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{{short description|Wikipediaartikel listdaftar articleWikipedia}}
Berikut ini adalah daftar keesktreman di antara [[eksoplanet]] yang diketahui. Properti yang tercantum di sini adalah properti yang nilainya diketahui secara terpercaya.
{{Use dmy dates|date=July 2013}}
The following are lists of extremes among the known [[exoplanet]]s. The properties listed here are those for which values are known reliably.
 
== Ekstrem dari sudut pandang Bumi ==
==Extremes from Earth's viewpoint==
{| class="wikitable"
|-
! TitleJudul
! Planet
! StarBintang
! Data
! NotesCatatan
|-
| Paling jauh ditemukan
| Most distant discovered
| [[SWEEPS-11]] / [[SWEEPS-04]]
| SWEEPS J175902.67−291153.5
| 27,710 [[lighttahun year]]scahaya.<ref>{{cite web | url=http://phl.upr.edu/projects/habitable-exoplanets-catalog/top10 | title= HEC: Top 10 Exoplanets | publisher=University of Puerto Rico at Arecibo | date=5 December 2015 | accessdate=1 August 2017 | archive-date=2013-12-17 | archive-url=https://web.archive.org/web/20131217224149/http://phl.upr.edu/projects/habitable-exoplanets-catalog/top10 | dead-url=yes }}</ref>
| AnSebuah analysisanalisis ofkurva thecahaya lightcurvedari ofperistiwa thepelensaan microlensing eventmikro [[PA-99-N2]] menunjukkan suggestsadanya the presence of asebuah planet orbitingyang amengorbit starbintang in thedi [[Galaksi Andromeda Galaxy]] (2.,54 ± 0.,11 Mly).<ref>{{cite encyclopedia |title=Notes for star PA-99-N2 |encyclopedia=The Extrasolar Planets Encyclopaedia |url=http://exoplanet.eu/star.php?st=PA-99-N2 |date= |year= |author=Schneider, J. |accessdate=2010-08-06 }}</ref> InPada lateakhir JanuaryJanuari 2018,<ref name="Dai Guerras p=L27">{{cite journal | last=Dai | first=Xinyu | last2=Guerras | first2=Eduardo | title=Probing Extragalactic Planets Using Quasar Microlensing | journal=The Astrophysical Journal | volume=853 | issue=2 | date=2 February 2018 | issn=2041-8213 | doi=10.3847/2041-8213/aaa5fb | page=L27 |arxiv=1802.00049 | bibcode=2018ApJ...853L..27D}}</ref> asebuah teamtim ofilmuwan scientistsyang leddipimpin byoleh Xinyu Dai claimedmengklaim totelah havemenemukan discoveredkumpulan a collection of aboutsekitar 2,.000 [[rogueplanet planetpengembara]]s indi themikrolensa [[quasarkuasar]] microlens [[RX J1131-1231]], whichyang isberjarak 3.,8 billionmiliar light-yearstahun distantcahaya. TheMassa bodiesbenda-benda rangetersebut inberkisar massdari fromBulan thathingga ofbeberapa the Moon to severalmassa Jupiter masses.<ref>{{cite web|title=Astronomers Claim to Find Population of Rogue Exoplanets in Distant Galaxy |website=Science News |url=http://www.sci-news.com/astronomy/rogue-exoplanets-distant-galaxy-05691.html}}</ref><ref name="Dai Guerras p=L27" />
ThePlanet mostpaling distantjauh potentiallyyang habitableberpotensi planetdapat dihuni yang confirmeddikonfirmasi isadalah Kepler-443b, atpada jarak 2,.540 light-yearstahun distantcahaya,<ref>{{cite web|url=http://exoplanet.eu/catalog/kepler-443_b/ |title=The Extrasolar Planet Encyclopaedia — Kepler-443 b |publisher=Exoplanet.eu |date=2015-01-09 |accessdate=2018-10-20}}</ref> although the unconfirmedmeskipun planet [[KOI-5889.01]] isyang overbelum dikonfirmasi berjarak lebih dari 5,.000 light-yearstahun distantcahaya.
|-
| Terdekat
| Least distant
| {{nowrap|[[Proxima Centauri b]]}} anddan c
| {{nowrap|[[Proxima Centauri]]}}
| 4.22 lighttahun yearscahaya
| Proxima Centauri b isadalah theeksoplanet closestberbatu rockyterdekat exoplanet and closestdan [[ListDaftar eksoplanet ofyang potentiallyberpotensi habitablelaik exoplanetshuni|potentiallyeksoplanet habitableterdekat exoplanetyang berpotensi dihuni]] known, anddan c is the closestadalah super-EarthBumi andterdekat potentially-ringeddan planet yang berpotensi memiliki cincin. AsKarena Proxima Centauri isadalah thebintang closestterdekat stardengan to the SunMatahari (anddan willakan staytetap sodemikian for the nextselama 25,.000 yearstahun ke depan), thisini isadalah ansebuah absoluterekor recordmutlak.
|-
| Terlihat secara langsung paling jauh
| Most distant directly visible
| [[CVSO 30]] c
| [[CVSO 30]]
| 1,200 [[light year|tahun cahaya]]s
| AlsoJuga firstpertama directlykali imagedmencitrakan planet insecara systemlangsung withdalam asistem transitingdengan sebuah planet transit.
|-
| Terlihat secara langsung paling tidak jauh
| Least distant directly visible
| [[Proxima Centauri c]]
| [[Proxima Centauri]]
| 4.22 [[lighttahun yearcahaya]]s
| ConfirmedDikonfirmasi inpada 2020 usingmenggunakan archivaldata arsip Hubble datadari fromtahun 1995+.
|-
| StarBintang with the brightestdengan [[apparentmagnitudo magnitudetampak]] withpaling terang dengan asebuah planet
| [[Pollux b]]
| [[Pollux (star)|Pollux]]<ref name=apj162_217>{{citation | last1=Lee | first1=T. A. | title=Photometry of high-luminosity M-type stars | journal=Astrophysical Journal | volume=162 | page=217 |date=October 1970 | doi=10.1086/150648 | bibcode=1970ApJ...162..217L }}</ref>
| ApparentMagnitudo magnitudetampak isadalah 1.14
| The evidence of planets around [[Vega]] with an apparent magnitude of 0.03 is strongly suggested by [[circumstellar disk]]s surrounding it. {{As of|2018}}, no planets had yet been confirmed.<ref>{{cite press release | title= NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega | url=http://www.nasa.gov/home/hqnews/2013/jan/HQ_13-006_Vega_Asteroid_Belt.html | publisher=Whitney Clavin, NASA | date=8 January 2013 | accessdate=4 March 2013}}</ref>
 
Baris 51 ⟶ 50:
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|-
| Pemisahan [[jarak sudut]] terbesar dari bintang induknya
| Largest [[angular distance]] separation from its host star
| [[GU Piscium b]]
| [[GU Piscium]]
| 42 arcdetik secondsark<ref>{{cite encyclopedia |title=GU Psc b |encyclopedia=The Extrasolar Planet Encyclopaedia |url=http://exoplanet.eu/catalog/gu_psc_b/ |date= |year= |publisher= |location= |id= }}</ref>
| The upper mass limit (13 Jupiter masses) may make this a brown dwarf. WD 0806-661 b has an angular separation of 130.2 arc seconds from [[WD 0806-661]]. However, its planetary origin is also unknown. Not counting either of these, [[DT Virginis]] b would be the widest-separated definite exoplanet.
<!-- --uncomment this when this is filled out--
Baris 65 ⟶ 64:
|}
 
==Karakteristik keplanetan==
==Planetary characteristics==
{| class="wikitable"
|-
! TitleJudul
! Planet
! StarBintang
! Data
! NotesCatatan
|-
 
| Paling tidak masif
| Least massive
|[[WD 1145+017 b]]
|[[WD 1145+017]]
Baris 81 ⟶ 80:
|
|-
| Paling masif
| Most massive
| colspan="4" |TheKandidat candidateplanet forpaling themasif mostmasih massive planet is contentiousdiperdebatkan, askarena itsulit isuntuk difficultmenentukan toantara determinesebuah betweenplanet ayang highlysangat massivemasif planetdan and asebuah [[brownkatai dwarfcoklat]]. ItPlanet isterbesar estimateddiperkirakan theberukuran largestsekitar planetsselusin are approximately a dozenmassa [[Jupiter]] masses.
|-
| Jari-jari terbesar
| Largest radius
| [[HD 100546 b]]
| [[HD 100546]]
| 6.9{{±|2.7|2.9}}<ref name="quanz2014">{{cite journal|author=Quanz, Sasch P.|display-authors=4|author2=Amara, Adam|author3=Meyer, Michael P.|author4=Kenworthy, Matthew P.|author5=Kasper, Markus|author6=Girard, Julien H.|date=2014|title=Confirmation and characterization of the protoplanet HD100546 b - Direct evidence for gas giant planet formation at 50 au|journal= Astrophysical Journal|volume=807|issue=1|pages=64|arxiv = 1412.5173 |bibcode = 2015ApJ...807...64Q |doi = 10.1088/0004-637X/807/1/64 }}</ref> Jupiter radii
| LargestEksoplanet exoplanetterbesar in thedalam [[NASA Exoplanet Archive]], althoughmeskipun becausekarena offluks flux from thedari planet anddan thecakram diskyang that are superimposedditumpangkan, the exact size ofukuran thispasti planet cannottersebut betidak determineddapat andditentukan thedan emittingwilayah areapemancarannya hasmemiliki thisukuran sizetersebut, composedterdiri of thedari planet and includingdan itstermasuk diskcakramnya, notbukan tountuk bedisalahartikan mistakensebagai assebuah a singlejari-jari planet radiustunggal. OverSeiring timewaktu, it willplanet shrinktersebut toakan themenyusut sizemenjadi ofseukuran Jupiter. 20 {{Jupiter mass}}MJ; iskemungkinan likelyadalah asebuah brownkatai dwarfcoklat. </small>
|-
| Jari-jari terpendek
| Smallest radius
|[[SDSS J1228+1040 b]]
|[[SDSS J1228+1040 ]]
| 126 &nbsp;km<ref>{{Cite web|url=http://exoplanet.eu/catalog/sdss_j1228+1040_b/|title=Planet SDSS J1228+1040 b|website=exoplanet.eu|access-date=2019-08-05}}</ref>
|
|-
| MostPaling denserapat
|[[K2-38b]]
|[[K2-38]]
Baris 102 ⟶ 101:
|
|-
| Paling tidak rapat
| Least dense
| [[Kepler-51c]], [[Kepler-51b|b]] anddan/oratau possiblykemungkinan [[Kepler-51d|d]]<ref name="Masuda">[http://arxiv.org/abs/1401.2885 Very Low-Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event]: Kento Masuda</ref>
| [[Kepler-51]]<ref name="Masuda" />
| ~ 0.03 g/cm<sup>3</sup><ref name="Masuda" />
| The densities of Kepler-51 b and c have been constrained to be below 0.05 g/cm<sup>3</sup> (expected value 0.03 g/cm<sup>3</sup> for each). The density of Kepler-51d is determined to be 0.046±0.009 g/cm<sup>3</sup>.<ref name="Masuda" />
|-
| Terpanas
| Hottest
| {{nowrap| [[Kepler-70b]] }}
| {{nowrap| [[Kepler-70]] }}
Baris 114 ⟶ 113:
|
|-
| Terdingin
| Coldest
| {{nowrap| [[OGLE-2016-BLG-1195Lb]] }}
| {{nowrap| [[OGLE-2016-BLG-1195L]] }}
Baris 120 ⟶ 119:
|
|-
| Highest [[albedoAlbedo]] terbesar
| [[Kepler-10b]]{{citation needed|date=March 2014}}
| [[Kepler-10]]
| 0.5–0.6 (geometric albedo geometrik)
|
|-
| Albedo terendah
| Lowest albedo
| {{nowrap|[[TrES-2b]]}}
| {{nowrap|[[GSC 03549-02811]]}}
| [[GeometricAlbedo albedogeometrik]] {{nowrap|< 1%}}<ref name=darkest>{{cite journal|url=http://www.astro.princeton.edu/~dsp/PrincetonSite/Home_files/darkest_world.pdf |author=David M. Kipping |display-authors=etal |title=Detection of visible light from the darkest world |journal=[[Monthly Notices of the Royal Astronomical Society]] |accessdate=2011-08-12 |doi=10.1111/j.1745-3933.2011.01127.x |arxiv=1108.2297 |bibcode=2011MNRAS.417L..88K |url-status=dead |archiveurl=https://web.archive.org/web/20120317203801/http://www.astro.princeton.edu/~dsp/PrincetonSite/Home_files/darkest_world.pdf |archivedate=17 March 2012 |volume=417 |issue=1 |pages=L88–L92|year=2011 }}</ref>
| Best-fit model for albedo gives 0.04% (0.0004)<ref name=darkest/>
|-
| Termuda
| Youngest
|[[Proplyd 133-353]]
|[[Proplyd 133-353]]
| 0.5&nbsp;[[Mth|Myr]]<ref>{{Cite journal|last=Fang|first=Min|last2=Kim|first2=Jinyoung Serena|last3=Pascucci|first3=Ilaria|last4=Apai|first4=Dániel|last5=Manara|first5=Carlo Felice|date=2016-12-12|title=A candidate planetary-mass object with a photoevaporating disk in Orion|journal=The Astrophysical Journal|volume=833|issue=2|pages=L16|doi=10.3847/2041-8213/833/2/L16|issn=2041-8213|arxiv=1611.09761}}</ref><ref>{{Cite web|url=http://exoplanet.eu/catalog/proplyd_133-353/|title=The Extrasolar Planet Encyclopaedia — Proplyd 133-353|website=exoplanet.eu|access-date=2019-03-30}}</ref>
|TheBatas uppermassa massyang limitlebih tinggi (13 massa Jupiter masses) may make thisdapat amenjadikannya brownkatai dwarfcoklat.
|-
| OldestTertua
| {{nowrap| [[PSR B1620-26 b]] }}
| {{nowrap| [[PSR B1620-26]] }}
| 13&nbsp;[[GigayearGigatahun|Gyr]]
| Orbits in a circumbinary orbit around two stellar remnants{{snd}} a [[pulsar]] and a [[white dwarf]]. [[Kapteyn b]] is the oldest potentially habitable exoplanet at 11 Gyr.<ref>{{cite web|url=https://phys.org/news/2014-06-earth-bigger-older-brother-planet.html|title=Introducing Earth's bigger, older brother: planet Kapteyn b| date=14 June 2014}}</ref>
|}
 
==Karakteristik orbit==
==Orbital characteristics==
{| class="wikitable" style="text-align:left;"
|-
Baris 154 ⟶ 153:
! style="background:#efefef;"| Notes
|-
| LongestPeriode [[orbit]]al periodterlama <br/> <small>(LongestTahun yearterlama)</small>
| [[2MASS J2126-8140]]
| [[TYC 9486-927-1]]
| <!---... days--> ~1,000,000 yearstahun
| [[GU Piscium b]] previously held record at<!---... days--> 163,000 years.
|-
| ShortestPeriode orbital periodorbit terpendek<br/> <small>(ShortestTahun yearterpendek)</small>
| {{nowrap|[[SWIFT J1756.9-2508 b]]}}
| {{nowrap|[[SWIFT J1756.9-2508]]}}
| {{nowrap|48 minutesmenit, 56.5 secondsdetik}}<ref>{{cite web|url=http://exoplanet.eu/catalog/swift_j1756-2508/|title=The Extrasolar Planet Encyclopaedia — SWIFT J1756-2508|website=exoplanet.eu|access-date=2018-08-22}}</ref>
| [[K2-137b]] hasmemiliki theorbit shortestterpendek orbitdi aroundsekitar asebuah main-sequencebintang starderet utama (ankatai M dwarf) atpada 4.,31 hoursjam.<ref>{{cite web |website=Exoplanet.eu |year=2018 |title=The Extrasolar Planet Encyclopaedia — K2-137 b. |url=http://exoplanet.eu/catalog/k2-137_b/}}</ref>
|-
| [[Eksentrisitas orbit|Orbit tereksentrik]]
| Most [[Orbital eccentricity|eccentric orbit]]
| {{nowrap|[[HD 20782 b]]}}<ref name=SD-2009-12-12>{{cite web | title=HD 20781 b | website=Open Exoplanet Catalogue | url=http://www.openexoplanetcatalogue.com/system.html?id=HD+20781+b | access-date=20 October 2018}}</ref>
| [[HD 20782]]
| {{val|0.956|0.004}}
| <ref>{{Cite web|url=http://exoplanet.eu/catalog/hd_20782_b/|title=The Extrasolar Planet Encyclopaedia — HD 20782 b|website=exoplanet.eu|access-date=2019-05-04}}</ref> Record among confirmed planets. Putative satellite of [[VB 10]] may have higher eccentricity of 0.98.<ref>{{Cite web|url=http://exoplanet.eu/catalog/vb_10_b/|title=The Extrasolar Planet Encyclopaedia — VB 10 b|website=exoplanet.eu|access-date=2020-02-12}}</ref>
|-
<!-- "Least eccentric" makes no sense: there are *many* planets with e = 0 measurements
Baris 211 ⟶ 210:
-->
|-
| Orbit terbesar di sekitar sebuah bintang tunggal
| Largest orbit around a single star
| {{nowrap|[[2MASS J2126-8140]]}}
| {{nowrap|[[TYC 9486-927-1]]}}
Baris 217 ⟶ 216:
| The upper mass limit (13 Jupiter masses) may make this a brown dwarf. Next largest are [[CVSO 30]] c with ~660 AU and [[HD 106906 b]]<ref name="HD106906b">{{cite web | last = Chow | first = Denise | url = http://www.space.com/23858-most-distant-alien-planet-discovery-hd106906b.html | title = Giant Alien Planet Discovered in Most Distant Orbit Ever Seen | date = 6 December 2013 | work = [[space.com]] | accessdate = 8 December 2013 }}</ref><ref name="BaileyEtAl2013">{{cite journal | last = Bailey | first = Vanessa |display-authors=etal | arxiv = 1312.1265 | title = HD 106906 b: A planetary-mass companion outside a massive debris disk | date = January 2014 <!-- arXiv v1: 4 December 2013 --> | journal=The Astrophysical Journal Letters | volume=780 | issue=1 | id=L4 | doi=10.1088/2041-8205/780/1/L4 | bibcode=2014ApJ...780L...4B | page=L4}}</ref> with ~650 AU
|-
| Orbit terkecil
| Smallest orbit
| {{nowrap|[[WD 1202-024 B]]}}<ref name="Bailes2011">{{cite journal |doi=10.1126/science.1208890 |title=Transformation of a Star into a Planet in a Millisecond Pulsar Binary |year=2011 |last1=Bailes |first1=M. |last2=Bates |first2=S. D. |last3=Bhalerao |first3=V. |last4=Bhat |first4=N. D. R. |last5=Burgay |first5=M. |last6=Burke-Spolaor |first6=S. |last7=d'Amico |first7=N. |last8=Johnston |first8=S. |last9=Keith |first9=M. J. |journal=Science |url=http://www.swinburne.edu.au/chancellery/mediacentre/resources/Diamond-planet-Science.pdf|bibcode = 2011Sci...333.1717B |pmid=21868629 |volume=333 |issue=6050 |pages=1717–20|arxiv = 1108.5201 |display-authors=9 |last10=Kramer |first10=M. |last11=Kulkarni |first11=S. R. |last12=Levin |first12=L. |last13=Lyne |first13=A. G. |last14=Milia |first14=S. |last15=Possenti |first15=A. |last16=Spitler |first16=L. |last17=Stappers |first17=B. |last18=Van Straten |first18=W. |citeseerx=10.1.1.753.7160 }}</ref>
| {{nowrap|[[WD 1202-024]]}}
Baris 223 ⟶ 222:
|
|-
| Orbit terkecil di sekitar bintang biner
| Smallest orbit around binary star
| {{nowrap|[[Kepler-47b]]}}
| {{nowrap|[[Kepler-47]]AB}}
Baris 229 ⟶ 228:
|<ref>{{cite journal | journal = Science |title=Kepler-47: A Transiting Circumbinary Multi-Planet System |date=2012| author= OROSZ J. | author2= WELSH W. | author3= CARTER J.| author4= FABRYCKY D. | author5= COCHRAN W. | display-authors= etal | doi = 10.1126/science.1228380 | volume = 337 | issue = 6101 | pages = 1511–4 | pmid = 22933522 |bibcode = 2012Sci...337.1511O |arxiv = 1208.5489 }}</ref>
|-
| SmallestRasio ratio ofterkecil [[sumbu semi-major axismayor]] ofdari asebuah planet orbityang tomengorbit binarydengan starorbit orbitbintang biner
| {{nowrap|[[Kepler-16b]]}}
| {{nowrap|[[Kepler-16]]AB}}
Baris 235 ⟶ 234:
|<ref name="kepler16b">{{cite journal |author= Laurance R. Doyle |author2= Joshua A. Carter |author3= Daniel C. Fabrycky|author4= Robert W. Slawson |author5= Steve B. Howell|author6= Joshua N. Winn |author7= Jerome A. Orosz|author8= Andrej Prsa |author9= William F. Welsh |arxiv=1109.3432 |title=Kepler-16: A Transiting Circumbinary Planet |date=2011 |version= |display-authors=etal |doi=10.1126/science.1210923 |volume=333 |issue= 6049 |journal=Science |pages=1602–1606 |pmid=21921192|bibcode = 2011Sci...333.1602D }}</ref>
|-
| Orbit terbesar di sekitar bintang biner
| Largest orbit around binary star
| {{nowrap|[[DT Virginis c]]}}
| {{nowrap|[[DT Virginis]]}}
| 1,168 AU
| StarSistem systembintang istersebut alsojuga knowndikenal assebagai Ross 458 AB. ThePlanet planettersebut wasakhirnya eventuallydipastikan confirmedberada todi bebawah belowbatas pembakaran deuterium burning limit but itstetapi formationasal originpembentukannya istidak unknowndiketahui.
|-
| Orbit terbesar di sekitar sebuah bintang tunggal dalam sistem bintang ganda
| Largest orbit around a single star in a multiple star system
| {{nowrap|[[Fomalhaut b]]}}
| {{nowrap|[[Fomalhaut]]}}
Baris 247 ⟶ 246:
| The second stellar component of the system, [[TW Piscis Austrini]], has a semi-major axis of 57,000 AU from Fomalhaut and the third stellar component, LP 876-10 orbits 158,000 AU away from Fomalhaut.
|-
| Jarak terjauh antara bintang biner dengan sebuah planet sirkumbiner
| Largest distance between binary stars with a circumbinary planet
| [[FW Tauri AB b]]
| [[FW Tau AB]]
| ≈11 AU
| FW Tauri AB b orbitsmengorbit atpada a distance ofjarak 150-300 AUSA.<ref>{{Cite journal|last=Kraus|first=Adam|last2=J. Ireland|first2=Michael|last3=A. Cieza|first3=Lucas|last4=Hinkley|first4=Sasha|last5=J. Dupuy|first5=Trent|last6=P. Bowler|first6=Brendan|last7=C. Liu|first7=Michael|date=2 January 2014|title=Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B|journal=Science|volume=781|issue=1|page=1311|arxiv=1311.7664|doi=10.1088/0004-637X/781/1/20|bibcode=2014ApJ...781...20K}}</ref>
|-
| ClosestOrbit orbitterdekat betweenantara starsbintang withdengan asebuah planet orbitingyang onemengorbit ofsalah thesatu starsbintang
| {{nowrap|[[OGLE-2013-BLG-0341LBb]]}}
| {{nowrap|[[OGLE-2013-BLG-0341LB]]}}
| ~12–17 AU <br>(10 or 14 AU projected distance)<ref name="Gould Udalski Shin Porritt pp. 46–49">{{cite journal | last=Gould | first=A. | last2=Udalski | first2=A. | last3=Shin | first3=I.- G. | last4=Porritt | first4=I. | last5=Skowron | first5=J. | last6=Han | first6=C. | last7=Yee | first7=J. C. | last8=Koz owski | first8=S. | last9=Choi | first9=J.- Y. | last10=Poleski | first10=R. | last11=Wyrzykowski | first11= . | last12=Ulaczyk | first12=K. | last13=Pietrukowicz | first13=P. | last14=Mroz | first14=P. | last15=Szyma ski | first15=M. K. | last16=Kubiak | first16=M. | last17=Soszy ski | first17=I. | last18=Pietrzy ski | first18=G. | last19=Gaudi | first19=B. S. | last20=Christie | first20=G. W. | last21=Drummond | first21=J. | last22=McCormick | first22=J. | last23=Natusch | first23=T. | last24=Ngan | first24=H. | last25=Tan | first25=T.- G. | last26=Albrow | first26=M. | last27=DePoy | first27=D. L. | last28=Hwang | first28=K.- H. | last29=Jung | first29=Y. K. | last30=Lee | first30=C.- U. | last31=Park | first31=H. | last32=Pogge | first32=R. W. | last33=Abe | first33=F. | last34=Bennett | first34=D. P. | last35=Bond | first35=I. A. | last36=Botzler | first36=C. S. | last37=Freeman | first37=M. | last38=Fukui | first38=A. | last39=Fukunaga | first39=D. | last40=Itow | first40=Y. | last41=Koshimoto | first41=N. | last42=Larsen | first42=P. | last43=Ling | first43=C. H. | last44=Masuda | first44=K. | last45=Matsubara | first45=Y. | last46=Muraki | first46=Y. | last47=Namba | first47=S. | last48=Ohnishi | first48=K. | last49=Philpott | first49=L. | last50=Rattenbury | first50=N. J. | last51=Saito | first51=T. | last52=Sullivan | first52=D. J. | last53=Sumi | first53=T. | last54=Suzuki | first54=D. | last55=Tristram | first55=P. J. | last56=Tsurumi | first56=N. | last57=Wada | first57=K. | last58=Yamai | first58=N. | last59=Yock | first59=P. C. M. | last60=Yonehara | first60=A. | last61=Shvartzvald | first61=Y. | last62=Maoz | first62=D. | last63=Kaspi | first63=S. | last64=Friedmann | first64=M. | title=A terrestrial planet in a ~1-AU orbit around one member of a 15-AU binary | journal=Science | volume=345 | issue=6192 | date=3 July 2014 | issn=0036-8075 | doi=10.1126/science.1251527 | pages=46–49|arxiv=1407.1115|pmid=24994642|bibcode = 2014Sci...345...46G|display-authors=1|quote=these projected separations are good proxies for the semi-major axis (afterupward adjustment by <math> \sqrt{3/2}</math> to correct for projection effects)}}</ref>
| Sumbu semi-mayor OGLE-2013-BLG-0341L b's semi-major axis isadalah 0.,7 AUSA.<ref name="Gould Udalski Shin Porritt pp. 46–49" />
|-
| Perbedaan sumbu semi-mayor terkecil antara planet berturut-turut
| Smallest semi-major axis <!---ratio---> difference between consecutive planets
| [[Kepler-70b]] and [[Kepler-70c]]<ref name=HottestExoplanet />
| [[Kepler-70]]
| 0.0016 AU (about 240,000&nbsp;km)
| DuringSelama closestpendekatan approachterbesarnya, Kepler-70c wouldakan appearmuncul 5 timeskali theukuran sizeBulan ofdi the Moon inlangit Kepler-70b's sky.
|-
| Rasio sumbu semi-mayor terkecil antara planet berturut-turut
| Smallest semi-major axis ratio between consecutive planets
| [[Kepler-36b]] and [[Kepler-36c]]
| [[Kepler-36]]
| 11%
| Kepler-36b anddan c have semimasing-majormasing axesmemiliki ofsumbu semi-mayor 0.,1153 AU anddan 0.,1283 AU respectivelySA, c isberjarak 11% furtherlebih fromjauh stardari thanbintang bdaripada b.
|-
| Perbedaan sumbu semi-mayor terbesar antara planet berturut-turut
| Largest semi-major axis <!---ratio---> difference between consecutive planets
| PTFO 8-8695 / [[CVSO 30]] b and [[CVSO 30]] c
| [[CVSO 30]]
| ~662 AU (about 99,000,000,000&nbsp;km)
| CurrentlySaat ini c isadalah at (least)setidaknya 127 timeskali thepemisahan separation of SunMatahari-Jupiter fromdari b oratau 22 timeskali SunMatahari-NeptuneNeptunus (outerplanet solartata systemsurya planetbagian luar)
|-
| Rasio sumbu semi-mayor terbesar antara planet berturut-turut
| Largest semi-major axis ratio between consecutive planets
| PTFO 8-8695 b / [[CVSO 30]] b and [[CVSO 30]] c
| [[CVSO 30]]
| 7,900,000%
| PTFO 8-8695 b / [[CVSO 30]] b anddan [[CVSO 30]] c have semimasing-majormasing axesmemiliki ofsumbu semi-mayor 0.,0084 AU anddan 662 AU respectively. c isadalah 78,.998 timeskali furtherlebih fromjauh thedari starbintangnya thandaripada b.
|}
 
==Karakteristik bintang==
==Stellar characteristics==
{| class="wikitable" style="text-align:left;"
|-
Baris 293 ⟶ 292:
! style="background:#efefef;"| Notes
|-
| [[Metalisitas]] terbesar
| Highest [[metallicity]]
| {{nowrap|[[HD 126614 Ab]]}}
| {{nowrap|[[HD 126614|HD 126614 A]]}}
| +0.56&nbsp;[[logarithm|dex]]
| Terletak dalam sebuah sistem bintang tripel.
| Located in a triple star system.
|-
| Metalisitas terendah
| Lowest metallicity
| [[Kapteyn b]]
| [[Kapteyn's Star]]
Baris 305 ⟶ 304:
| [[BD+20°2457]] may be the lowest metallicity planet host (<nowiki>[Fe/H]=−1.00</nowiki>), however the proposed planetary system is dynamically unstable.<ref>http://adsabs.harvard.edu/abs/2014MNRAS.439.1176H</ref> After Kapteyn's Star, the next lowest-metallicity system is Kepler-271, at -0.951 dex. Planets were announced around even the extremely low metallicity stars [[HIP 13044]] and [[HIP 11952]], however these claims have since been disproven.<ref>http://adsabs.harvard.edu/abs/2014A&A...562A.129J</ref>
|-
| Massa bintang terbesar
| Highest stellar mass
| {{nowrap|[[HD 13189 b]]}}<ref name=XPE13189-2010-11-28>{{cite encyclopedia | title=Notes for planet HD 13189 b | encyclopedia=The Extrasolar Planets Encyclopaedia | url=http://exoplanet.eu/catalog/hd_13189_b/ | accessdate=2015-09-15}}</ref>
| {{nowrap|[[HD 13189]]}}<ref name=XPE13189-2010-11-28/>
| {{Solar mass|link=y|4.5±2.5}}<ref name=XPE13189-2010-11-28/>
| Margin of error means the star [[NGC 4349-127]] with a stellar mass of {{Solar mass|3.9}} is potentially the most massive known planet-harboring star.<ref>{{cite encyclopedia | title=Notes for planet NGC 4349-127 b | encyclopedia=The Extrasolar Planets Encyclopaedia | url=http://exoplanet.eu/catalog/ngc_4349_no_127_b/| accessdate=2017-08-28| archive-date=2017-08-28| archive-url=https://web.archive.org/web/20170828225846/http://exoplanet.eu/catalog/ngc_4349_no_127_b/| dead-url=yes}}</ref>
[[Mirfak]] ({{Solar mass|8.4}} hypothetically has one planet, but this remains unproven.
The extremely massive stars R66 ({{Solar mass|70}}) and R126 ({{Solar mass|30}}) have protoplanetary disks but it is unknown if there are planets in this system.
|-
| Massa bintang terendah (deret utama)
| Lowest stellar mass (main sequence)
| {{nowrap|[[2MASS J1119-1137]]}}
| {{nowrap|[[2MASS J1119–1137 ]]}}
| {{Solar mass|0.0033}}
| The system 2MASS J1119-1137 AB is a pair of binary rogue planets approximately 3.7 Jupiter masses each.<ref>{{cite encyclopedia | title=Notes for planet 2MASSS J1119-1137 AB | encyclopedia=The Extrasolar Planets Encyclopaedia | url=http://exoplanet.eu/catalog/2mass_j11193254_ab/| accessdate=2017-08-29| archive-date=2017-08-29| archive-url=https://web.archive.org/web/20170829203252/http://exoplanet.eu/catalog/2mass_j11193254_ab/| dead-url=yes}}</ref>
 
The least massive main sequence star with known planets is [[OGLE-2016-BLG-1195L]], at 0.078 {{Solar_mass}}.
|-
|Massa bintang terendah (bintang deret utama)
|Lowest stellar mass (main sequence star)
|[[VHS 1256-1257 b]]
|[[VHS 1256-1257]]
Baris 327 ⟶ 326:
|
|-
| Massa bintang terendah (katai cokelat)
| Lowest stellar mass (brown dwarf)
| {{nowrap|[[2M J044144 b]]}}<ref name=XPE2mj0-2010-11-28>{{cite encyclopedia |author=Schneider, J. |title=Notes for planet 2M J044144 b |encyclopedia=The Extrasolar Planets Encyclopaedia |url=http://exoplanet.eu/planet.php?p1=2M+J044144&p2=b |accessdate=2010-11-28 |url-status=dead |archiveurl=https://web.archive.org/web/20101122054924/http://exoplanet.eu/planet.php?p1=2M+J044144&p2=b |archivedate=22 November 2010 |df=dmy-all }}</ref>
| {{nowrap|[[2M J044144]]}}<ref name=XPE2mj0-2010-11-28/>
Baris 333 ⟶ 332:
|
|-
| Jari-jari bintang terbesar
| Largest stellar radius
| [[R Leonis]] b
| [[R Leonis]]
| {{Solar radius|299 or 320-350}}<ref name=debeck>{{cite journal|bibcode=2010A&A...523A..18D|arxiv=1008.1083|title=Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae|journal=Astronomy and Astrophysics|volume=523|pages=A18|last1=De Beck|first1=E.|last2=Decin|first2=L.|last3=De Koter|first3=A.|last4=Justtanont|first4=K.|last5=Verhoelst|first5=T.|last6=Kemper|first6=F.|last7=Menten|first7=K. M.|year=2010|doi=10.1051/0004-6361/200913771}}</ref><ref name="Fedele et al.">{{Cite journal | arxiv=astro-ph/0411133 | author=Fedele | display-authors=etal | title=The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI | journal=[[Astronomy and Astrophysics]] | volume=431 | issue=3 | pages=1019–1026 | date=2005 | bibcode=2005A&A...431.1019F|doi = 10.1051/0004-6361:20042013 }}</ref>
| Bintang tersebut adalah sebuah [[variabel Mira]].
| Star is a [[Mira variable]].
|-
| Jari-jari bintang terkecil (bintang deret utama)
| Smallest stellar radius (main sequence star)
|[[VB 10 b]]
|[[VB 10]]
Baris 345 ⟶ 344:
|
|-
| Jari-jari bintang terkecil (katai cokelat)
| Smallest stellar radius (brown dwarf)
| [[2M 0746+20 b]]<ref>{{cite web|url=http://exoplanet.eu/catalog/2m_0746+20_b/|title=The Extrasolar Planet Encyclopaedia — 2M 0746+20 b|work=exoplanet.eu|access-date=2020-08-25|archive-date=2019-09-04|archive-url=https://web.archive.org/web/20190904012129/http://exoplanet.eu/catalog/2m_0746+20_b/|dead-url=yes}}</ref>
| [[2M 0746+20]]
| {{Solar radius|0.089 (± 0.003)}}
| Planet'sMassa massplanet issangat verytidak uncertainmenentu atpada 30.,0 (± 25.,0) Mjup.
|-
| SmallestJari-jari stellarbintang radiusterkecil (pulsar)
| [[PSR J1719-1438 b]]<ref>{{cite web|url=http://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=PSR+J1719-1438+b&type=CONFIRMED_PLANET|title=PSR J1719-1438 b|work=caltech.edu}}</ref>
| [[PSR J1719-1438]]
Baris 357 ⟶ 356:
|
|-
| Bintang tertua
| Oldest star
| {{nowrap|[[HD 164922 b]]}}
| {{nowrap|[[HD 164922]]}}<ref name=HD_164922>{{cite encyclopedia|url=http://exoplanet.eu/catalog/hd_164922_b/|encyclopedia=The Extrasolar Planets Encyclopaedia|title=HD 164922 b|accessdate=2012-12-19}}</ref>
| 13.4 billionmiliar yearstahun<ref name=HD_164922 />
|
|-
| HottestBintang starterpanas withdengan asebuah planet
| {{nowrap|[[NY Vir b|NY Virginis b]]}}
| {{nowrap|[[NY Virginis]]}}<ref>{{cite web|url=http://sciencythoughts.blogspot.com/2011/12/planets-in-ny-virginis-system.html|title=Sciency Thoughts: Planets in the NY Virginis system.|author=Joe Bauwens|work=sciencythoughts.blogspot.com|date=2011-12-29}}</ref>
| 33,247 K
| ThisBintang startersebut isadalah asebuah [[subdwarfbintang Bsubkatai starB]] anddan hasmemiliki apasangan redkatai dwarf companion ofmerah 0.,14 solarmassa massesmatahari withdengan asumbu semi-majormayor axissedikit ofdi slightly underbawah 4 millionjuta kilometerskilometer fromdari thekomponen primary componentutama. TheSistem [[NN Serpentis]] systemmemiliki hasdua two exoplanetseksoplanet (NN Serpentis c anddan NN Serpentis d), withdengan thebintang star atpada ~57,.000K.
|-
| HottestBintang main-sequencederet starutama withterpanas adengan sebuah planet
| {{nowrap|[[Fomalhaut b]]}}
| {{nowrap|[[Fomalhaut]]}}<ref name=Fomalhaut>{{cite encyclopedia|encyclopedia=The Extrasolar Planets Encyclopaedia |url=http://exoplanet.eu/catalog/fomalhaut_b/ |title=Fomalhaut b|accessdate=2013-03-30}}</ref>
| 8,590 K
| HIP 78530 hasmemiliki asuhu surface temperature ofpermukaan 10,.500K, but ittetapi istidak uncertainpasti whetherapakah thependamping orbitingyang companionmengorbitnya isadalah asebuah brownkatai dwarfcoklat oratau planet.
|-
| ColdestBintang starterdingin withdengan asebuah planet
| [[TRAPPIST-1b]], [[TRAPPIST-1c|c]], [[TRAPPIST-1d|d]], [[TRAPPIST-1e|e]], [[TRAPPIST-1f|f]], [[TRAPPIST-1g|g]], anddan [[TRAPPIST-1h|h]].
| [[TRAPPIST-1]]
| 2,511 K
| TechnicallySecara teknis [[Oph 162225-240515 b|Oph 162225-240515]], [[CFBDSIR J145829+101343 b|CFBDSIR J145829+101343]], anddan [[WISE 1217+1626 b|WISE 1217+1626]] arelebih colderdingin, buttetapi aremereka classifieddiklasifikasikan assebagai brownkatai dwarfscoklat.
|}
 
==Karakteristik sistem==
==System characteristics==
{| class="wikitable"
|-
Baris 391 ⟶ 390:
! Notes
|-
| Sistem dengan planet terbanyak
| System with most planets
|[[Kepler-90]]
| 8<ref>{{Cite news|url=https://www.nasa.gov/press-release/artificial-intelligence-nasa-data-used-to-discover-eighth-planet-circling-distant-star|title=Artificial Intelligence, NASA Data Used to Discover Exoplanet|last=Northon|first=Karen|date=2017-12-14|work=NASA|access-date=2017-12-14}}</ref>
| 1
| StarBintang HD 10180 hasmemiliki 7 confirmedplanet andyang dikonfirmasi dan 2 unconfirmedplanet yang belum planetsterkonfirmasi.<ref name=HD_10180_i>{{cite encyclopedia|encyclopedia=The Extrasolar Planets Encyclopaedia|url=http://exoplanet.eu/catalog/hd_10180_i/|title=HD 10180 i|accessdate=2012-12-24}}</ref><ref name=HD_10180_j>{{cite encyclopedia|encyclopedia=The Extrasolar Planets Encyclopaedia|title=HD 10180 j|url=http://exoplanet.eu/catalog/hd_10180_j/|accessdate=2012-12-24}}</ref>
|-
|Sistem dengan planet terbanyak dalam zona laik huni
|System with most planets in habitable zone
|[[TRAPPIST-1]]
|7
|1
|ThreeTiga planetsplanet indalam thissistem systemtersebut (''e'', ''f'' anddan ''g'') orbitmengorbit within thedalam [[habitablezona laik zonehuni]].<ref>{{Cite web|url=https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/|title=NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star|work=Exoplanet Exploration: Planets Beyond our Solar System|access-date=2017-12-14 |date=21 February 2017 |publisher=nasa.gov}}</ref>
|-
| Sistem dengan bintang terbanyak
| System with most stars
| Kepler 64
| [[PH1b]] (Kepler 64b)
| 4
| PH1 hasmemiliki a circumbinarysebuah orbit lingkar bintang.
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terkecil (planet yang terdekat dengan bintangnya)
| Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star)
| Kepler 42<br>Kepler 70
| b, [[Kepler-42c|c]], d<br>[[Kepler-70b|b]], [[Kepler-70c|c]], d?
| 1<br>1
| Kepler-42 b, c, anddan d havemasing-masing amemiliki semimajorsumbu axissemimayor of onlyhanya 0.,0116, 0.,006, anddan 0.,0154 AU, respectively.<br>Kepler-70 b, c, anddan d (unconfirmedbelum dikonfirmasi) have amasing-masing semimajormemiliki axissumbu ofsemimayor onlyhanya 0.,006, 0.,0076, anddan ~0.,0065 AU, respectively.
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terbesar (planet yang terjauh dari bintangnya)
| Multiplanetary system with largest mean semi-major axis (planets are farthest from their star)
| [[HR 8799]]
| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]
| 1
| HR 8799 b, c, d, anddan e havemasing-masing amemiliki semimajorsumbu axis ofsemimayor 68, 38, 24, anddan 14.5 AU, respectively.
|-
| Sistem multiplanet dengan jarak sumbu semi-mayor terkecil (perbedaan terkecil antara planet terdekat dari bintang dan planet terjauh)
| Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet)
| Kepler-70
| [[Kepler-70b|b]], [[Kepler-70c|c]], d?
| 1
| Kepler-70 b, c, anddan d (unconfirmedbelum dikonfirmasi) havemasing-masing amemiliki semimajorsumbu axissemimayor of onlyhanya 0.,006, 0.,0076, anddan ~0.,0065 AU, respectively. TheJarak separationantara betweenyang closestterdekat anddan furthestterjauh is onlyhanya 0.,0016 AU.
|-
| Sistem multiplanet dengan jarak sumbu semi-mayor terbesar (perbedaan terbesar antara planet terdekat dari bintang dan planet terjauh)
| Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet)
| [[HR 8799]]
| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]
| 1
| HR 8799 b, c, d, anddan e havemasing-masing amemiliki semimajorsumbu axis ofsemimayor 68, 38, 24, anddan 14.5 AU, respectivelySA. TheJarak separationantara betweenyang closestterdekat anddan furthestterjauh isadalah 53.,5 AUSA.
|-
| Sistem multiplanet dengan perbedaan rata-rata terkecil dalam sumbu semi-mayor antar planet tetangga (jarak orbit paling dekat satu sama lain)
| Multiplanetary system with smallest mean difference in semi-major axis between neighboring planets (orbits are most closely spaced to each other)
|
|
Baris 439 ⟶ 438:
|
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terbesar di antara planet-planet tetangga (orbit paling tersebar satu sama lain)
| Multiplanetary system with largest mean semi-major axis between neighboring planets (orbits are most spread out with respect to each other)
|
|
Baris 445 ⟶ 444:
|
|-
| Sistem dengan massa planet total terkecil
| System with smallest total planetary mass
| [[Kepler-444]]
| b, c, d, e, f
Baris 451 ⟶ 450:
| The planets in the [[Kepler-444]] 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 [[Mars]]. For comparison, [[Mars]] has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
|-
| Sistem dengan massa planet total terbesar
| System with largest total planetary mass
| Kepler-52?
| b, c, d
| 1
| Kepler-52 b anddan c havemasing-masing massesmemiliki ofmassa 8.,7 anddan 10.,41 Massa Jupiter Masses, respectively. The mass ofMassa Kepler-52 d is nottidak knowndiketahui.
|-
| SystemSistem withdengan smallestrasio ratiomassa ofplanet total planetaryterkecil mass toterhadap stellarmassa massbintang
|
|
Baris 463 ⟶ 462:
|
|-
| Sistem dengan rasio massa planet total terbesar terhadap massa bintang
| System with largest ratio of total planetary mass to stellar mass
|
|
Baris 469 ⟶ 468:
|
|-
| Sistem multiplanet dengan rata-rata massa planet terkecil
| Multiplanetary system with smallest mean planetary mass
| [[Kepler-444]]
| b, c, d, e, f
| 1
| The planetsPlanet-planet indalam thesistem [[Kepler-444]] systemmasing-masing havememiliki radii ofjari-jari 0.,4, 0.,497, 0.,53, 0.,546, anddan 0.,741 Earth radiijari-jari respectivelyBumi. DueKarena toukuran theirdan sizekedekatannya and proximity todengan Kepler-444, thesemereka mustdipastikan beplanet rocky planetsberbatu, with masses closedengan tomassa thatyang ofmendekati [[Mars]]. ForSebagai comparisonperbandingan, [[Mars]] hasmemiliki a mass ofmassa 0.,105 Earthmassa massesBumi and adan radius of 0.,53 Earthjari-jari radiiBumi.
|-
| Sistem multiplanet dengan rasio massa planet rata-rata terkecil terhadap massa bintang
| Multiplanetary system with smallest ratio of mean planetary mass to stellar mass
|
|
Baris 481 ⟶ 480:
|
|-
| Sistem multiplanet dengan rata-rata massa planet terbesar
| Multiplanetary system with largest mean planetary mass
| Kepler-52?
| b, c, d
| 1
| Kepler-52 b anddan c havemasing-masing massesmemiliki ofmassa 8.,7 anddan 10.,41 Massa Jupiter Masses, respectively. The mass ofMassa Kepler-52 d is nottidak knowndiketahui.
|-
| Multiplanetary system with largest ratio of mean planetary mass to stellar mass
Baris 493 ⟶ 492:
|
|-
| Sistem multiplanet dengan jarak terkecil dalam massa planet, skala log (perbedaan proporsional terkecil antara planet paling masif dan paling kecil)
| Multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets)
| [[Bintang Teegarden's Star]]
| b, c
| 1
| [[Teegarden b]] anddan [[Teegarden c|c]] arediperkirakan estimatedmemiliki tomassa have masses ofmasing-masing 1.,05 anddan 1.,11 Earth masses,massa respectivelyBumi.
|-
| Sistem multiplanet dengan jarak terbesar dalam massa planet, skala log (perbedaan proporsional terbesar antara planet paling masif dan paling kecil)
| Multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets)
| [[SolarTata SystemSurya]]
| MercuryMerkurius, Jupiter
| 1
| [[Mercury (planet)|MercuryMerkurius]] anddan [[Jupiter]] havememiliki arasio mass ratio ofmassa 5,750 tobanding 1. [[Kepler-37]] d anddan b maykemungkinan havememiliki arasio massmassa ratio betweenantara 500 anddan 1000, anddan [[Gliese 676]] c anddan d have a massmemiliki ratiorasio ofmassa 491.
|}
 
Baris 511 ⟶ 510:
* [[Daftar bintang dengan proplid]]
* [[Metode pendeteksian eksoplanet]]
* [[Eksoplanet paling serupa Bumi|Eksoplanet ekstrakebumiankebumian]]
 
==Catatan==
Baris 525 ⟶ 524:
 
{{DEFAULTSORT:Daftar Keekstreman Planet Ekstrasurya}}
[[CategoryKategori:Sistem keplanetan|*Keesktreman planet]]
[[CategoryKategori:Daftar bintang|Keekstreman planet ekstrasurya]]
[[CategoryKategori:Daftar superlatif dalam astronomi|Planet ekstrasurya ekstrem]]
[[CategoryKategori:Daftar eksoplanet|Ekstrem]]
[[CategoryKategori:Daftar titik ekstrem|eksoplanet]]
Diperoleh dari "https://wiki-indonesia.club/wiki/Daftar_eksoplanet_ekstrem"