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</ul> </li> <li id="toc-See_also" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#See_also"> <div class="vector-toc-text"> 6 See also </div> </a> <ul id="toc-See_also-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Notes_and_references" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Notes_and_references"> <div class="vector-toc-text"> 7 Notes and references </div> </a> <ul id="toc-Notes_and_references-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-External_links" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#External_links"> <div class="vector-toc-text"> 8 External links </div> </a> <ul id="toc-External_links-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="Contents" 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="Toggle the table of contents" > <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" > Toggle the table of contents </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">List of exoplanet extremes</h1> <div 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The properties listed here are those for which values are known reliably. It is important to note that the study of exoplanets is one of the most dynamic emerging fields of science, and these values may change wildly as new discoveries are made. <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Extremes_from_Earth's_viewpoint">Extremes from Earth's viewpoint</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=1" title="Edit section: Extremes from Earth's viewpoint">edit</a>]</div> <table class="wikitable"> <tbody><tr> <th>Title </th> <th>Planet </th> <th>Star </th> <th>Data </th> <th>Notes </th></tr> <tr> <td>Most distant discovered </td> <td><a href="/wiki/SWEEPS-11" title="SWEEPS-11">SWEEPS-11</a> / <a href="/wiki/SWEEPS-04" title="SWEEPS-04">SWEEPS-04</a> </td> <td>SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6 </td> <td>27 710 <a href="/wiki/Light-year" title="Light-year">light-years</a><a href="#cite_note-1">[1]</a> </td> <td>Several candidate <a href="/wiki/Extragalactic_planet" title="Extragalactic planet">extragalactic planets</a> have been detected. Assuming the largest distance value from the <a href="/wiki/Gravitational_microlensing" title="Gravitational microlensing">microlensing</a> light-curve, the planet OGLE-2017-BLG-0364Lb might be more distant, at around 32 600 light-years (10 000 <a href="/wiki/Parsec" title="Parsec">pc</a>).<a href="#cite_note-2">[2]</a> <a href="/wiki/SGR_1935%2B2154" title="SGR 1935+2154">SGR 1935+2154 b</a> could also be the most distant exoplanet, with distance estimates ranging from 21,500<a href="#cite_note-Shao2024-3">[3]</a> to 28,400 ly.<a href="#cite_note-Kurban2024-4">[4]</a> The most distant potentially habitable planet confirmed is <a href="/wiki/Kepler-1606b" class="mw-redirect" title="Kepler-1606b">Kepler-1606b</a>, at 2870 <a href="/wiki/Light-year" title="Light-year">light-years</a> distant,<a href="#cite_note-5">[5]</a> although the unconfirmed planet <a href="/w/index.php?title=KOI-5889.01&action=edit&redlink=1" class="new" title="KOI-5889.01 (page does not exist)">KOI-5889.01</a> is over 5000 light-years distant. On 31 March 2022, <a href="/wiki/K2-2016-BLG-0005Lb" title="K2-2016-BLG-0005Lb">K2-2016-BLG-0005Lb</a> was reported to be the most distant <a href="/wiki/Exoplanet" title="Exoplanet">exoplanet</a> discovered by the <a href="/wiki/Kepler_space_telescope" title="Kepler space telescope">Kepler telescope</a>, at 17 000 light-years away.<a href="#cite_note-ARX_20220331-6">[6]</a> </td></tr> <tr> <td><a href="/wiki/List_of_nearest_exoplanets" title="List of nearest exoplanets">Least distant</a> </td> <td><a href="/wiki/Proxima_Centauri_b" title="Proxima Centauri b">Proxima Centauri b</a>, (<a href="/wiki/Proxima_Centauri_c" title="Proxima Centauri c">c</a> and <a href="/wiki/Proxima_Centauri_d" title="Proxima Centauri d">d</a>) </td> <td><a href="/wiki/Proxima_Centauri" title="Proxima Centauri">Proxima Centauri</a> </td> <td>4.25 light-years </td> <td>Proxima Centauri b and (the candidate planet) d are the closest potentially rocky exoplanets,<a href="#cite_note-7">[7]</a> b is the closest <a href="/wiki/List_of_potentially_habitable_exoplanets" title="List of potentially habitable exoplanets">potentially habitable exoplanet</a> known, and (the disputed planet) c is the closest <a href="/wiki/Mini-Neptune" title="Mini-Neptune">mini-Neptune</a>/<a href="/wiki/Super-Earth" title="Super-Earth">Super-Earth</a> and potentially ringed planet. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25 000 years), this is an absolute record. </td></tr> <tr> <td>Most distant directly visible </td> <td><a href="/wiki/CT_Chamaeleontis_b" class="mw-redirect" title="CT Chamaeleontis b">CT Chamaeleontis b</a> </td> <td><a href="/wiki/CT_Chamaeleontis" title="CT Chamaeleontis">CT Chamaeleontis</a> </td> <td>622 light-years<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td>The disputed planet candidate <a href="/wiki/CVSO_30_c" class="mw-redirect" title="CVSO 30 c">CVSO 30 c</a> may be more distant, at 1,200 <a href="/wiki/Light-year" title="Light-year">light-years</a>. </td></tr> <tr> <td>Closest directly visible </td> <td><a href="/wiki/Epsilon_Indi_Ab" title="Epsilon Indi Ab">Epsilon Indi Ab</a> </td> <td><a href="/wiki/Epsilon_Indi" title="Epsilon Indi">Epsilon Indi</a> </td> <td>12.05 light-years </td> <td><a href="/wiki/COCONUTS-2b" title="COCONUTS-2b">COCONUTS-2b</a> at 35.5 light-years is the next closest directly visible.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> <a href="/wiki/Proxima_Centauri_c" title="Proxima Centauri c">Proxima Centauri c</a> (confirmed in 2020 using archival Hubble data from 1995+) may have been directly imaged.<a href="#cite_note-Gratton2020-9">[9]</a> </td></tr> <tr> <td>Star with the brightest <a href="/wiki/Apparent_magnitude" title="Apparent magnitude">apparent magnitude</a> with a planet </td> <td><a href="/wiki/Alpha_Arietis_b#Hamal" class="mw-redirect" title="Alpha Arietis b">Alpha Arietis</a> </td> <td><a href="/wiki/Hamal" title="Hamal">Hamal</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a><a href="#cite_note-10">[a]</a> </td> <td>Apparent magnitude is 2.005 </td> <td><a href="/wiki/Alpha_Centauri" title="Alpha Centauri">Alpha Centauri</a> A (apparent magnitude 0.01) has a planet candidate. The evidence of planets around <a href="/wiki/Vega" title="Vega">Vega</a> with an apparent magnitude of 0.03 is strongly suggested by <a href="/wiki/Circumstellar_disk" class="mw-redirect" title="Circumstellar disk">circumstellar disks</a> surrounding it.<a href="#cite_note-11">[10]</a> As of 2021<a class="external text" href="https://en.wikipedia.org/w/index.php?title=List_of_exoplanet_extremes&action=edit">[update]</a>, a candidate planet around Vega has been detected.<a href="#cite_note-Hurt2021-12">[11]</a> <a href="/wiki/Aldebaran" title="Aldebaran">Aldebaran</a> (apparent magnitude varies between 0.75 and 0.95) was suspected to have a candidate planet, however later studies found the existence of the planet inconclusive.<a href="#cite_note-Reichert2019-13">[12]</a> <a href="/wiki/Pollux_(star)" title="Pollux (star)">Pollux</a> (apparent magnitude 1.14<a href="#cite_note-14">[13]</a>) has a reported planet (<a href="/wiki/Thestias_(exoplanet)" class="mw-redirect" title="Thestias (exoplanet)">Thestias</a>), but the existence of this planet has been questioned.<a href="#cite_note-Aurière2014-15">[14]</a><a href="#cite_note-Aurière2021-16">[15]</a> Mirfak (<a href="/wiki/Alpha_Persei" title="Alpha Persei">α Per</a>, apparent magnitude 1.806) was claimed to have an orbiting planet, whose existence has likewise been disputed.<a href="#cite_note-mirfak-17">[16]</a> A 2023 study detected 10 luminous point sources around the primary star of <a href="/wiki/Fomalhaut" title="Fomalhaut">Fomalhaut</a> system (apparent magnitude = 1.16), of which the last source may be either an unrelated background object or a planetary-mass companion.<a href="#cite_note-18">[17]</a> </td></tr> <tr> <td>Star with the faintest apparent magnitude with a planet </td> <td><a href="/w/index.php?title=MOA-bin-29Lb&action=edit&redlink=1" class="new" title="MOA-bin-29Lb (page does not exist)">MOA-bin-29Lb</a> </td> <td><a href="/w/index.php?title=MOA-bin-29L&action=edit&redlink=1" class="new" title="MOA-bin-29L (page does not exist)">MOA-bin-29L</a> </td> <td>Apparent magnitude is 44.61<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td> </td></tr> <tr> <td>Star with the highest apparent motion (i.e, <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a>) with a planet </td> <td><a href="/wiki/Barnard%27s_Star#Planetary_system" title="Barnard's Star">Barnard's Star b</a><a href="#cite_note-19">[18]</a> </td> <td><a href="/wiki/Barnard%27s_Star" title="Barnard's Star">Barnard's Star</a> </td> <td>10.358 <a href="/wiki/Minute_and_second_of_arc" title="Minute and second of arc">arcsec</a>/yr<a href="#cite_note-:10-20">[19]</a> </td> <td>As Barnard's Star has the highest apparent motion in the sky,<a href="#cite_note-:10-20">[19]</a> this is currently an absolute record. </td></tr> <tr> <td>Largest <a href="/wiki/Angular_distance" title="Angular distance">angular distance</a> separation from its host star </td> <td><a href="/wiki/COCONUTS-2b" title="COCONUTS-2b">COCONUTS-2b</a> </td> <td><a href="/wiki/COCONUTS-2b#Host_star" title="COCONUTS-2b">COCONUTS-2</a> </td> <td>594 <a href="/wiki/Arcsecond" class="mw-redirect" title="Arcsecond">arcseconds</a><a href="#cite_note-:0-21">[20]</a> </td> <td>A candidate planet or brown dwarf around <a href="/wiki/BD%2B29_5007" title="BD+29 5007">BD+29 5007</a> might have an even larger angular separation of about 935 arcseconds.<a href="#cite_note-Baig2024b-22">[21]</a> </td></tr> <tr> <td>Smallest angular distance separation from its parent star </td> <td><a href="/wiki/SWIFT_J1756.9%E2%88%922508_b" class="mw-redirect" title="SWIFT J1756.9−2508 b">SWIFT J1756.9−2508 b</a> </td> <td><a href="/wiki/SWIFT_J1756.9%E2%88%922508" title="SWIFT J1756.9−2508">SWIFT J1756.9−2508</a> </td> <td>0.34 <a href="/wiki/Microarcsecond" class="mw-redirect" title="Microarcsecond">microarcseconds</a> </td> <td>Derived from its separation of 0.00269 AU and its distance of ~26 000 <a href="/wiki/Light-year" title="Light-year">light-years</a> (8000 pc).<a href="#cite_note-23">[22]</a> </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="Planetary_characteristics">Planetary characteristics</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=2" title="Edit section: Planetary characteristics">edit</a>]</div> <table class="wikitable"> <tbody><tr> <th>Title </th> <th>Planet </th> <th>Star </th> <th>Data </th> <th>Notes </th></tr> <tr> <td> Most massive </td> <td colspan="4">The most massive planet is difficult to define due to the blurry line between planets and <a href="/wiki/Brown_dwarf" title="Brown dwarf">brown dwarfs</a>. If the borderline is defined as the <a href="/wiki/Deuterium_fusion" title="Deuterium fusion">deuterium fusion</a> threshold (roughly 13 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a> at solar <a href="/wiki/Metallicity" title="Metallicity">metallicity</a><a href="#cite_note-24">[23]</a><a href="#cite_note-25">[b]</a>), the most massive planets are those with true mass closest to that cutoff; if planets and brown dwarfs are differentiated based on formation, their mass ranges overlap.<a href="#cite_note-IAUplanetdef-26">[24]</a><a href="#cite_note-Kirkpatrick2024-27">[25]</a>: 62  A candidate for the most massive object that formed in a protoplanetary disk is <a href="/w/index.php?title=HD_206893&action=edit&redlink=1" class="new" title="HD 206893 (page does not exist)">HD 206893 b</a>, at about 28 <var>M</var>J. Both this object and its 13 <var>M</var>J sibling HD 206893 c fuse deuterium.<a href="#cite_note-Hinkley2023-28">[26]</a><a href="#cite_note-Baburaj2024-29">[27]</a> </td></tr> <tr> <td>Least massive </td> <td><a href="/wiki/PSR_B1257%2B12_A" title="PSR B1257+12 A">PSR B1257+12 b</a> (Draugr) </td> <td><a href="/wiki/PSR_B1257%2B12" title="PSR B1257+12">PSR B1257+12</a> (Lich) </td> <td>0.020±0.002 <a href="/wiki/Earth_mass" title="Earth mass">M🜨</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td>The extrasolar <a href="/wiki/Planetesimal" title="Planetesimal">planetesimal</a> <a href="/wiki/WD_1145%2B017_b" title="WD 1145+017 b">WD 1145+017 b</a> is less massive, at 0.00067 <a href="/wiki/Earth_mass" title="Earth mass"><var>M</var>E</a>.<a href="#cite_note-:0-21">[20]</a> A candidate planet at <a href="/wiki/PSR_J0337%2B1715" title="PSR J0337+1715">PSR J0337+1715</a> is even lighter, with half of the Moon's mass or 0.062 <var>M</var>E.<a href="#cite_note-30">[28]</a> </td></tr> <tr> <td><a href="/wiki/List_of_largest_exoplanets" title="List of largest exoplanets">Largest radius</a> </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> Ab </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> </td> <td>2.7±0.8 <a href="/wiki/Jupiter_radius" title="Jupiter radius"><var>R</var>J</a><a href="#cite_note-31">[29]</a> </td> <td>Next largest is PDS 70 b with 2.09+0.23 −0.31 – 2.72+0.15 −0.17 <a href="/wiki/Jupiter_radius" title="Jupiter radius"><var>R</var>J</a>.<a href="#cite_note-Wang2020-32">[30]</a> Proplyd 133-353 is larger at up to 7.4±0.3 – 8.0±1.1 <a href="/wiki/Jupiter_radius" title="Jupiter radius"><var>R</var>J</a>.<a href="#cite_note-Fang2016-33">[31]</a><a href="#cite_note-L/Teff-34">[c]</a> It might be considered as a <a href="/wiki/Sub-brown_dwarf" title="Sub-brown dwarf">sub-brown dwarf</a> or a <a href="/wiki/Rogue_planet" title="Rogue planet">rogue planet</a>, with a <a href="/wiki/Photo_evaporating" class="mw-redirect" title="Photo evaporating">photoevaporating</a> disk. <a href="/wiki/HAT-P-67b" class="mw-redirect" title="HAT-P-67b">HAT-P-67b</a> has the largest accurately and precisely measured radius, at 2.165+0.024 −0.022 <a href="/wiki/Jupiter_radius" title="Jupiter radius">RJ</a>.<a href="#cite_note-Gully-Santiago-35">[32]</a> </td></tr> <tr> <td><a href="/wiki/List_of_smallest_exoplanets" title="List of smallest exoplanets">Smallest radius</a> </td> <td><a href="/wiki/Kepler-37b" title="Kepler-37b">Kepler-37b</a> </td> <td><a href="/wiki/Kepler-37" title="Kepler-37">Kepler-37</a> </td> <td>0.296±0.037 <a href="/wiki/Earth_radius" title="Earth radius">R🜨</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td>The extrasolar <a href="/wiki/Planetesimal" title="Planetesimal">planetesimals</a> <a href="/wiki/SDSS_J1228%2B1040_b" title="SDSS J1228+1040 b">SDSS J1228+1040 b</a><a href="#cite_note-:1-36">[33]</a> and <a href="/wiki/WD_1145%2B017_b" title="WD 1145+017 b">WD 1145+017 b</a> are smaller. </td></tr> <tr> <td>Most dense </td> <td><a href="/wiki/PSR_J1719%E2%88%921438_b" title="PSR J1719−1438 b">PSR J1719−1438 b</a> </td> <td><a href="/wiki/PSR_J1719%E2%88%921438" title="PSR J1719−1438">PSR J1719−1438</a> </td> <td>≥ 23 g/cm3 <a href="#cite_note-37">[34]</a> </td> <td>According to the IAU working definition of <a href="/wiki/Exoplanet" title="Exoplanet">exoplanets</a> <a href="/wiki/PSR_J1719%E2%88%921438_b" title="PSR J1719−1438 b">PSR J1719−1438 b</a>, being slightly more massive than Jupiter, is an exoplanet, despite it possibly formed like a <a href="/wiki/White_dwarf" title="White dwarf">white dwarf</a> from a <a href="/wiki/Yellow_dwarf_star" class="mw-redirect" title="Yellow dwarf star">yellow dwarf star</a> and suffered from the influence of the host star to become a <a href="/wiki/Diamond#In_space" title="Diamond">carbon</a>-rich diamond-like object. For reference, it is about as dense or denser than <a href="/wiki/Osmium" title="Osmium">Osmium</a> at 293 K, the densest naturally occurring element on <a href="/wiki/Earth" title="Earth">Earth</a>. TOI-4603b is the next densest with 14.1+1.7 −1.6 g/cm3,<a href="#cite_note-38">[35]</a> a mass of 12.89+0.58 −0.57 MJ and a radius of 1.042+0.038 −0.035 RJ.<a href="#cite_note-39">[36]</a> <a href="/wiki/KELT-1" title="KELT-1">KELT-1b</a> is similarly dense with 22.1+5.62 −9.16 g/cm3.<a href="#cite_note-:12-40">[37]</a> But, with a mass of 27.23 MJ, it is likely a brown dwarf. <a href="/wiki/Kepler-131c" class="mw-redirect" title="Kepler-131c">Kepler-131c</a> might be more dense at 77.7+55 −55 g/cm3,<a href="#cite_note-41">[38]</a> but the value is highly uncertain. </td></tr> <tr> <td>Least dense </td> <td><a href="/wiki/Kepler-51c" class="mw-redirect" title="Kepler-51c">Kepler-51c</a> and/or possibly <a href="/wiki/Kepler-51d" class="mw-redirect" title="Kepler-51d">d</a> </td> <td><a href="/wiki/Kepler-51" title="Kepler-51">Kepler-51</a><a href="#cite_note-Masuda-42">[39]</a> </td> <td>0.034+0.069 −0.019 g/cm3 <a href="#cite_note-:8-43">[40]</a> </td> <td>The bulk density of Kepler-51 d has been constrained to be 0.038 ± 0.006 g/cm3.<a href="#cite_note-:8-43">[40]</a> Next least dense are the <a href="/wiki/Hot_Saturn" class="mw-redirect" title="Hot Saturn">Hot Saturn</a> <a href="/wiki/HAT-P-67" title="HAT-P-67">HAT-P-67</a> with about 0.044 g/cm3 and the <a href="/wiki/Super-Neptune" title="Super-Neptune">super-Neptune</a> planet <a href="/wiki/WASP-193b" title="WASP-193b">WASP-193b</a>, with 0.059 ± 0.014 g/cm3.<a href="#cite_note-44">[41]</a> </td></tr> <tr> <td>Largest ratio of <a href="/wiki/Exoplanet_orbital_and_physical_parameters#Rotation_and_axial_tilt" title="Exoplanet orbital and physical parameters">rotation rate</a> to breakup velocity </td> <td><a href="/wiki/Kappa_Andromedae_b" title="Kappa Andromedae b">Kappa Andromedae b</a> </td> <td><a href="/wiki/Kappa_Andromedae" title="Kappa Andromedae">Kappa Andromedae</a> </td> <td>~0.5 <a href="#cite_note-45">[42]</a> </td> <td> </td></tr> <tr> <td><a href="/wiki/List_of_hottest_exoplanets" title="List of hottest exoplanets">Hottest</a> (irradiated hot Jupiter) </td> <td><a href="/wiki/KELT-9b" title="KELT-9b">KELT-9b</a> </td> <td><a href="/wiki/KELT-9" class="mw-redirect" title="KELT-9">KELT-9</a> </td> <td>4050 ± 180 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a>(3777 °C) </td> <td>The unconfirmed planets <a href="/wiki/Kepler-70b" class="mw-redirect" title="Kepler-70b">Kepler-70b</a> and <a href="/wiki/Kepler-70c" class="mw-redirect" title="Kepler-70c">Kepler-70c</a> may be hotter, both at >6800 <a href="/wiki/Kelvin" title="Kelvin">K</a> (assuming an albedo of 0.1 for both).<a href="#cite_note-darkest-46">[43]</a> </td></tr> <tr> <td>Hottest (self-luminous) </td> <td><a href="/wiki/GQ_Lupi_b" title="GQ Lupi b">GQ Lupi b</a> </td> <td><a href="/wiki/GQ_Lupi" title="GQ Lupi">GQ Lupi</a> </td> <td>2650 ± 100 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-47">[44]</a>(2377 °C) </td> <td>Depending on its mass value, GQ Lupi b may be either a massive planet or a brown dwarf.<a href="#cite_note-48">[45]</a> </td></tr> <tr> <td><a href="/wiki/List_of_coolest_exoplanets" title="List of coolest exoplanets">Coldest</a> </td> <td> <a href="/wiki/OGLE-2005-BLG-390Lb" title="OGLE-2005-BLG-390Lb">OGLE-2005-BLG-390Lb</a> </td> <td> <a href="/wiki/OGLE-2005-BLG-390L" title="OGLE-2005-BLG-390L">OGLE-2005-BLG-390L</a> </td> <td>50 K (−223.2 °C)<a href="#cite_note-49">[46]</a><a href="#cite_note-50">[d]</a> </td> <td>The disputed planet <a href="/wiki/Proxima_Centauri_c" title="Proxima Centauri c">Proxima Centauri c</a> may be cooler, at 39 K (−234.2 °C).<a href="#cite_note-51">[47]</a> </td></tr> <tr> <td>Highest <a href="/wiki/Albedo" title="Albedo">albedo</a> </td> <td><a href="/wiki/LTT_9779_b" title="LTT 9779 b">LTT 9779 b</a> </td> <td><a href="/wiki/LTT_9779" title="LTT 9779">LTT 9779</a> </td> <td>0.8<a href="#cite_note-52">[48]</a> </td> <td>For comparison, Earth is 0.3 and Venus is 0.76. </td></tr> <tr> <td>Lowest albedo </td> <td><a href="/wiki/TrES-2b" title="TrES-2b">TrES-2b</a> </td> <td><a href="/wiki/GSC_03549-02811" title="GSC 03549-02811">GSC 03549-02811</a> </td> <td><a href="/wiki/Geometric_albedo" title="Geometric albedo">Geometric albedo</a> < 1%<a href="#cite_note-darkest2-53">[49]</a> </td> <td>Best-fit model for albedo gives 0.04% (0.0004).<a href="#cite_note-darkest-46">[43]</a> </td></tr> <tr> <td>Youngest </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> b </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> </td> <td>0.7+0.3 −0.2 <a href="/wiki/Myr" class="mw-redirect" title="Myr">Myr</a><a href="#cite_note-Xuan-2024-54">[50]</a> </td> <td>The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.<a href="#cite_note-:5-55">[51]</a><a href="#cite_note-56">[52]</a> However, as a free-floating planet, it does not meet the <a href="/wiki/International_Astronomical_Union" title="International Astronomical Union">IAU</a>'s working definition of a planet.<a href="#cite_note-:7-57">[53]</a> <a href="/wiki/2MASS_J04414489%2B2301513_b" class="mw-redirect" title="2MASS J04414489+2301513 b">2MASS J04414489+2301513 b</a> is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr,<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> but fails the mass ratio criterion of the <a href="/wiki/IAU" class="mw-redirect" title="IAU">IAU</a> working definition of an exoplanet; the mass ratio with the primary is larger than the <a href="/wiki/Lagrange_point#Stability" title="Lagrange point">L4/L5 limit of stability</a> ≈ 1/25<a href="#cite_note-:7-57">[53]</a> and 'more likely to have been produced by cloud core fragmentation' (like a star).<a href="#cite_note-58">[54]</a> <a href="/wiki/IRAS_04125%2B2902_b" title="IRAS 04125+2902 b">IRAS 04125+2902 b</a> is the youngest <a href="/wiki/Transiting_planet" class="mw-redirect" title="Transiting planet">transiting planet</a> at an age of 3 Myr.<a href="#cite_note-59">[55]</a> <a href="/wiki/CI_Tauri" title="CI Tauri">CI Tauri c</a> would be the youngest <a href="/wiki/Radial_velocity_method" class="mw-redirect" title="Radial velocity method">radial velocity planet</a> at an age of 2–3 Myr, if confirmed.<a href="#cite_note-60">[56]</a> </td></tr> <tr> <td>Oldest </td> <td><a href="/w/index.php?title=TOI-157_b&action=edit&redlink=1" class="new" title="TOI-157 b (page does not exist)">TOI-157 b</a> </td> <td><a href="/w/index.php?title=TOI-157&action=edit&redlink=1" class="new" title="TOI-157 (page does not exist)">TOI-157</a> </td> <td>12.82+0.73 −1.40 <a href="/wiki/Gigayear" class="mw-redirect" title="Gigayear">Gyr</a><a href="#cite_note-61">[57]</a> </td> <td>The currently accepted <a href="/wiki/Age_of_the_universe" title="Age of the universe">age of the universe</a> is around 13.8 billion years. Could alternatively be <a href="/wiki/PSR_B1620%E2%88%9226_b" title="PSR B1620−26 b">PSR B1620-26 b</a> with 11.2–12.7 <a href="/wiki/Gigayear" class="mw-redirect" title="Gigayear">Gyr</a>.<a href="#cite_note-62">[58]</a> </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="Orbital_characteristics">Orbital characteristics</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=3" title="Edit section: Orbital characteristics">edit</a>]</div> <table class="wikitable" style="text-align:left;"> <tbody><tr> <th style="background:#efefef;">Title </th> <th style="background:#efefef;">Planet </th> <th style="background:#efefef;">Star </th> <th style="background:#efefef;">Data </th> <th style="background:#efefef;">Notes </th></tr> <tr> <td>Longest <a href="/wiki/Orbital_period" title="Orbital period">orbital period</a> (Longest year) </td> <td><a href="/wiki/Gliese_900_b" class="mw-redirect" title="Gliese 900 b">Gliese 900 b</a> (CW2335+0142) </td> <td><a href="/wiki/Gliese_900" title="Gliese 900">Gliese 900</a> </td> <td>1.27 million years<a href="#cite_note-63">[59]</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a><a href="#cite_note-64">[e]</a> </td> <td><a href="/wiki/COCONUTS-2b" title="COCONUTS-2b">COCONUTS-2b</a> previously held this record at 1,100,000 years. </td></tr> <tr> <td>Shortest orbital period (Shortest year) </td> <td><a href="/w/index.php?title=SDSS_J1730%2B5545_b&action=edit&redlink=1" class="new" title="SDSS J1730+5545 b (page does not exist)">SDSS J1730+5545 b</a> </td> <td><a href="/w/index.php?title=SDSS_J1730%2B5545&action=edit&redlink=1" class="new" title="SDSS J1730+5545 (page does not exist)">SDSS J1730+5545</a> </td> <td>0.5866 h (35 minutes)<a href="#cite_note-SDSS_J1730+5545-65">[60]</a> </td> <td><a href="/w/index.php?title=K2-137b&action=edit&redlink=1" class="new" title="K2-137b (page does not exist)">K2-137b</a> has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.<a href="#cite_note-66">[61]</a> </td></tr> <tr> <td>Largest orbital separation </td> <td><a href="/wiki/Gliese_900_b" class="mw-redirect" title="Gliese 900 b">Gliese 900 b</a> (CW2335+0142) </td> <td><a href="/wiki/Gliese_900" title="Gliese 900">Gliese 900</a> </td> <td>12 000 <a href="/wiki/Astronomical_unit" title="Astronomical unit">AU</a><a href="#cite_note-:6-67">[62]</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td>UCAC4 328-061594 b has an even longer orbital separation (19 000 <a href="/wiki/Astronomical_unit" title="Astronomical unit">AU</a>), although its mass (21 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>) <a href="#cite_note-NASAExoplanetArchive-8">[8]</a><a href="#cite_note-:6-67">[62]</a> is higher than the deuterium burning limit (13 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>). Another candidate around <a href="/wiki/BD%2B29_5007" title="BD+29 5007">BD+29 5007</a> has an even larger orbit of about 22 100 <a href="/wiki/Astronomical_unit" title="Astronomical unit">AU</a>. There is no consensus about its age and resulting mass, and it could be a field brown dwarf. The companion of <a href="/w/index.php?title=ASASSN-21js&action=edit&redlink=1" class="new" title="ASASSN-21js (page does not exist)">ASASSN-21js</a> has an orbit of 13 000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass.<a href="#cite_note-68">[63]</a> </td></tr> <tr> <td>Smallest orbital separation </td> <td><a href="/w/index.php?title=SDSS_J1730%2B5545_b&action=edit&redlink=1" class="new" title="SDSS J1730+5545 b (page does not exist)">SDSS J1730+5545 b</a> </td> <td><a href="/w/index.php?title=SDSS_J1730%2B5545&action=edit&redlink=1" class="new" title="SDSS J1730+5545 (page does not exist)">SDSS J1730+5545</a> </td> <td>0.00139 <a href="/wiki/Astronomical_unit" title="Astronomical unit">AU</a><a href="#cite_note-SDSS_J1730+5545-65">[60]</a> </td> <td> </td></tr> <tr> <td>Most <a href="/wiki/Orbital_eccentricity" title="Orbital eccentricity">eccentric orbit</a> </td> <td><a href="/wiki/SGR_1935%2B2154#Planetary_system" title="SGR 1935+2154">SGR 1935+2154 b</a> </td> <td><a href="/wiki/SGR_1935%2B2154" title="SGR 1935+2154">SGR 1935+2154</a> </td> <td>0.992 or 0.994 </td> <td><a href="#cite_note-Kurban2024-4">[4]</a> </td></tr> <tr> <td>Highest <a href="/wiki/Orbital_inclination" title="Orbital inclination">orbital inclination</a> </td> <td><a href="/wiki/HD_204313#Planetary_system" title="HD 204313">HD 204313 e</a> </td> <td><a href="/wiki/HD_204313" title="HD 204313">HD 204313</a> </td> <td>176.092<a href="/wiki/Degree_(angle)" title="Degree (angle)">°</a>+0.963<a href="/wiki/Degree_(angle)" title="Degree (angle)">°</a> −2.122<a href="/wiki/Degree_(angle)" title="Degree (angle)">°</a> </td> <td><a href="#cite_note-69">[64]</a><a href="#cite_note-:3-70">[65]</a> </td></tr> <tr> <td>Lowest orbital inclination </td> <td><a href="/w/index.php?title=HD_331093_b&action=edit&redlink=1" class="new" title="HD 331093 b (page does not exist)">HD 331093 b</a> </td> <td><a href="/w/index.php?title=HD_331093&action=edit&redlink=1" class="new" title="HD 331093 (page does not exist)">HD 331093</a> </td> <td>>0.3704° </td> <td><a href="#cite_note-71">[66]</a><a href="#cite_note-:3-70">[65]</a> <a href="/wiki/HD_43197" title="HD 43197">HD 43197 c</a> has the lowest orbital inclination that is not a <a href="/wiki/Lower_limit" class="mw-redirect" title="Lower limit">lower limit</a>, of 11.42°+5.388° −3.07°.<a href="#cite_note-:3-70">[65]</a> </td></tr> <tr> <td>Largest orbit around a single star </td> <td><a href="/wiki/COCONUTS-2b" title="COCONUTS-2b">COCONUTS-2b</a> </td> <td><a href="/wiki/L_34-26" class="mw-redirect" title="L 34-26">L 34-26</a> </td> <td>7506 AU </td> <td>Next largest are <a href="/wiki/2MASS_J2126%E2%80%938140" title="2MASS J2126–8140">2MASS J2126–8140</a> with 6900 AU and <a href="/wiki/HD_106906_b" title="HD 106906 b">HD 106906 b</a><a href="#cite_note-HD106906b-72">[67]</a> with ~738 AU. UCAC4 328-061594 b has an even longer orbital separation (19,000 AU), although its mass (21 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>)<a href="#cite_note-NASAExoplanetArchive-8">[8]</a><a href="#cite_note-:6-67">[62]</a> is higher than the deuterium burning limit (13 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>). </td></tr> <tr> <td>Smallest orbit around binary star </td> <td><a href="/wiki/Kepler-47b" title="Kepler-47b">Kepler-47b</a> </td> <td><a href="/wiki/Kepler-47" title="Kepler-47">Kepler-47</a>AB </td> <td>0.2877+0.0014 −0.0011 AU<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td><a href="#cite_note-73">[68]</a> </td></tr> <tr> <td>Smallest ratio of <a href="/wiki/Semi-major_axis" class="mw-redirect" title="Semi-major axis">semi-major axis</a> of a planet orbit to binary star orbit </td> <td><a href="/wiki/Kepler-16b" title="Kepler-16b">Kepler-16b</a> </td> <td><a href="/wiki/Kepler-16" title="Kepler-16">Kepler-16</a>AB </td> <td>3.14 ± 0.01 </td> <td><a href="#cite_note-kepler16b-74">[69]</a> </td></tr> <tr> <td>Largest orbit around binary star </td> <td><a href="/w/index.php?title=SR_12_(AB)_c&action=edit&redlink=1" class="new" title="SR 12 (AB) c (page does not exist)">SR 12 (AB) c</a> </td> <td><a href="/w/index.php?title=SR_12_AB&action=edit&redlink=1" class="new" title="SR 12 AB (page does not exist)">SR 12 AB</a> </td> <td>≈1100 AU<a href="#cite_note-:2-75">[70]</a> </td> <td><a href="/w/index.php?title=SR_12_(AB)_c&action=edit&redlink=1" class="new" title="SR 12 (AB) c (page does not exist)">SR 12 (AB) c</a> has a mass of 0.013±0.007 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a>.<a href="#cite_note-:2-75">[70]</a> <a href="/wiki/ROXs_42Bb" title="ROXs 42Bb">ROXs 42B (AB) b</a> is lower in mass at 9.0+6 −3 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>, however also in projected separation of ≈150 AU.<a href="#cite_note-Currie2013-76">[71]</a> <a href="/wiki/DT_Virginis_c" class="mw-redirect" title="DT Virginis c">DT Virginis c</a>, also known as Ross 458 (AB) c, at a projected separation of ≈1200 AU, with several mass estimates below the <a href="/wiki/Deuterium" title="Deuterium">deuterium</a> burning limit, has a latest mass determination of 27±4 <var>M</var>J.<a href="#cite_note-77">[72]</a> </td></tr> <tr> <td>Largest orbit around a single star in a multiple star system </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> b </td> <td><a href="/wiki/DH_Tauri" title="DH Tauri">DH Tauri</a> </td> <td>330 AU<a href="#cite_note-78">[73]</a> </td> <td> </td></tr> <tr> <td>Largest separation between binary stars with a circumbinary planet </td> <td><a href="/w/index.php?title=FW_Tauri_b&action=edit&redlink=1" class="new" title="FW Tauri b (page does not exist)">SR 12 (AB) c</a> </td> <td><a href="/w/index.php?title=FW_Tauri&action=edit&redlink=1" class="new" title="FW Tauri (page does not exist)">SR 12 AB</a> </td> <td>≈26 AU<a href="#cite_note-:2-75">[70]</a> </td> <td><a href="/w/index.php?title=SR_12_(AB)_c&action=edit&redlink=1" class="new" title="SR 12 (AB) c (page does not exist)">SR 12 (AB) c</a> has a mass of 0.013±0.007 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a> at a projected separation of ≈1100 AU.<a href="#cite_note-:2-75">[70]</a> <a href="/w/index.php?title=FW_Tauri_b&action=edit&redlink=1" class="new" title="FW Tauri b (page does not exist)">FW Tauri b</a> orbits at a projected separation of 330±30 <a href="/wiki/Astronomical_unit" title="Astronomical unit">AU</a> around a ≈11 AU separated binary.<a href="#cite_note-79">[74]</a> It was shown to be more likely a 0.1 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a> star surrounded by a protoplanetary disk than a planetary-mass companion.<a href="#cite_note-80">[75]</a> </td></tr> <tr> <td>Largest orbit around three stars </td> <td><a href="/wiki/Gliese_900_b" class="mw-redirect" title="Gliese 900 b">Gliese 900 b</a> (CW2335+0142) </td> <td><a href="/wiki/Gliese_900" title="Gliese 900">Gliese 900</a> </td> <td>12 000 AU<a href="#cite_note-:6-67">[62]</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td> </td></tr> <tr> <td>Closest orbit between stars with a planet orbiting one of the stars (<a href="/wiki/Habitability_of_binary_star_systems#Non-circumbinary_planet_(S-Type)" title="Habitability of binary star systems">S-type planet</a>) </td> <td><a href="/wiki/HD_42936#Planetary_system" title="HD 42936">DMPP-3 Ab</a> </td> <td><a href="/wiki/HD_42936" title="HD 42936">HD 42936</a> </td> <td>1.139 AU<a href="#cite_note-81">[76]</a><a href="#cite_note-82">[77]</a> </td> <td>DMPP-3 Ab's semi-major axis is around 0.067 AU. The next closest orbit between stars with an S-type planet occurs in <a href="/wiki/Nu_Octantis" title="Nu Octantis">Nu Octantis</a> system, of which the separation between the stellar components is 2.629 AU.<a href="#cite_note-83">[78]</a> </td></tr> <tr> <td>Smallest semi-major axis ratio between consecutive planets </td> <td><a href="/wiki/Kepler-36b" title="Kepler-36b">Kepler-36b</a> and <a href="/wiki/Kepler-36c" class="mw-redirect" title="Kepler-36c">Kepler-36c</a> </td> <td><a href="/wiki/Kepler-36" title="Kepler-36">Kepler-36</a> </td> <td>1.11 </td> <td>Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively; hence the planet c is 1.11 times further from star than b. </td></tr> <tr> <td>Largest semi-major axis ratio between consecutive planets </td> <td><a href="/wiki/HD_83443_b" title="HD 83443 b">HD 83443 b</a> and <a href="/wiki/HD_83443#Planetary_system" title="HD 83443">HD 83443 c</a> </td> <td><a href="/wiki/HD_83443" title="HD 83443">HD 83443</a> </td> <td>205.1 </td> <td>HD 83443 b and c have semi-major axes of 0.039 AU and 8.0 AU,<a href="#cite_note-Errico2022-84">[79]</a> respectively; hence the planet c is 205.1 times further from star than b. </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="Stellar_characteristics">Stellar characteristics</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=4" title="Edit section: Stellar characteristics">edit</a>]</div> <table class="wikitable" style="text-align:left;"> <tbody><tr> <th style="background:#efefef;">Title </th> <th style="background:#efefef;">Planet </th> <th style="background:#efefef;">Star </th> <th style="background:#efefef;">Data </th> <th style="background:#efefef;">Notes </th></tr> <tr> <td>Highest <a href="/wiki/Metallicity" title="Metallicity">metallicity</a> </td> <td><a href="/wiki/HD_126614_Ab" title="HD 126614 Ab">HD 126614 Ab</a> </td> <td><a href="/wiki/HD_126614" title="HD 126614">HD 126614</a> A </td> <td>+0.56 <a href="/wiki/Metallicity#Chemical_abundance_ratios" title="Metallicity">dex</a> </td> <td>Located in a triple star system. </td></tr> <tr> <td>Lowest metallicity </td> <td><a href="/w/index.php?title=K2-344b&action=edit&redlink=1" class="new" title="K2-344b (page does not exist)">K2-344b</a> </td> <td><a href="/w/index.php?title=K2-344&action=edit&redlink=1" class="new" title="K2-344 (page does not exist)">K2-344</a> </td> <td>−0.95±0.02 <a href="/wiki/Metallicity#Chemical_abundance_ratios" title="Metallicity">dex</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td><a href="/wiki/BD%2B20%C2%B02457" class="mw-redirect" title="BD+20°2457">BD+20°2457</a> may be the lowest-metallicity planet host ([Fe/H]=−1.00); however, the proposed planetary system is dynamically unstable.<a href="#cite_note-Horner-85">[80]</a> Planets were announced around even the extremely low-metallicity stars <a href="/wiki/HIP_13044" title="HIP 13044">HIP 13044</a> and <a href="/wiki/HIP_11952" title="HIP 11952">HIP 11952</a>; however, these claims have since been disproven.<a href="#cite_note-86">[81]</a> A brown dwarf or massive planetary companion was announced around the population II star <a href="/wiki/HE_1523-0901" title="HE 1523-0901">HE 1523-0901</a>, whose metallicity is −2.65±0.22 dex.<a href="#cite_note-reggiani2022-87">[82]</a> While the inclination of the companion is not known, if its orbit is nearly face-on, it would be sufficiently massive to become a <a href="/wiki/Red_dwarf" title="Red dwarf">red dwarf</a> instead.<a href="#cite_note-88">[83]</a> </td></tr> <tr> <td>Highest stellar mass </td> <td><a href="/wiki/B_Centauri_b" title="B Centauri b">b Centauri b</a> </td> <td><a href="/wiki/HD_129116" title="HD 129116">b Centauri</a> </td> <td>5 - 6 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a> </td> <td><a href="/wiki/Mu2_Scorpii" title="Mu2 Scorpii">Pipirima</a> has a higher mass of 9.1±0.3 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a>,<a href="#cite_note-89">[84]</a> but its planet candidate <a href="/wiki/Mu2_Scorpii_b" class="mw-redirect" title="Mu2 Scorpii b">Mu2 Scorpii b</a> is most likely a brown dwarf having 14.4 ± 0.8 <a href="/wiki/Jupiter_mass" title="Jupiter mass">MJ</a>. The candidate planet <a href="/wiki/M51-ULS-1b" class="mw-redirect" title="M51-ULS-1b">M51-ULS-1b</a> and the candidate <a href="/wiki/Planetary-mass_object" title="Planetary-mass object">planemo</a> IGR J12580+0134 b might be the <a href="/wiki/Blanets" class="mw-redirect" title="Blanets">blanets</a>, whose hosts have masses of ≫10 and 9 150 000 Solar masses, respectively.<a href="#cite_note-90">[85]</a><a href="#cite_note-91">[86]</a> The stars R126 (<a href="/wiki/HD_37974" title="HD 37974">HD 37974</a>), R66 (<a href="/wiki/HD_268835" title="HD 268835">HD 268835</a>) and <a href="/w/index.php?title=HH_1177&action=edit&redlink=1" class="new" title="HH 1177 (page does not exist)">HH 1177</a> in the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> have masses of 70, 30 and 15 solar masses and have dust discs<a href="#cite_note-92">[87]</a> but no planets have been detected yet. </td></tr> <tr> <td>Lowest stellar mass (main sequence) </td> <td><a href="/w/index.php?title=KMT-2021-BLG-1554Lb&action=edit&redlink=1" class="new" title="KMT-2021-BLG-1554Lb (page does not exist)">KMT-2021-BLG-1554Lb</a> </td> <td><a href="/w/index.php?title=KMT-2021-BLG-1554L&action=edit&redlink=1" class="new" title="KMT-2021-BLG-1554L (page does not exist)">KMT-2021-BLG-1554L</a> </td> <td>0.08+0.013 −0.014 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a><a href="#cite_note-:3-70">[65]</a> </td> <td>The mass of this star is near the <a href="/wiki/Hydrogen_burning_limit" class="mw-redirect" title="Hydrogen burning limit">hydrogen burning limit</a>. <a href="/w/index.php?title=KMT-2016-BLG-2142L&action=edit&redlink=1" class="new" title="KMT-2016-BLG-2142L (page does not exist)">KMT-2016-BLG-2142L</a> has a lower mass of 0.073+0.117 −0.04 <a href="/wiki/Solar_mass" title="Solar mass">M☉</a>, but the value is highly uncertain.<a href="#cite_note-:3-70">[65]</a> </td></tr> <tr> <td>Largest stellar radius </td> <td><a href="/wiki/HD_208527" title="HD 208527">HD 208527 b</a> </td> <td><a href="/wiki/HD_208527" title="HD 208527">HD 208527</a> </td> <td>51.1±8.3 <a href="/wiki/Solar_radius" title="Solar radius">R☉</a><a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td> <td>Other stars, such as <a href="/wiki/HD_18438" title="HD 18438">HD 18438</a>, <a href="/wiki/Mirach" title="Mirach">Mirach</a> and <a href="/wiki/Delta_Virginis" title="Delta Virginis">Delta Virginis</a> are larger, but their substellar companions are more massive than the deuterium burning limit (13 <a href="/wiki/Jupiter_mass" title="Jupiter mass"><var>M</var>J</a>), and thus might be brown dwarfs rather than exoplanets.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> <a href="/wiki/R_Leonis" title="R Leonis">R Leonis</a> (320-350 <var>R</var>☉)<a href="#cite_note-Fedele_et_al.-93">[88]</a> has a candidate planet. <a href="/wiki/R_Fornacis" title="R Fornacis">R Fornacis</a> at 585 <var>R</var>☉<a href="#cite_note-94">[f]</a> also has a planet candidate.<a href="#cite_note-Paladini_et_al.-95">[89]</a><a href="#cite_note-96">[90]</a> The stars R126 and R66 in the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> have radius of 78 <var>R</var>☉ and 131 <var>R</var>☉<a href="#cite_note-kastner-97">[91]</a> and have dust discs but no planets have been detected yet. </td></tr> <tr> <td>Smallest stellar radius (main sequence star) </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> planets </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> </td> <td>0.1192±0.0013 <a href="/wiki/Solar_radius" title="Solar radius">R☉</a><a href="#cite_note-98">[92]</a> </td> <td><a href="/wiki/VB_10" title="VB 10">VB 10</a> (0.102 <var>R</var>☉)<a href="#cite_note-99">[93]</a> has a disproven planet candidate. </td></tr> <tr> <td>Smallest stellar radius (stellar remnant) </td> <td><a href="/wiki/SGR_1935%2B2154#Planetary_system" title="SGR 1935+2154">SGR 1935+2154 b</a> </td> <td><a href="/wiki/SGR_1935%2B2154" title="SGR 1935+2154">SGR 1935+2154</a> </td> <td>4.35 km (6.25×10−6 R☉) </td> <td><a href="#cite_note-Shao2024-3">[3]</a> <a href="/wiki/PSR_B0943%2B10" title="PSR B0943+10">PSR B0943+10</a> may be a <a href="/wiki/Quark_star" title="Quark star">quark star</a>. If so, its radius is predicted to be 2.6 km. If a normal neutron star, its radius is 10 km.<a href="#cite_note-:4-100">[94]</a> </td></tr> <tr> <td>Highest <a href="/wiki/Stellar_luminosity" class="mw-redirect" title="Stellar luminosity">stellar luminosity</a> </td> <td><a href="/wiki/Beta_Cancri_b" title="Beta Cancri b">Beta Cancri b</a> </td> <td><a href="/wiki/Beta_Cancri" title="Beta Cancri">Beta Cancri</a> </td> <td>794 <a href="/wiki/Solar_luminosity" title="Solar luminosity">L☉</a><a href="#cite_note-:3-70">[65]</a> </td> <td>This is the most luminous star to host a planet that is not a potential brown dwarf.<a href="#cite_note-:3-70">[65]</a> The star Mirfak, whose luminosity is 3780 L☉,<a href="#cite_note-McDonald-101">[95]</a> was claimed to have an orbiting planet with a minimum mass of 6.6 ± 0.2 Jupiter masses. However, the existence of the planet is doubtful.<a href="#cite_note-mirfak-17">[16]</a> R Leonis (at 3537 L☉)<a href="#cite_note-Fedele_et_al.-93">[88]</a> has a candidate planet. R Fornacis (at 5800 L☉)<a href="#cite_note-Paladini_et_al.-95">[89]</a> also has a candidate planet. The bright giant BD+20°2457 (at 1479 L☉<a href="#cite_note-102">[96]</a>) was believed to have two planetary-mass companions orbiting although the claimed system configuration is dynamically unstable.<a href="#cite_note-Horner-85">[80]</a> The stars R126 and R66 in the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> have luminosities of 1400000 L☉ and 320000 L☉<a href="#cite_note-kastner-97">[91]</a> and have dust discs but no planets have been detected yet. </td></tr> <tr> <td>Lowest stellar luminosity (main sequence star) </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> planets </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> </td> <td>0.0005495 L☉ </td> <td><a href="#cite_note-103">[97]</a><a href="#cite_note-:3-70">[65]</a> </td></tr> <tr> <td>Hottest star with a planet </td> <td><a href="/wiki/PSR_B0943%2B10" title="PSR B0943+10">PSR B0943+10 b and c</a> </td> <td><a href="/wiki/PSR_B0943%2B10" title="PSR B0943+10">PSR B0943+10</a> </td> <td>3 100 000 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-:9-104">[98]</a> </td> <td><a href="/wiki/Blackbody_temperature" class="mw-redirect" title="Blackbody temperature">Blackbody temperature</a> of a small emitting area at the poles.<a href="#cite_note-:9-104">[98]</a> Suggested to actually be a low-mass <a href="/wiki/Quark_star" title="Quark star">quark star</a>. </td></tr> <tr> <td>Hottest non-<a href="/wiki/Compact_object" title="Compact object">degenerate</a> star with a planet </td> <td><a href="/wiki/NSVS_14256825" title="NSVS 14256825">NSVS 14256825 b</a> </td> <td><a href="/wiki/NSVS_14256825" title="NSVS 14256825">NSVS 14256825</a> </td> <td>40 000 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-105">[99]</a> </td> <td><a href="/wiki/NN_Serpentis" title="NN Serpentis">NN Serpentis</a> is hotter, with a temperature of 57 000 K,<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> but the existence of its planets is disputed.<a href="#cite_note-106">[100]</a> </td></tr> <tr> <td>Hottest normal star with a planet<a href="#cite_note-107">[g]</a> </td> <td><a href="/wiki/B_Centauri_b" title="B Centauri b">b Centauri b</a> </td> <td><a href="/wiki/HD_129116" title="HD 129116">b Centauri</a> </td> <td>18 310 ± 320 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-108">[101]</a> </td> <td><a href="/wiki/V921_Scorpii_b" title="V921 Scorpii b">V921 Scorpii b</a> orbits a hotter star, at 30,000 K. Its host star is a 20-solar-mass B0IV-class subgiant.<a href="#cite_note-V921Sco-109">[102]</a> However, at 60 Jupiter masses, it is not considered a planet under most definitions. The candidate planet <a href="/wiki/M51-ULS-1b" class="mw-redirect" title="M51-ULS-1b">M51-ULS-1b</a>'s supergiant primary is an O5-class supergiant with an estimated surface temperature of 40,000 K. </td></tr> <tr> <td>Coolest star with a planet </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> planets </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> </td> <td>2511 K </td> <td>Technically <a href="/wiki/Oph_162225-240515" title="Oph 162225-240515">Oph 162225-240515</a>, <a href="/wiki/CFBDSIR_1458%2B10" class="mw-redirect" title="CFBDSIR 1458+10">CFBDSIR 1458+10</a> and <a href="/wiki/WISE_1217%2B1626" title="WISE 1217+1626">WISE 1217+1626</a> are cooler, but are classified as brown dwarfs. </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="System_characteristics">System characteristics</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=5" title="Edit section: System characteristics">edit</a>]</div> <table class="wikitable"> <tbody><tr> <th>Title </th> <th>System(s) </th> <th>Planet(s) </th> <th>Star(s) </th> <th>Notes </th></tr> <tr> <td>System with most planets </td> <td><a href="/wiki/Kepler-90" title="Kepler-90">Kepler-90</a> </td> <td>8 </td> <td>1 </td> <td><a href="/wiki/Tau_Ceti" title="Tau Ceti">Tau Ceti</a> currently has no confirmed planetary companion, although it has been proposed that the number of orbiting planets may be 8, 9 or even 10.<a href="#cite_note-Dietrich_Apai_2020-110">[103]</a> The four planets <a href="/wiki/Tau_Ceti_e" title="Tau Ceti e">Tau Ceti e</a>, <a href="/wiki/Tau_Ceti_f" title="Tau Ceti f">f</a>, g and h are considered as strong candidates.<a href="#cite_note-111">[104]</a> <a href="/wiki/HD_10180" title="HD 10180">HD 10180</a> has six confirmed planets and potentially three more planets.<a href="#cite_note-112">[105]</a> </td></tr> <tr> <td>System with most planets in habitable zone </td> <td><a href="/wiki/TRAPPIST-1" title="TRAPPIST-1">TRAPPIST-1</a> </td> <td>7 </td> <td>1 </td> <td>Four planets in this system (d, e, f and g) orbit within the <a href="/wiki/Habitable_zone" title="Habitable zone">habitable zone</a>.<a href="#cite_note-113">[106]</a> </td></tr> <tr> <td>System with most stars </td> <td><a href="/wiki/Kepler-64" class="mw-redirect" title="Kepler-64">Kepler-64</a> </td> <td><a href="/wiki/PH1b" title="PH1b">PH1b</a> (Kepler-64b) </td> <td>4 </td> <td>PH1b has a circumbinary orbit. <a href="/wiki/30_Arietis" title="30 Arietis">30 Arietis Bb</a> was believed to be either brown dwarf or a massive gas giant in a quadruple star system until later studies revealed a true mass well above 80 <a href="/wiki/Jupiter_mass" title="Jupiter mass">MJup</a>.<a href="#cite_note-Kiefer2020-114">[107]</a> The quintuple star system <a href="/wiki/GG_Tauri" title="GG Tauri">GG Tauri</a> has several protoplanetary disks but no planets have been detected yet.<a href="#cite_note-115">[108]</a> </td></tr> <tr> <td>Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star) </td> <td><a href="/wiki/Kepler-42" title="Kepler-42">Kepler-42</a> </td> <td><a href="/wiki/Kepler-42b" class="mw-redirect" title="Kepler-42b">b</a>, <a href="/wiki/Kepler-42c" title="Kepler-42c">c</a>, <a href="/wiki/Kepler-42d" class="mw-redirect" title="Kepler-42d">d</a> </td> <td>1 </td> <td>Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively. Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. </td></tr> <tr> <td>Multiplanetary system with largest mean semi-major axis (planets are farthest from their star) </td> <td><a href="/wiki/TYC_8998-760-1" title="TYC 8998-760-1">TYC 8998-760-1</a> </td> <td><a href="/wiki/TYC_8998-760-1_b" class="mw-redirect" title="TYC 8998-760-1 b">b</a>, <a href="/wiki/TYC_8998-760-1_c" class="mw-redirect" title="TYC 8998-760-1 c">c</a> </td> <td>1 </td> <td>TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> </td></tr> <tr> <td>Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet) </td> <td><a href="/wiki/Kepler-429" title="Kepler-429">Kepler-429</a> </td> <td><a href="/w/index.php?title=Kepler-429b&action=edit&redlink=1" class="new" title="Kepler-429b (page does not exist)">b</a>, <a href="/w/index.php?title=Kepler-429c&action=edit&redlink=1" class="new" title="Kepler-429c (page does not exist)">c</a>, <a href="/wiki/Kepler-429d" class="mw-redirect" title="Kepler-429d">d</a> </td> <td>1 </td> <td>Kepler-429 b, c and d have a semi-major axis of only 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is only 0.0094 AU. Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. The separation between closest and furthest is only 0.0016 AU (239,356 km). </td></tr> <tr> <td>Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet) </td> <td><a href="/wiki/TYC_8998-760-1" title="TYC 8998-760-1">TYC 8998-760-1</a> </td> <td><a href="/wiki/TYC_8998-760-1_b" class="mw-redirect" title="TYC 8998-760-1 b">b</a>, <a href="/wiki/TYC_8998-760-1_c" class="mw-redirect" title="TYC 8998-760-1 c">c</a> </td> <td>1 </td> <td>TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> The separation between closest and furthest is 158 AU. </td></tr> <tr> <td>System with smallest total planetary mass </td> <td><a href="/wiki/Kepler-444" title="Kepler-444">Kepler-444</a> </td> <td>b, c, d, e, f </td> <td>3 </td> <td>The planets in the <a href="/wiki/Kepler-444" title="Kepler-444">Kepler-444</a> system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of <a href="/wiki/Mars" title="Mars">Mars</a>. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii. </td></tr> <tr> <td>System with largest total planetary mass </td> <td><a href="/wiki/HR_8799" title="HR 8799">HR 8799</a> </td> <td>b, c, d, e </td> <td>1 </td> <td>Four planets having > 5 Jupiter masses each. <a href="/wiki/Nu_Ophiuchi" title="Nu Ophiuchi">Nu Ophiuchi</a> b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> They are likely brown dwarfs. </td></tr> <tr> <td>Multiplanetary system with smallest mean planetary mass </td> <td><a href="/wiki/Kepler-444" title="Kepler-444">Kepler-444</a> </td> <td>b, c, d, e, f </td> <td>3 </td> <td>The planets in the <a href="/wiki/Kepler-444" title="Kepler-444">Kepler-444</a> system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of <a href="/wiki/Mars" title="Mars">Mars</a>. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii. </td></tr> <tr> <td>Multiplanetary system with largest mean planetary mass </td> <td><a href="/wiki/HR_8799" title="HR 8799">HR 8799</a> </td> <td>b, c, d, e </td> <td>1 </td> <td>Four planets having > 5 Jupiter masses each. <a href="/wiki/Nu_Ophiuchi" title="Nu Ophiuchi">Nu Ophiuchi</a> b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively.<a href="#cite_note-NASAExoplanetArchive-8">[8]</a> They are likely brown dwarfs. </td></tr> <tr> <td>Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets) </td> <td><a href="/wiki/Teegarden%27s_Star" title="Teegarden's Star">Teegarden's Star</a> </td> <td>b, c </td> <td>1 </td> <td><a href="/wiki/Teegarden_b" class="mw-redirect" title="Teegarden b">Teegarden b</a> and <a href="/wiki/Teegarden_c" class="mw-redirect" title="Teegarden c">c</a> are estimated to have masses of 1.05 and 1.11 Earth masses, respectively. </td></tr> <tr> <td>Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets) </td> <td><a href="/wiki/Kepler-37" title="Kepler-37">Kepler-37</a> </td> <td><a href="/wiki/Kepler-37b" title="Kepler-37b">b</a>, <a href="/wiki/Kepler-37d" title="Kepler-37d">d</a> </td> <td>1 </td> <td><a href="/wiki/Mercury_(planet)" title="Mercury (planet)">Mercury</a> and <a href="/wiki/Jupiter" title="Jupiter">Jupiter</a> have a mass ratio of 5750 to 1. <a href="/wiki/Kepler-37" title="Kepler-37">Kepler-37</a> d and b may have a mass ratio between 500 and 1000, and <a href="/wiki/Gliese_676" title="Gliese 676">Gliese 676</a> c and d have a mass ratio of 491. </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=6" title="Edit section: See also">edit</a>]</div> <ul><li><a href="/wiki/Extremes_on_Earth" title="Extremes on Earth">Extremes on Earth</a></li> <li><a href="/wiki/Lists_of_exoplanets" class="mw-redirect" title="Lists of exoplanets">Lists of exoplanets</a></li> <li><a href="/wiki/List_of_exoplanet_firsts" title="List of exoplanet firsts">List of exoplanet firsts</a></li> <li><a href="/wiki/List_of_stars_with_proplyds" title="List of stars with proplyds">List of stars with proplyds</a></li> <li><a href="/wiki/Methods_of_detecting_exoplanets" title="Methods of detecting exoplanets">Methods of detecting exoplanets</a></li> <li><a href="/wiki/List_of_potentially_habitable_exoplanets" title="List of potentially habitable exoplanets">List of potentially habitable exoplanets</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="Notes_and_references">Notes and references</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=7" title="Edit section: Notes and references">edit</a>]</div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist"> <div 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Exoplanet Exploration: Planets Beyond our Solar System. nasa.gov. 21 February 2017. Retrieved 14 December 2017.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Exoplanet+Exploration%3A+Planets+Beyond+our+Solar+System&rft.atitle=NASA+telescope+reveals+largest+batch+of+Earth-size%2C+habitable-zone+planets+around+single+star&rft.date=2017-02-21&rft_id=https%3A%2F%2Fexoplanets.nasa.gov%2Fnews%2F1419%2Fnasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star%2F&rfr_id=info%3Asid%2Fen.wikipedia.org%3AList+of+exoplanet+extremes" class="Z3988"> </li> <li id="cite_note-Kiefer2020-114"><a href="#cite_ref-Kiefer2020_114-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKieferHébrardLecavelier_des_EtangsMartioli2021" class="citation journal cs1">Kiefer, F.; et al. (January 2021). <a rel="nofollow" class="external text" href="https://doi.org/10.1051%2F0004-6361%2F202039168">"Determining the true mass of radial-velocity exoplanets with Gaia. Nine planet candidates in the brown dwarf or stellar regime and 27 confirmed planets"</a>. Astronomy & Astrophysics. 645 A7. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/2009.14164">2009.14164</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2021A&A...645A...7K">2021A&A...645A...7K</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1051%2F0004-6361%2F202039168">10.1051/0004-6361/202039168</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:221995447">221995447</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astronomy+%26+Astrophysics&rft.atitle=Determining+the+true+mass+of+radial-velocity+exoplanets+with+Gaia.+Nine+planet+candidates+in+the+brown+dwarf+or+stellar+regime+and+27+confirmed+planets&rft.volume=645&rft.artnum=A7&rft.date=2021-01&rft_id=info%3Aarxiv%2F2009.14164&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A221995447%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1051%2F0004-6361%2F202039168&rft_id=info%3Abibcode%2F2021A%26A...645A...7K&rft.aulast=Kiefer&rft.aufirst=F.&rft.au=H%C3%A9brard%2C+G.&rft.au=Lecavelier+des+Etangs%2C+A.&rft.au=Martioli%2C+E.&rft.au=Dalal%2C+S.&rft.au=Vidal-Madjar%2C+A.&rft_id=https%3A%2F%2Fdoi.org%2F10.1051%252F0004-6361%252F202039168&rfr_id=info%3Asid%2Fen.wikipedia.org%3AList+of+exoplanet+extremes" class="Z3988"> </li> <li id="cite_note-115"><a href="#cite_ref-115">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://www.sci-news.com/astronomy/science-ezekiels-wheel-in-wheel-binary-system-gg-tauri-a-02241.html">"Astronomers Examine Ezekiel-like 'Wheel in a Wheel' in Binary System GG Tauri-A"</a>. Sci-News.com. 30 October 2014. Retrieved 10 February 2017.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Sci-News.com&rft.atitle=Astronomers+Examine+Ezekiel-like+%27Wheel+in+a+Wheel%27+in+Binary+System+GG+Tauri-A&rft.date=2014-10-30&rft_id=https%3A%2F%2Fwww.sci-news.com%2Fastronomy%2Fscience-ezekiels-wheel-in-wheel-binary-system-gg-tauri-a-02241.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AList+of+exoplanet+extremes" class="Z3988"> </li> </ol></div></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239543626"><div class="reflist reflist-lower-alpha"> <div class="mw-references-wrap"><ol class="references"> <li id="cite_note-10"><a href="#cite_ref-10">^</a> Gamma Leonis is mentioned to have a slightly higher magnitude (1.99), but it is the combined magnitude of the system and not of the planet-hosting star. The true apparent magnitude is 2.37. </li> <li id="cite_note-25"><a href="#cite_ref-25">^</a> The deuterium burning limit also depends on the metallicity and abundance of helium. Metal-rich planets, for example, need a lower mass to fuse deuterium. </li> <li id="cite_note-L/Teff-34"><a href="#cite_ref-L/Teff_34-0">^</a> Based on the estimated temperature and luminosity. </li> <li id="cite_note-50"><a href="#cite_ref-50">^</a> This is the calculated <a href="/wiki/Black-body_radiation" title="Black-body radiation">equilibrium temperature</a>, assuming an albedo of 0.3 </li> <li id="cite_note-64"><a href="#cite_ref-64">^</a> Assuming a circular orbit and using the <a href="/wiki/Kepler%27s_laws_of_planetary_motion" title="Kepler's laws of planetary motion">Kepler's Third law</a> </li> <li id="cite_note-94"><a href="#cite_ref-94">^</a> Determined using angular diameter and distance. 0.008 <a href="/wiki/Milliarcsecond" class="mw-redirect" title="Milliarcsecond">milliarcseconds</a> * 680 <a href="/wiki/Parsec" title="Parsec">pc</a> = diameter of 5.44 <a href="/wiki/Astronomical_unit" title="Astronomical unit">au</a>. </li> <li id="cite_note-107"><a href="#cite_ref-107">^</a> A normal star is a star that is past its <a href="/wiki/Protostar" title="Protostar">protostar</a> period, in its main fusion period, before becoming a degenerate star, black hole, or post-stellar nebula, and is not a brown dwarf </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2>[<a href="/w/index.php?title=List_of_exoplanet_extremes&action=edit&section=8" title="Edit section: External links">edit</a>]</div> <ul><li>WiredScience, <a rel="nofollow" class="external text" href="https://www.wired.com/wiredscience/2009/01/top-exoplanets/">Top 5 Most Extreme Exoplanets</a>, <a href="/wiki/Clara_Moskowitz" title="Clara Moskowitz">Clara Moskowitz</a>, 21 January 2009</li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r1129693374">.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 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href="/wiki/Template:Exoplanet" title="Template:Exoplanet"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Exoplanet" title="Template talk:Exoplanet"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Exoplanet" title="Special:EditPage/Template:Exoplanet"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Exoplanets" style="font-size:114%;margin:0 4em">Exoplanets</div></th></tr><tr><td class="navbox-abovebelow" colspan="3"><div> <ul><li><a href="/wiki/Planet" title="Planet">Planet</a> <ul><li><a href="/wiki/Definition_of_planet" title="Definition of planet">Definition</a> <ul><li><a href="/wiki/IAU_definition_of_planet" title="IAU definition of planet">IAU</a></li></ul></li></ul></li> <li><a href="/wiki/Planetary_science" title="Planetary science">Planetary science</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;">Main topics</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Exoplanet" title="Exoplanet">Exoplanet</a></li> <li><a href="/wiki/Exoplanet_orbital_and_physical_parameters" title="Exoplanet orbital and physical parameters">Exoplanet orbital and physical parameters</a></li> <li><a href="/wiki/Methods_of_detecting_exoplanets" title="Methods of detecting exoplanets">Methods of detecting exoplanets</a></li> <li><a href="/wiki/Planetary_system" title="Planetary system">Planetary system</a></li> <li><a href="/wiki/Planet-hosting_star" title="Planet-hosting star">Planet-hosting stars</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="10" style="width:1px;padding:0 0 0 2px"><div><a href="/wiki/PDS_70" title="PDS 70"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/1/1c/PDS_70.jpg/100px-PDS_70.jpg" decoding="async" width="100" height="85" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/1/1c/PDS_70.jpg/150px-PDS_70.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/1/1c/PDS_70.jpg/200px-PDS_70.jpg 2x" data-file-width="2000" data-file-height="1692" /></a></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;">Sizes and <a href="/wiki/List_of_planet_types" title="List of planet types">types</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%;text-align:center;"><a href="/wiki/Terrestrial_planet" title="Terrestrial planet">Terrestrial</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Carbon_planet" title="Carbon planet">Carbon planet</a></li> <li><a href="/wiki/Coreless_planet" title="Coreless planet">Coreless planet</a></li> <li><a href="/wiki/Desert_planet" title="Desert planet">Desert planet</a></li> <li><a href="/wiki/Dwarf_planet" title="Dwarf planet">Dwarf planet</a></li> <li><a href="/wiki/Hycean_planet" title="Hycean planet">Hycean planet</a></li> <li><a href="/wiki/Ice_planet" title="Ice planet">Ice planet</a></li> <li><a href="/wiki/Iron_planet" title="Iron planet">Iron planet</a> (Super-Mercury)</li> <li><a href="/wiki/Lava_planet" title="Lava planet">Lava planet</a></li> <li><a href="/wiki/Ocean_world" title="Ocean world">Ocean world</a></li> <li><a href="/wiki/Mega-Earth" title="Mega-Earth">Mega-Earth</a></li> <li><a href="/wiki/Sub-Earth" title="Sub-Earth">Sub-Earth</a></li> <li><a href="/wiki/Super-Earth" title="Super-Earth">Super-Earth</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:center;"><a href="/wiki/Gas_giant" title="Gas giant">Gaseous</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Eccentric_Jupiter" title="Eccentric Jupiter">Eccentric Jupiter</a></li> <li><a href="/wiki/Mini-Neptune" title="Mini-Neptune">Mini-Neptune</a> (Gas dwarf)</li> <li><a href="/wiki/Helium_planet" title="Helium planet">Helium planet</a></li> <li><a href="/wiki/Hot_Jupiter" title="Hot Jupiter">Hot Jupiter</a></li> <li><a href="/wiki/Hot_Neptune" title="Hot Neptune">Hot Neptune</a></li> <li><a href="/wiki/Gas_giant" title="Gas giant">Gas giant</a></li> <li><a href="/wiki/Ice_giant" title="Ice giant">Ice giant</a></li> <li><a href="/wiki/Super-Jupiter" title="Super-Jupiter">Super-Jupiter</a></li> <li><a href="/wiki/Super-Neptune" title="Super-Neptune">Super-Neptune</a></li> <li><a href="/wiki/Super-puff" title="Super-puff">Super-puff</a></li> <li><a href="/wiki/Ultra-hot_Jupiter" class="mw-redirect" title="Ultra-hot Jupiter">Ultra-hot Jupiter</a></li> <li><a href="/wiki/Ultra-hot_Neptune" class="mw-redirect" title="Ultra-hot Neptune">Ultra-hot Neptune</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:center;">Other types</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Blanet" title="Blanet">Blanet</a></li> <li><a href="/wiki/Brown_dwarf" title="Brown dwarf">Brown dwarf</a></li> <li><a href="/wiki/Chthonian_planet" title="Chthonian planet">Chthonian planet</a></li> <li><a href="/wiki/Circumbinary_planet" title="Circumbinary planet">Circumbinary planet</a></li> <li><a href="/wiki/Circumtriple_planet" title="Circumtriple planet">Circumtriple planet</a></li> <li><a href="/wiki/Disrupted_planet" title="Disrupted planet">Disrupted planet</a></li> <li><a href="/wiki/Double_planet" title="Double planet">Double planet</a></li> <li><a href="/wiki/Ecumenopolis" title="Ecumenopolis">Ecumenopolis</a></li> <li><a href="/wiki/Eyeball_planet" title="Eyeball planet">Eyeball planet</a></li> <li><a href="/wiki/Giant_planet" title="Giant planet">Giant planet</a></li> <li><a href="/wiki/Mesoplanet" title="Mesoplanet">Mesoplanet</a></li> <li><a href="/wiki/Planetary-mass_object" title="Planetary-mass object">Planemo</a></li> <li><a href="/wiki/Brown_dwarf#Low-mass_brown_dwarfs_versus_high-mass_planets" title="Brown dwarf">Planet/Brown dwarf boundary</a></li> <li><a href="/wiki/Planetesimal" title="Planetesimal">Planetesimal</a></li> <li><a href="/wiki/Protoplanet" title="Protoplanet">Protoplanet</a></li> <li><a href="/wiki/Pulsar_planet" title="Pulsar planet">Pulsar planet</a></li> <li><a href="/wiki/Sub-brown_dwarf" title="Sub-brown dwarf">Sub-brown dwarf</a></li> <li><a href="/wiki/Sub-Neptune" title="Sub-Neptune">Sub-Neptune</a></li> <li><a href="/wiki/Toroidal_planet" title="Toroidal planet">Toroidal planet</a></li> <li><a href="/wiki/Ultra-cool_dwarf" title="Ultra-cool dwarf">Ultra-cool dwarf</a></li> <li><a href="/wiki/Ultra-short_period_planet" title="Ultra-short period planet">Ultra-short period planet (USP)</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Formation_and_evolution_of_the_Solar_System" title="Formation and evolution of the Solar System">Formation and evolution</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">Accretion</a></li> <li><a href="/wiki/Accretion_disk" title="Accretion disk">Accretion disk</a></li> <li><a href="/wiki/Asteroid_belt" title="Asteroid belt">Asteroid belt</a></li> <li><a href="/wiki/Circumplanetary_disk" title="Circumplanetary disk">Circumplanetary disk</a></li> <li><a href="/wiki/Circumstellar_disc" title="Circumstellar disc">Circumstellar disc</a></li> <li><a href="/wiki/Circumstellar_envelope" title="Circumstellar envelope">Circumstellar envelope</a></li> <li><a href="/wiki/Cosmic_dust" title="Cosmic dust">Cosmic dust</a></li> <li><a href="/wiki/Debris_disk" title="Debris disk">Debris disk</a></li> <li><a href="/wiki/Detached_object" title="Detached object">Detached object</a></li> <li><a href="/wiki/Disrupted_planet" title="Disrupted planet">Disrupted planet</a></li> <li><a href="/wiki/Accretion_disk#Excretion_disk" title="Accretion disk">Excretion disk</a></li> <li><a href="/wiki/Exozodiacal_dust" title="Exozodiacal dust">Exozodiacal dust</a></li> <li><a href="/wiki/Extraterrestrial_materials" title="Extraterrestrial materials">Extraterrestrial materials</a></li> <li><a href="/wiki/Extraterrestrial_sample_curation" title="Extraterrestrial sample curation">Extraterrestrial sample curation</a></li> <li><a href="/wiki/Giant-impact_hypothesis" title="Giant-impact hypothesis">Giant-impact hypothesis</a></li> <li><a href="/wiki/Gravitational_collapse" title="Gravitational collapse">Gravitational collapse</a></li> <li><a href="/wiki/Hills_cloud" title="Hills cloud">Hills cloud</a></li> <li><a href="/wiki/Exoplanet_interiors" title="Exoplanet interiors">Internal structure</a></li> <li><a href="/wiki/Interplanetary_dust_cloud" title="Interplanetary dust cloud">Interplanetary dust cloud</a></li> <li><a href="/wiki/Interplanetary_medium" title="Interplanetary medium">Interplanetary medium</a></li> <li><a href="/wiki/Interplanetary_space" class="mw-redirect" title="Interplanetary space">Interplanetary space</a></li> <li><a href="/wiki/Interstellar_cloud" title="Interstellar cloud">Interstellar cloud</a></li> <li><a href="/wiki/Interstellar_dust" class="mw-redirect" title="Interstellar dust">Interstellar dust</a></li> <li><a href="/wiki/Interstellar_medium" title="Interstellar medium">Interstellar medium</a></li> <li><a href="/wiki/Outer_space#Interstellar_space" title="Outer space">Interstellar space</a></li> <li><a href="/wiki/Kuiper_belt" title="Kuiper belt">Kuiper belt</a></li> <li><a href="/wiki/List_of_interstellar_and_circumstellar_molecules" title="List of interstellar and circumstellar molecules">List of interstellar and circumstellar molecules</a></li> <li><a href="/wiki/Stellar_collision#Formation_of_planets" title="Stellar collision">Merging stars</a></li> <li><a href="/wiki/Molecular_cloud" title="Molecular cloud">Molecular cloud</a></li> <li><a href="/wiki/Nebular_hypothesis" title="Nebular hypothesis">Nebular hypothesis</a></li> <li><a href="/wiki/Oort_cloud" title="Oort cloud">Oort cloud</a></li> <li><a href="/wiki/Outer_space" title="Outer space">Outer space</a></li> <li><a href="/wiki/Planetary_migration" title="Planetary migration">Planetary migration</a></li> <li><a href="/wiki/Planetary_system" title="Planetary system">Planetary system</a></li> <li><a href="/wiki/Planetesimal" title="Planetesimal">Planetesimal</a></li> <li><a href="/wiki/Nebular_hypothesis#Formation_of_planets" title="Nebular hypothesis">Planet formation</a></li> <li><a href="/wiki/Protoplanetary_disk" title="Protoplanetary disk">Protoplanetary disk</a></li> <li><a href="/wiki/Ring_system" title="Ring system">Ring system</a></li> <li><a href="/wiki/Rubble_pile" title="Rubble pile">Rubble pile</a></li> <li><a href="/wiki/Sample-return_mission" title="Sample-return mission">Sample-return mission</a></li> <li><a href="/wiki/Scattered_disc" title="Scattered disc">Scattered disc</a></li> <li><a href="/wiki/Star_formation" title="Star formation">Star formation</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Planetary_system" title="Planetary system">Systems</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Exocomet" title="Exocomet">Exocomet</a> <ul><li><a href="/wiki/Interstellar_comet" class="mw-redirect" title="Interstellar comet">Interstellar</a></li></ul></li> <li><a href="/wiki/Exomoon" title="Exomoon">Exomoon</a> <ul><li><a href="/wiki/Tidally_detached_exomoon" title="Tidally detached exomoon">Tidally detached</a></li></ul></li> <li><a href="/wiki/Rogue_planet" title="Rogue planet">Rogue planet</a></li> <li>Orbits <ul><li><a href="/wiki/Retrograde_and_prograde_motion#Exoplanets" title="Retrograde and prograde motion">Retrograde</a></li> <li><a href="/wiki/Co-orbital_configuration#Trojans" title="Co-orbital configuration">Trojan</a></li> <li><a href="/wiki/Orbital_resonance#Mean-motion_resonances_among_extrasolar_planets" title="Orbital resonance">Mean-motion resonances</a></li> <li><a href="/wiki/Titius%E2%80%93Bode_law#Lunar_systems_and_other_planetary_systems" title="Titius–Bode law">Titius–Bode law</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Planetary_system#Planet-hosting_stars" title="Planetary system">Host stars</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/A-type_main-sequence_star#Planets" title="A-type main-sequence star">A</a></li> <li><a href="/wiki/B-type_main-sequence_star#Planets" title="B-type main-sequence star">B</a></li> <li><a href="/wiki/Binary_star#Planets" title="Binary star">Binary star</a></li> <li><a href="/wiki/Brown_dwarf#Planets_around_brown_dwarfs" title="Brown dwarf">Brown dwarfs</a></li> <li><a href="/wiki/F-type_main-sequence_star#Planets" title="F-type main-sequence star">F/Yellow-white dwarfs</a></li> <li><a href="/wiki/G-type_main-sequence_star#Planets" title="G-type main-sequence star">G/Yellow dwarfs</a></li> <li><a href="/wiki/Herbig_Ae/Be_star#Planets" title="Herbig Ae/Be star">Herbig Ae/Be</a></li> <li><a href="/wiki/K-type_main-sequence_star#Planets" title="K-type main-sequence star">K/Orange dwarfs</a></li> <li><a href="/wiki/Red_dwarf#Planets" title="Red dwarf">M/Red dwarfs</a></li> <li><a href="/wiki/Pulsar_planet" title="Pulsar planet">Pulsar</a></li> <li><a href="/wiki/Red_giant#Planets" title="Red giant">Red giant</a></li> <li><a href="/wiki/Subdwarf_B_star#Planetary_systems" title="Subdwarf B star">Subdwarf B</a></li> <li><a href="/wiki/Subgiant#Planets" title="Subgiant">Subgiant</a></li> <li><a href="/wiki/T_Tauri_star#Planets" title="T Tauri star">T Tauri</a></li> <li><a href="/wiki/White_dwarf#Debris_disks_and_planets" title="White dwarf">White dwarfs</a></li> <li><a href="/wiki/Yellow_giant#Planets" class="mw-redirect" title="Yellow giant">Yellow giants</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Methods_of_detecting_exoplanets" title="Methods of detecting exoplanets">Detection</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Astrometry" title="Astrometry">Astrometry</a></li> <li><a href="/wiki/Methods_of_detecting_exoplanets#Direct_imaging" title="Methods of detecting exoplanets">Direct imaging</a> <ul><li><a href="/wiki/List_of_directly_imaged_exoplanets" title="List of directly imaged exoplanets">list</a></li></ul></li> <li><a href="/wiki/Gravitational_microlensing" title="Gravitational microlensing">Microlensing</a> <ul><li><a href="/wiki/List_of_exoplanets_detected_by_microlensing" title="List of exoplanets detected by microlensing">list</a></li></ul></li> <li><a href="/wiki/Polarimetry" title="Polarimetry">Polarimetry</a></li> <li><a href="/wiki/Methods_of_detecting_exoplanets#Pulsar_timing" title="Methods of detecting exoplanets">Timing</a> <ul><li><a href="/wiki/List_of_exoplanets_detected_by_timing" title="List of exoplanets detected by timing">list</a></li></ul></li> <li><a href="/wiki/Doppler_spectroscopy" title="Doppler spectroscopy">Radial velocity</a> <ul><li><a href="/wiki/List_of_exoplanets_detected_by_radial_velocity" title="List of exoplanets detected by radial velocity">list</a></li></ul></li> <li><a href="/wiki/Methods_of_detecting_exoplanets#Transit_photometry" title="Methods of detecting exoplanets">Transit method</a> <ul><li><a href="/wiki/List_of_transiting_exoplanets" title="List of transiting exoplanets">list</a></li></ul></li> <li><a href="/wiki/Transit-timing_variation" title="Transit-timing variation">Transit-timing variation</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Planetary_habitability" title="Planetary habitability">Habitability</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Astrobiology" title="Astrobiology">Astrobiology</a></li> <li><a href="/wiki/Astrooceanography" class="mw-redirect" title="Astrooceanography">Astrooceanography</a></li> <li><a href="/wiki/Circumstellar_habitable_zone" class="mw-redirect" title="Circumstellar habitable zone">Circumstellar habitable zone</a></li> <li><a href="/wiki/Earth_analog" title="Earth analog">Earth analog</a></li> <li><a href="/wiki/Extraterrestrial_liquid_water" title="Extraterrestrial liquid water">Extraterrestrial liquid water</a></li> <li><a href="/wiki/Galactic_habitable_zone" title="Galactic habitable zone">Galactic habitable zone</a></li> <li><a href="/wiki/Habitability_of_binary_star_systems" title="Habitability of binary star systems">Habitability of binary star systems</a></li> <li><a href="/wiki/Habitability_of_F-type_main-sequence_star_systems" title="Habitability of F-type main-sequence star systems">Habitability of F-type main-sequence star systems</a></li> <li><a href="/wiki/Habitability_of_K-type_main-sequence_star_systems" title="Habitability of K-type main-sequence star systems">Habitability of K-type main-sequence star systems</a></li> <li><a href="/wiki/Habitability_of_natural_satellites" title="Habitability of natural satellites">Habitability of natural satellites</a></li> <li><a href="/wiki/Habitability_of_neutron_star_systems" title="Habitability of neutron star systems">Habitability of neutron star systems</a></li> <li><a href="/wiki/Habitability_of_red_dwarf_systems" title="Habitability of red dwarf systems">Habitability of red dwarf systems</a></li> <li><a href="/wiki/Habitability_of_yellow_dwarf_systems" title="Habitability of yellow dwarf systems">Habitability of yellow dwarf systems</a></li> <li><a href="/wiki/Habitable_zone_for_complex_life" title="Habitable zone for complex life">Habitable zone for complex life</a></li> <li><a href="/wiki/List_of_potentially_habitable_exoplanets" title="List of potentially habitable exoplanets">List of potentially habitable exoplanets</a></li> <li><a href="/wiki/Tholin" title="Tholin">Tholin</a></li> <li><a href="/wiki/Superhabitable_planet" class="mw-redirect" title="Superhabitable planet">Superhabitable planet</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;">Catalogues</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Catalog_of_Nearby_Habitable_Systems" title="Catalog of Nearby Habitable Systems">Nearby Habitable Systems</a></li> <li><a href="/wiki/Exoplanet_Data_Explorer" title="Exoplanet Data Explorer">Exoplanet Data Explorer</a></li> <li><a href="/wiki/Extrasolar_Planets_Encyclopaedia" title="Extrasolar Planets Encyclopaedia">Extrasolar Planets Encyclopaedia</a></li> <li><a href="/wiki/NASA_Exoplanet_Archive" title="NASA Exoplanet Archive">NASA Exoplanet Archive</a></li> <li><a href="/wiki/NASA_Star_and_Exoplanet_Database" title="NASA Star and Exoplanet Database">NASA Star and Exoplanet Database</a></li> <li><a href="/wiki/Open_Exoplanet_Catalogue" title="Open Exoplanet Catalogue">Open Exoplanet Catalogue</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;"><a href="/wiki/Lists_of_planets" title="Lists of planets">Lists</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li>Exoplanetary systems <ul><li><a href="/wiki/List_of_exoplanetary_host_stars" class="mw-redirect" title="List of exoplanetary host stars">Host stars</a></li> <li><a href="/wiki/List_of_multiplanetary_systems" title="List of multiplanetary systems">Multiplanetary systems</a></li> <li><a href="/wiki/List_of_stars_with_proplyds" title="List of stars with proplyds">Stars with proto-planetary discs</a></li></ul></li></ul> <ul><li><a href="/wiki/Lists_of_exoplanets" class="mw-redirect" title="Lists of exoplanets">Exoplanets</a> <ul><li><a href="/wiki/Discoveries_of_exoplanets" title="Discoveries of exoplanets">Discoveries</a></li> <li><a class="mw-selflink selflink">Extremes</a></li> <li><a href="/wiki/List_of_exoplanet_firsts" title="List of exoplanet firsts">Firsts</a></li> <li><a href="/wiki/List_of_nearest_exoplanets" title="List of nearest exoplanets">Nearest</a></li> <li><a href="/wiki/List_of_largest_exoplanets" title="List of largest exoplanets">Largest</a></li> <li><a href="/wiki/List_of_most_massive_exoplanets" class="mw-redirect" title="List of most massive exoplanets">Heaviest</a></li> <li><a href="/wiki/List_of_nearest_terrestrial_exoplanet_candidates" title="List of nearest terrestrial exoplanet candidates">Terrestrial candidates</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_by_the_Kepler_space_telescope" title="List of exoplanets discovered by the Kepler space telescope">Kepler</a> <ul><li><a href="/wiki/List_of_exoplanets_discovered_by_the_Kepler_space_telescope:_1%E2%80%93500" title="List of exoplanets discovered by the Kepler space telescope: 1–500">1–500</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_by_the_Kepler_space_telescope:_501%E2%80%931000" title="List of exoplanets discovered by the Kepler space telescope: 501–1000">501–1000</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_by_the_Kepler_space_telescope:_1001%E2%80%931500" title="List of exoplanets discovered by the Kepler space telescope: 1001–1500">1001–1500</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_by_the_Kepler_space_telescope:_1501%E2%80%932000" title="List of exoplanets discovered by the Kepler space telescope: 1501–2000">1501–2000</a></li></ul></li> <li><a href="/wiki/List_of_exoplanets_observed_during_Kepler%27s_K2_mission" title="List of exoplanets observed during Kepler's K2 mission">K2</a></li> <li><a href="/wiki/List_of_potentially_habitable_exoplanets" title="List of potentially habitable exoplanets">Potentially habitable</a></li> <li><a href="/wiki/List_of_proper_names_of_exoplanets" title="List of proper names of exoplanets">Proper names</a></li></ul></li></ul> <ul><li>Discovered exoplanets by year <ul><li><a href="/wiki/List_of_exoplanets_discovered_before_2000" title="List of exoplanets discovered before 2000">before 2000</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_between_2000%E2%80%932009" title="List of exoplanets discovered between 2000–2009">2000–2009</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2010" title="List of exoplanets discovered in 2010">2010</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2011" title="List of exoplanets discovered in 2011">2011</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2012" title="List of exoplanets discovered in 2012">2012</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2013" title="List of exoplanets discovered in 2013">2013</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2014" title="List of exoplanets discovered in 2014">2014</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2015" title="List of exoplanets discovered in 2015">2015</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2016" title="List of exoplanets discovered in 2016">2016</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2017" title="List of exoplanets discovered in 2017">2017</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2018" title="List of exoplanets discovered in 2018">2018</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2019" title="List of exoplanets discovered in 2019">2019</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2020" title="List of exoplanets discovered in 2020">2020</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2021" title="List of exoplanets discovered in 2021">2021</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2022" title="List of exoplanets discovered in 2022">2022</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2023" title="List of exoplanets discovered in 2023">2023</a></li> <li><a href="/wiki/List_of_exoplanets_discovered_in_2024" title="List of exoplanets discovered in 2024">2024</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%;text-align:right;">Other</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Carl_Sagan_Institute" title="Carl Sagan Institute">Carl Sagan Institute</a></li> <li><a href="/wiki/Exoplanet_naming_convention" title="Exoplanet naming convention">Exoplanet naming convention</a></li> <li><a href="/wiki/Phase_curve_(astronomy)#Exoplanets" title="Phase curve (astronomy)">Exoplanet phase curves</a></li> <li><a href="/wiki/Exoplanetary_Circumstellar_Environments_and_Disk_Explorer" title="Exoplanetary Circumstellar Environments and Disk Explorer">Exoplanetary Circumstellar Environments and Disk Explorer</a></li> <li><a href="/wiki/Extragalactic_planet" title="Extragalactic planet">Extragalactic planet</a></li> <li><a href="/wiki/Extrasolar_planets_in_fiction" title="Extrasolar planets in fiction">Extrasolar planets in fiction</a></li> <li><a href="/wiki/Geodynamics_of_terrestrial_exoplanets" title="Geodynamics of terrestrial exoplanets">Geodynamics of terrestrial exoplanets</a></li> <li><a href="/wiki/Neptunian_desert" title="Neptunian desert">Neptunian desert</a></li> <li><a href="/wiki/Nexus_for_Exoplanet_System_Science" title="Nexus for Exoplanet System Science">Nexus for Exoplanet System Science</a></li> <li><a href="/wiki/Globular_cluster#Planets" title="Globular cluster">Planets in globular clusters</a></li> <li><a href="/wiki/Small_planet_radius_gap" title="Small planet radius gap">Small planet radius gap</a></li> <li><a href="/wiki/Sudarsky%27s_gas_giant_classification" title="Sudarsky's gas giant classification">Sudarsky's gas giant classification</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="3"><div> <ul><li><a href="/wiki/Discoveries_of_exoplanets" title="Discoveries of exoplanets">Discoveries of exoplanets</a></li> <li><a href="/wiki/List_of_exoplanet_search_projects" title="List of exoplanet search projects">Search projects</a></li></ul> </div></td></tr></tbody></table></div> <style data-mw-deduplicate="TemplateStyles:r1130092004">.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;justify-content:center;align-items:baseline}.mw-parser-output .portal-bar-bordered{padding:0 2em;background-color:#fdfdfd;border:1px solid #a2a9b1;clear:both;margin:1em auto 0}.mw-parser-output .portal-bar-related{font-size:100%;justify-content:flex-start}.mw-parser-output .portal-bar-unbordered{padding:0 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