <span class="nowrap"> <a href="/wiki/%E6%97%A5%E9%A3%9F" title="日食">日食</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%98%B3%E5%85%89" title="太阳光">太阳光</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%99%BD%E8%BC%BB%E5%B0%84" title="太陽輻射">太陽輻射</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%98%B3%E8%83%BD" title="太阳能">太阳能</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%98%B3%E7%89%A9%E7%90%86%E5%AD%A6" title="太阳物理学">太阳物理学</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%98%B3%E6%97%A5" title="太阳日">太阳日</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%98%B3%E7%B3%BB" title="太阳系">太阳系</a> ·</span> <span class="nowrap"> <a href="/wiki/%E5%A4%AA%E9%99%BD%E5%B8%B8%E6%95%B8" title="太陽常數">太陽常數</a> ·</span> <span class="nowrap"><a href="/wiki/%E5%A4%AA%E9%98%B3%E4%B8%AD%E5%BE%AE%E5%AD%90%E9%97%AE%E9%A2%98" title="太阳中微子问题">太陽微中子問題</a> ·</span> <span class="nowrap"><a href="/wiki/%E4%B8%AD%E5%BE%AE%E5%AD%90%E6%8C%AF%E8%8D%A1" title="中微子振荡">中微子振盪</a> ·</span> <span class="nowrap"><a href="/wiki/%E8%92%99%E5%BE%B7%E6%A5%B5%E5%B0%8F%E6%9C%9F" title="蒙德極小期">蒙德極小期</a> ·</span> <span class="nowrap"><a href="/wiki/%E5%A4%AA%E9%99%BD%E6%98%9F%E9%9B%B2" title="太陽星雲">太陽星雲</a> ·</span> <span class="nowrap"><a href="/wiki/%E5%A4%AA%E9%98%B3%E7%B3%BB%E7%9A%84%E5%BD%A2%E6%88%90%E4%B8%8E%E6%BC%94%E5%8C%96" title="太阳系的形成与演化">太阳系的形成与演化</a> ·</span> <span class="nowrap"><a href="/wiki/%E6%97%A5%E9%9C%87%E5%AD%B8" title="日震學">日震學</a> ·</span> <span class="nowrap"><a href="/wiki/%E6%A8%99%E6%BA%96%E5%A4%AA%E9%99%BD%E6%A8%A1%E5%9E%8B" title="標準太陽模型">標準太陽模型</a></span></div></td></tr><tr><td class="navbox-abovebelow" colspan="3" style="text-align: center;"><div> <ul><li><a href="/wiki/%E6%81%92%E6%98%9F%E5%85%89%E8%B0%B1" title="恒星光谱">恒星光谱</a>：<a href="/wiki/G%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="G型主序星">G型主序星</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84265675"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84261037"></div><div role="navigation" class="navbox" aria-labelledby="恒星" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="collapsible-title navbox-title" colspan="2"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84265675"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r84244141"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:%E6%81%92%E6%98%9F" title="Template:恒星"><abbr title="查看该模板">查</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:%E6%81%92%E6%98%9F" title="Template talk:恒星"><abbr title="讨论该模板">论</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:%E7%BC%96%E8%BE%91%E9%A1%B5%E9%9D%A2/Template:%E6%81%92%E6%98%9F" title="Special:编辑页面/Template:恒星"><abbr title="编辑该模板">编</abbr></a></li></ul></div><div id="恒星" style="font-size:110%;margin:0 5em"><a href="/wiki/%E6%81%92%E6%98%9F" title="恒星">恒星</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%86%E6%98%9F%E6%BC%94%E5%8C%96" title="恆星演化">演化</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E6%81%86%E6%98%9F%E5%BD%A2%E6%88%90" title="恆星形成">恆星形成</a></li> <li><a href="/wiki/%E4%B8%BB%E5%BA%8F%E5%89%8D%E6%98%9F" title="主序前星">主序前星</a></li> <li><a href="/wiki/%E4%B8%BB%E5%BA%8F%E6%98%9F" title="主序星">主序星</a></li> <li><a href="/wiki/%E6%B0%B4%E5%B9%B3%E5%88%86%E6%94%AF" title="水平分支">水平分支</a> (<a href="/wiki/%E7%B4%85%E7%BE%A4%E8%81%9A" title="紅群聚">紅群聚</a>)</li> <li><a href="/wiki/%E7%B4%85%E5%B7%A8%E6%98%9F%E5%88%86%E6%94%AF" title="紅巨星分支">紅巨星分支</a></li> <li><a href="/wiki/%E6%BC%B8%E8%BF%91%E5%B7%A8%E6%98%9F%E6%94%AF" title="漸近巨星支">漸近巨星分支</a></li> <li><a href="/wiki/%E8%97%8D%E8%BF%B4%E5%9C%88" title="藍迴圈">藍迴圈</a></li> <li><a href="/wiki/%E4%B8%8A%E7%BF%BB" title="上翻">上翻</a></li> <li><a href="/wiki/%E4%B8%8D%E7%A9%A9%E5%AE%9A%E5%B8%B6" title="不穩定帶">不穩定帶</a></li> <li><a href="/wiki/PG_1159%E6%98%9F" title="PG 1159星">PG 1159星</a></li> <li><a href="/wiki/%E8%92%AD%E8%97%81%E8%AE%8A%E6%98%9F" title="蒭藁變星">蒭藁變星</a></li> <li><a href="/wiki/%E8%A1%8C%E6%98%9F%E7%8A%B6%E6%98%9F%E4%BA%91" title="行星状星云">行星状星云</a></li> <li><a href="/wiki/%E5%8E%9F%E8%A1%8C%E6%98%9F%E9%9B%B2" title="原行星雲">原行星雲</a></li> <li><a href="/wiki/%E4%BA%AE%E7%B4%85%E6%96%B0%E6%98%9F" title="亮紅新星">亮紅新星</a></li> <li><a href="/wiki/%E9%AB%98%E5%85%89%E5%BA%A6%E8%97%8D%E8%AE%8A%E6%98%9F" title="高光度藍變星">高光度藍變星</a></li> <li><a href="/wiki/%E6%B2%83%E7%88%BE%E5%A4%AB-%E6%8B%89%E8%91%89%E6%98%9F" title="沃爾夫-拉葉星">沃爾夫-拉葉星</a></li> <li><a href="/wiki/%E5%81%87%E8%B6%85%E6%96%B0%E6%98%9F" title="假超新星">假超新星</a></li> <li><a href="/wiki/%E8%B6%85%E6%96%B0%E6%98%9F" title="超新星">超新星</a></li> <li><a href="/wiki/%E6%A5%B5%E8%B6%85%E6%96%B0%E6%98%9F" title="極超新星">極超新星</a></li> <li><a href="/wiki/%E8%B5%AB%E7%BE%85%E5%9C%96" title="赫羅圖">赫羅圖</a></li> <li><a href="/wiki/%E5%8F%8C%E8%89%B2%E5%9B%BE" title="双色图">双色图</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E5%8E%9F%E6%81%86%E6%98%9F" title="原恆星">原恆星</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E5%88%86%E5%AD%90%E9%9B%B2" title="分子雲">分子雲</a> <ul><li><a href="/wiki/%E7%94%B5%E7%A6%BB%E6%B0%A2%E5%8C%BA" title="电离氢区">电离氢区</a></li></ul></li> <li><a href="/wiki/%E5%8C%85%E5%85%8B%E9%9B%B2%E7%90%83" title="包克雲球">包克雲球</a></li> <li><a href="/wiki/%E5%88%9D%E6%9C%9F%E6%81%86%E6%98%9F%E9%AB%94" title="初期恆星體">初期恆星體</a></li> <li><a href="/wiki/%E8%B5%AB%E6%AF%94%E6%A0%BC-%E5%93%88%E7%BE%85%E5%A4%A9%E9%AB%94" title="赫比格-哈羅天體">赫比格-哈羅天體</a></li> <li><a href="/wiki/%E6%9E%97%E8%BB%8C%E8%B7%A1" title="林軌跡">林忠四郎軌跡</a></li> <li><a href="/wiki/%E6%9E%97%E6%A5%B5%E9%99%90" title="林極限">林忠四郎極限</a></li> <li><a href="/wiki/%E4%BA%A8%E8%80%B6%E8%B7%A1" title="亨耶跡">亨耶跡</a></li> <li><a href="/wiki/%E7%8D%B5%E6%88%B6%E5%9E%8B%E8%AE%8A%E6%98%9F" title="獵戶型變星">獵戶型變星</a> <ul><li><a href="/wiki/%E9%87%91%E7%89%9BT%E6%98%9F" title="金牛T星">金牛T星</a></li> <li><a href="/wiki/%E7%8D%B5%E6%88%B6FU%E5%9E%8B%E8%AE%8A%E6%98%9F" title="獵戶FU型變星">獵戶FU型變星</a></li></ul></li> <li><a href="/wiki/%E8%B5%AB%E6%AF%94%E6%A0%BCAe/Be%E6%98%9F" title="赫比格Ae/Be星">赫比格Ae/Be星</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">光度分类</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E6%AC%A1%E7%9F%AE%E6%98%9F" title="次矮星">次矮星</a></li> <li><a href="/wiki/%E4%B8%BB%E5%BA%8F%E6%98%9F" title="主序星">主序星</a> <ul><li><a href="/wiki/%E8%97%8D%E7%9F%AE%E6%98%9F_(%E7%B4%85%E7%9F%AE%E6%98%9F%E9%9A%8E%E6%AE%B5)" title="藍矮星 (紅矮星階段)">藍</a></li> <li><a href="/wiki/K%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="K型主序星">橙</a></li> <li><a href="/wiki/%E7%B4%85%E7%9F%AE%E6%98%9F" title="紅矮星">紅</a></li> <li><a href="/wiki/%E6%A3%95%E7%9F%AE%E6%98%9F" title="棕矮星">棕</a></li> <li><a href="/wiki/G%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="G型主序星">黃</a></li></ul></li> <li><a href="/wiki/%E6%AC%A1%E5%B7%A8%E6%98%9F" title="次巨星">次巨星</a></li> <li><a href="/wiki/%E5%B7%A8%E6%98%9F" title="巨星">巨星</a> <ul><li><a href="/wiki/%E7%B4%85%E5%B7%A8%E6%98%9F" title="紅巨星">紅</a></li> <li><a href="/wiki/%E8%97%8D%E5%B7%A8%E6%98%9F" title="藍巨星">蓝</a></li></ul></li> <li><a href="/wiki/%E4%BA%AE%E5%B7%A8%E6%98%9F" title="亮巨星">亮巨星</a></li> <li><a href="/wiki/%E8%B6%85%E5%B7%A8%E6%98%9F" title="超巨星">超巨星</a> <ul><li><a href="/wiki/%E8%97%8D%E8%B6%85%E5%B7%A8%E6%98%9F" title="藍超巨星">藍</a></li> <li><a href="/wiki/%E7%B4%85%E8%B6%85%E5%B7%A8%E6%98%9F" title="紅超巨星">紅</a></li> <li><a href="/wiki/%E9%BB%84%E8%B6%85%E5%B7%A8%E6%98%9F" title="黄超巨星">黃</a></li></ul></li> <li><a href="/wiki/%E7%89%B9%E8%B6%85%E5%B7%A8%E6%98%9F" title="特超巨星">特超巨星</a> <ul><li><a href="/wiki/%E9%BB%83%E7%89%B9%E8%B6%85%E5%B7%A8%E6%98%9F" title="黃特超巨星">黃</a></li></ul></li> <li><a href="/wiki/%E8%97%8D%E6%8E%89%E9%9A%8A%E6%98%9F" title="藍掉隊星">藍掉隊星</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%92%E6%98%9F%E5%85%89%E8%B0%B1" title="恒星光谱">光谱分类</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/O%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="O型主序星">O</a></li> <li><a href="/wiki/B%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="B型主序星">B</a></li> <li><a href="/wiki/A%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="A型主序星">A</a></li> <li><a href="/wiki/F%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="F型主序星">F</a></li> <li><a href="/wiki/G%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="G型主序星">G</a></li> <li><a href="/wiki/K%E5%9E%8B%E4%B8%BB%E5%BA%8F%E6%98%9F" title="K型主序星">K</a></li> <li><a href="/wiki/%E7%B4%85%E7%9F%AE%E6%98%9F" title="紅矮星">M</a></li> <li><a href="/wiki/Be%E6%98%9F" title="Be星">Be</a></li> <li><a href="/wiki/OB%E6%98%9F" title="OB星">OB</a></li> <li><a href="/wiki/B%E5%9E%8B%E6%AC%A1%E7%9F%AE%E6%98%9F" title="B型次矮星">B型次矮星</a></li> <li><a href="/wiki/%E6%99%9A%E6%9C%9F%E5%9E%8B%E6%98%9F" title="晚期型星">晚期型星</a></li> <li><a href="/wiki/%E7%89%B9%E6%AE%8A%E6%81%86%E6%98%9F" title="特殊恆星">特殊恆星</a> <ul><li><a href="/wiki/%E9%87%91%E5%B1%AC%E7%B7%9A%E6%98%9F" title="金屬線星">金屬線星</a></li> <li><a href="/wiki/Ap%E5%92%8CBp%E6%98%9F" title="Ap和Bp星">Ap和Bp星</a> <ul><li><a href="/wiki/%E5%BF%AB%E9%80%9F%E6%8C%AF%E7%9B%AAAp%E6%98%9F" title="快速振盪Ap星">快速振盪Ap星</a></li></ul></li> <li><a href="/wiki/%E9%8B%87%E6%98%9F" title="鋇星">鋇星</a></li> <li><a href="/wiki/%E7%A2%B3%E6%98%9F" title="碳星">碳星</a></li> <li><a href="/wiki/CN%E6%98%9F" title="CN星">CN星</a></li> <li><a href="/wiki/CH%E6%98%9F" title="CH星">CH星</a></li> <li><a href="/wiki/%E6%A5%B5%E7%AB%AF%E6%B0%A6%E6%98%9F" title="極端氦星">極端氦星</a></li> <li><a href="/wiki/%E7%89%A7%E5%A4%AB%E5%BA%A7%CE%BB%E5%9E%8B%E6%98%9F" title="牧夫座λ型星">牧夫λ</a></li> <li><a href="/wiki/%E9%89%9B%E6%98%9F" title="鉛星">鉛星</a></li> <li><a href="/wiki/%E6%B1%9E%E9%8C%B3%E6%98%9F" title="汞錳星">汞錳星</a></li> <li><a href="/wiki/S%E5%9E%8B%E6%98%9F" title="S型星">S型星</a></li> <li><a href="/wiki/%E6%AE%BC%E5%B1%A4%E6%98%9F" title="殼層星">殼層星</a></li> <li><a href="/wiki/%E9%8D%80%E6%98%9F" title="鍀星">鍀星</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">残骸</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E7%99%BD%E7%9F%AE%E6%98%9F" title="白矮星">白矮星</a> <ul><li><a href="/wiki/%E6%B0%A6%E8%A1%8C%E6%98%9F" title="氦行星">氦行星</a></li> <li><a href="/wiki/%E9%BB%91%E7%9F%AE%E6%98%9F" title="黑矮星">黑矮星</a></li></ul></li> <li><a href="/wiki/%E4%B8%AD%E5%AD%90%E6%98%9F" title="中子星">中子星</a> <ul><li><a href="/wiki/%E8%84%89%E5%86%B2%E6%98%9F" title="脉冲星">脉冲星</a> <ul><li><a href="/wiki/X%E5%B0%84%E7%BA%BF%E8%84%89%E5%86%B2%E6%98%9F" title="X射线脉冲星">X射线</a></li></ul></li> <li><a href="/wiki/%E7%A3%81%E6%98%9F" title="磁星">磁星</a></li></ul></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E9%BB%91%E6%B4%9E" title="恆星黑洞">恆星黑洞</a></li> <li><a href="/wiki/%E8%87%B4%E5%AF%86%E6%98%9F" title="致密星">致密星</a></li> <li><a href="/wiki/X%E5%B0%84%E7%BA%BF%E8%81%94%E6%98%9F" title="X射线联星">X射线联星</a> <ul><li><a href="/wiki/X%E5%B0%84%E7%B7%9A%E7%88%86%E7%99%BC%E6%BA%90" title="X射線爆發源">X射線爆發源</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">纯理论恒星</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E8%97%8D%E7%9F%AE%E6%98%9F_(%E7%B4%85%E7%9F%AE%E6%98%9F%E9%9A%8E%E6%AE%B5)" title="藍矮星 (紅矮星階段)">藍矮星</a></li> <li><a href="/wiki/%E7%B6%A0%E8%89%B2%E6%98%9F" title="綠色星">綠色星</a></li> <li><a href="/wiki/%E9%BB%91%E7%9F%AE%E6%98%9F" title="黑矮星">黑矮星</a></li> <li><a href="/wiki/%E5%A5%87%E7%89%B9%E6%98%9F" title="奇特星">奇特星</a> <ul><li><a href="/wiki/%E5%85%88%E5%AD%90%E6%98%9F" title="先子星">先子星</a></li> <li><span class="ilh-all" data-orig-title="普朗克恒星" data-lang-code="en" data-lang-name="英语" data-foreign-title="Planck star"><span class="ilh-page"><a href="/w/index.php?title=%E6%99%AE%E6%9C%97%E5%85%8B%E6%81%92%E6%98%9F&action=edit&redlink=1" class="new" title="普朗克恒星（页面不存在）">普朗克恒星</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Planck_star" class="extiw" title="en:Planck star"><span lang="en" dir="auto">Planck star</span></a></span>）</span></span></li> <li><a href="/wiki/%E5%A4%B8%E5%85%8B%E6%98%9F" title="夸克星">夸克星</a></li> <li><a href="/wiki/%E6%9A%97%E6%98%9F" class="mw-disambig" title="暗星">暗物质星</a></li> <li><a href="/wiki/Q%E6%98%9F" title="Q星">Q星</a></li></ul></li> <li><span class="ilh-all" data-orig-title="冰冻恒星" data-lang-code="fr" data-lang-name="法语" data-foreign-title="Étoile congelée"><span class="ilh-page"><a href="/w/index.php?title=%E5%86%B0%E5%86%BB%E6%81%92%E6%98%9F&action=edit&redlink=1" class="new" title="冰冻恒星（页面不存在）">冰冻恒星</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">法语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://fr.wikipedia.org/wiki/%C3%89toile_congel%C3%A9e" class="extiw" title="fr:Étoile congelée"><span lang="fr" dir="auto">Étoile congelée</span></a></span>）</span></span></li> <li><a href="/wiki/%E7%B1%BB%E6%98%9F" title="类星">类星</a></li> <li><a href="/wiki/%E7%B4%A2%E6%81%A9-%E7%A5%96%E7%89%B9%E9%98%94%E5%A4%AB%E5%A4%A9%E4%BD%93" title="索恩-祖特阔夫天体">索恩-祖特闊夫天體</a></li> <li><a href="/wiki/%E9%90%B5%E6%98%9F" title="鐵星">鐵星</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%86%E6%98%9F%E6%A0%B8%E5%90%88%E6%88%90" title="恆星核合成">核合成</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E6%B0%A6%E6%A0%B8%E4%BD%9C%E7%94%A8" title="氦核作用">氦核作用</a></li> <li><a href="/wiki/3%E6%B0%A6%E9%81%8E%E7%A8%8B" title="3氦過程">3氦過程</a></li> <li><a href="/wiki/%E8%B3%AA%E5%AD%90%E2%80%94%E8%B3%AA%E5%AD%90%E9%8F%88%E5%8F%8D%E6%87%89" title="質子—質子鏈反應">質子—質子鏈反應</a></li> <li><a href="/wiki/%E6%B0%A6%E9%96%83" title="氦閃">氦閃</a></li> <li><a href="/wiki/%E7%A2%B3%E6%B0%AE%E6%B0%A7%E5%BE%AA%E7%92%B0" title="碳氮氧循環">碳氮氧循環</a></li> <li><a href="/wiki/%E9%8B%B0%E7%87%83%E7%87%92" title="鋰燃燒">鋰燃燒</a></li> <li><a href="/wiki/%E7%A2%B3%E8%81%9A%E5%8F%98" title="碳聚变">碳燃烧</a></li> <li><a href="/wiki/%E6%B0%96%E7%87%83%E7%87%92%E9%81%8E%E7%A8%8B" title="氖燃燒過程">氖燃烧</a></li> <li><a href="/wiki/%E6%B0%A7%E7%87%83%E7%87%92%E9%81%8E%E7%A8%8B" title="氧燃燒過程">氧燃烧</a></li> <li><a href="/wiki/%E7%9F%BD%E7%87%83%E7%87%92%E9%81%8E%E7%A8%8B" title="矽燃燒過程">硅燃烧</a></li> <li><a href="/wiki/S%E9%81%8E%E7%A8%8B" title="S過程">s過程</a></li> <li><a href="/wiki/R%E9%81%8E%E7%A8%8B" title="R過程">r過程</a></li> <li><a href="/wiki/%E6%A0%B8%E8%9E%8D%E5%90%88%E9%AB%94" title="核融合體">核融合體</a></li> <li><a href="/wiki/%E6%96%B0%E6%98%9F" title="新星">新星</a> <ul><li><a href="/wiki/%E6%96%B0%E6%98%9F%E9%81%97%E8%BF%B9" title="新星遗迹">新星遗迹</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%86%E6%98%9F%E7%B5%90%E6%A7%8B" title="恆星結構">结构</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E5%A4%AA%E9%99%BD%E6%A0%B8%E5%BF%83" title="太陽核心">核心</a></li> <li><a href="/wiki/%E5%B0%8D%E6%B5%81%E5%B1%A4_(%E6%81%86%E6%98%9F)" title="對流層 (恆星)">对流层</a> <ul><li><span class="ilh-all" data-orig-title="微湍流" data-lang-code="en" data-lang-name="英语" data-foreign-title="Microturbulence"><span class="ilh-page"><a href="/w/index.php?title=%E5%BE%AE%E6%B9%8D%E6%B5%81&action=edit&redlink=1" class="new" title="微湍流（页面不存在）">微湍流</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/Microturbulence" class="extiw" title="en:Microturbulence"><span lang="en" dir="auto">Microturbulence</span></a></span>）</span></span></li></ul></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E5%A4%A7%E6%B0%A3%E5%B1%A4" title="恆星大氣層">大气层</a> <ul><li><a href="/wiki/%E8%BC%BB%E5%B0%84%E5%B1%A4" title="輻射層">輻射層</a></li> <li><a href="/wiki/%E5%85%89%E7%90%83" title="光球">光球层</a></li> <li><a href="/wiki/%E8%89%B2%E7%90%83" title="色球">色球层</a></li> <li><a href="/wiki/%E6%98%9F%E6%96%91" title="星斑">星斑</a></li> <li><a class="mw-selflink selflink">冕</a></li></ul></li> <li><a href="/wiki/%E6%98%9F%E9%A3%8E" title="星风">星风</a> <ul><li><a href="/wiki/%E6%98%9F%E9%A2%A8%E6%B3%A1" title="星風泡">星風泡</a></li></ul></li> <li><a href="/wiki/%E6%98%9F%E9%9C%87%E5%AD%B8" title="星震學">星震學</a></li> <li><a href="/wiki/%E7%88%B1%E4%B8%81%E9%A1%BF%E5%85%89%E5%BA%A6" title="爱丁顿光度">爱丁顿光度</a></li> <li><a href="/wiki/%E5%85%8B%E8%B5%AB%E6%AD%B7%E7%A8%8B" title="克赫歷程">开尔文-亥姆霍兹机制</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">特徵</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E6%81%86%E6%98%9F%E5%91%BD%E5%90%8D" title="恆星命名">命名</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E5%8B%95%E5%8A%9B%E5%AD%B8" title="恆星動力學">动力学</a></li> <li><a href="/wiki/%E6%9C%89%E6%95%88%E6%BA%AB%E5%BA%A6" title="有效溫度">有效溫度</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E9%81%8B%E5%8B%95%E5%AD%B8" title="恆星運動學">运动学</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E7%A3%81%E5%A0%B4" title="恆星磁場">磁场</a></li> <li><a href="/wiki/%E8%A7%86%E6%98%9F%E7%AD%89" title="视星等">视星等</a></li> <li><a href="/wiki/%E7%B5%95%E5%B0%8D%E6%98%9F%E7%AD%89" title="絕對星等">絕對星等</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E8%B3%AA%E9%87%8F" title="恆星質量">质量</a></li> <li><a href="/wiki/%E9%87%91%E5%B1%AC%E9%87%8F" title="金屬量">金屬量</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E8%87%AA%E8%BD%89" title="恆星自轉">自转</a></li> <li><a href="/wiki/UBV%E6%B5%8B%E5%85%89%E7%B3%BB%E7%BB%9F" title="UBV测光系统">UBV色</a></li> <li><a href="/wiki/%E8%AE%8A%E6%98%9F" title="變星">變星</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%86%E6%98%9F%E7%B3%BB%E7%B5%B1" title="恆星系統">恆星系統</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E9%9B%99%E6%98%9F" title="雙星">雙星</a> <ul><li><a href="/wiki/%E5%AF%86%E6%8E%A5%E8%81%AF%E6%98%9F" title="密接聯星">密接聯星</a></li> <li><a href="/wiki/%E5%85%B1%E6%9C%89%E5%8C%85%E5%B1%A4" title="共有包層">共有包層</a></li></ul></li> <li><a href="/wiki/%E8%81%9A%E6%98%9F" title="聚星">聚星</a></li> <li><a href="/wiki/%E5%90%B8%E7%A7%AF%E7%9B%98" title="吸积盘">吸积盘</a></li> <li><a href="/wiki/%E8%A1%8C%E6%98%9F%E7%B3%BB" title="行星系">行星系</a></li> <li><a href="/wiki/%E5%A4%AA%E9%98%B3%E7%B3%BB" title="太阳系">太阳系</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">地球视角</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E5%8C%97%E6%9E%81%E6%98%9F" title="北极星">北极星</a></li> <li><a href="/wiki/%E6%8B%B1%E6%A5%B5%E6%98%9F" title="拱極星">拱極星</a></li> <li><a href="/wiki/%E6%98%9F%E7%AD%89" title="星等">星等</a></li> <li><a href="/wiki/%E6%B6%88%E5%85%89" title="消光">消光</a></li> <li><a href="/wiki/%E5%8F%8C%E8%89%B2%E5%9B%BE" title="双色图">双色图</a></li> <li><a href="/wiki/%E5%BE%91%E5%90%91%E9%80%9F%E5%BA%A6" title="徑向速度">视向速度</a></li> <li><a href="/wiki/%E8%87%AA%E8%A1%8C" title="自行">自行</a></li> <li><a href="/wiki/%E8%A7%86%E5%B7%AE" title="视差">视差</a></li> <li><a href="/wiki/%E6%B5%8B%E5%85%89%E6%A0%87%E5%87%86%E6%98%9F" title="测光标准星">测光标准星</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/%E6%81%92%E6%98%9F%E5%88%97%E8%A1%A8" title="恒星列表">恒星列表</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><span class="ilh-all" data-orig-title="普通星名表" data-lang-code="en" data-lang-name="英语" data-foreign-title="List of proper names of stars"><span class="ilh-page"><a href="/w/index.php?title=%E6%99%AE%E9%80%9A%E6%98%9F%E5%90%8D%E8%A1%A8&action=edit&redlink=1" class="new" title="普通星名表（页面不存在）">普通星名表</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/List_of_proper_names_of_stars" class="extiw" title="en:List of proper names of stars"><span lang="en" dir="auto">List of proper names of stars</span></a></span>）</span></span> <ul><li><span class="ilh-all" data-orig-title="阿拉伯星名表" data-lang-code="en" data-lang-name="英语" data-foreign-title="List of Arabic star names"><span class="ilh-page"><a href="/w/index.php?title=%E9%98%BF%E6%8B%89%E4%BC%AF%E6%98%9F%E5%90%8D%E8%A1%A8&action=edit&redlink=1" class="new" title="阿拉伯星名表（页面不存在）">阿拉伯星名表</a></span><span class="noprint ilh-comment">（<span class="ilh-lang">英语</span><span class="ilh-colon">：</span><span class="ilh-link"><a href="https://en.wikipedia.org/wiki/List_of_Arabic_star_names" class="extiw" title="en:List of Arabic star names"><span lang="en" dir="auto">List of Arabic star names</span></a></span>）</span></span></li> <li><a href="/wiki/%E4%B8%AD%E8%A5%BF%E6%98%9F%E5%90%8D%E5%B0%8D%E7%85%A7%E8%A1%A8" title="中西星名對照表">中西星名對照表</a></li></ul></li> <li><a href="/wiki/%E6%98%9F%E5%BA%A7%E6%81%92%E6%98%9F%E5%88%97%E8%A1%A8" title="星座恒星列表">星座恒星</a></li> <li><a href="/wiki/%E5%B7%A8%E5%A4%A7%E8%B3%AA%E9%87%8F%E6%81%86%E6%98%9F%E5%88%97%E8%A1%A8" title="巨大質量恆星列表">巨大质量恒星</a></li> <li><a href="/wiki/%E6%9C%80%E5%B0%8F%E8%B3%AA%E9%87%8F%E6%81%86%E6%98%9F%E5%88%97%E8%A1%A8" title="最小質量恆星列表">最小质量恒星</a></li> <li><a href="/wiki/%E5%B7%A8%E5%A4%A7%E6%81%86%E6%98%9F%E5%88%97%E8%A1%A8" title="巨大恆星列表">巨大恒星</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E5%85%89%E5%BA%A6%E5%88%97%E8%A1%A8" title="恆星光度列表">恒星光度</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E4%BA%AE%E5%BA%A6%E5%88%97%E8%A1%A8" title="恆星亮度列表">恒星亮度</a></li> <li><a href="/wiki/%E9%84%B0%E8%BF%91%E6%81%86%E6%98%9F%E5%88%97%E8%A1%A8" title="鄰近恆星列表">临近恒星</a></li> <li><a href="/wiki/%E6%A3%95%E7%9F%AE%E6%98%9F%E5%88%97%E8%A1%A8" title="棕矮星列表">棕矮星</a></li> <li><a href="/wiki/%E8%A1%8C%E6%98%9F%E7%8A%B6%E6%98%9F%E4%BA%91%E5%88%97%E8%A1%A8" title="行星状星云列表">行星状星云</a></li> <li><a href="/wiki/%E8%B6%85%E6%96%B0%E6%98%9F%E5%88%97%E8%A1%A8" title="超新星列表">超新星</a></li> <li><a href="/wiki/%E8%B6%85%E6%96%B0%E6%98%9F%E5%80%99%E9%81%B8%E5%88%97%E8%A1%A8" title="超新星候選列表">超新星候选</a></li> <li><a href="/wiki/%E8%AE%8A%E6%98%9F%E5%88%97%E8%A1%A8" title="變星列表">变星</a></li> <li><a href="/wiki/%E4%BB%A5%E4%BA%BA%E5%90%8D%E5%91%BD%E5%90%8D%E7%9A%84%E6%81%86%E6%98%9F" title="以人名命名的恆星">以人名命名的恆星</a></li> <li><a href="/wiki/%E6%81%86%E6%98%9F%E5%A4%A9%E6%96%87%E5%AD%B8%E5%B9%B4%E8%A1%A8" title="恆星天文學年表">恆星天文學年表</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">相关条目</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0px"><div style="padding:0em 0.25em"> <ul><li><a href="/wiki/%E4%BA%9A%E6%81%92%E6%98%9F" title="亚恒星">亚恒星</a> <ul><li><a href="/wiki/%E6%A3%95%E7%9F%AE%E6%98%9F" title="棕矮星">棕矮星</a></li> <li><a href="/wiki/%E6%AC%A1%E6%A3%95%E7%9F%AE%E6%98%9F" title="次棕矮星">次棕矮星</a></li> <li><a href="/wiki/%E6%81%86%E8%A1%8C%E6%98%9F" title="恆行星">恆行星</a></li></ul></li> <li><a href="/wiki/%E5%BE%8C%E6%BC%B8%E8%BF%91%E5%B7%A8%E6%98%9F%E6%94%AF%E6%98%9F" title="後漸近巨星支星">後漸近巨星支星</a></li> <li><a href="/wiki/%E6%98%9F%E5%9B%A2" title="星团">星团</a> <ul><li><a href="/wiki/%E7%96%8F%E6%95%A3%E6%98%9F%E5%9B%A2" title="疏散星团">疏散星团</a></li> <li><a href="/wiki/%E7%90%83%E7%8B%80%E6%98%9F%E5%9C%98" title="球狀星團">球狀星團</a></li></ul></li> <li><a href="/wiki/%E6%98%9F%E7%B3%BB" title="星系">星系</a></li> <li><a href="/wiki/%E9%8A%80%E6%B2%B3%E5%B9%B4" title="銀河年">銀河年</a></li> <li><a href="/wiki/%E8%B6%85%E6%98%9F%E7%B3%BB%E5%9C%98" title="超星系團">超星系團</a></li> <li><a href="/wiki/%E6%97%A5%E9%9C%87%E5%AD%B8" title="日震學">日震學</a></li> <li><a href="/wiki/%E5%AE%A2%E6%98%9F" title="客星">客星</a></li> <li><a href="/wiki/%E6%98%9F%E5%BA%A7" title="星座">星座</a></li> <li><a href="/wiki/%E6%98%9F%E7%BE%A4" title="星群">星群</a></li> <li><a href="/wiki/%E5%BC%95%E5%8A%9B" title="引力">引力</a></li> <li><a href="/wiki/%E6%98%9F%E7%B3%BB%E9%9A%9B%E6%81%86%E6%98%9F" title="星系際恆星">星系際恆星</a></li> <li><a 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