Lihat sumber Daftar eksoplanet ekstrem

{{short description|artikel daftar Wikipedia}}
Berikut ini adalah daftar keesktreman di antara [[eksoplanet]] yang diketahui. Properti yang tercantum di sini adalah properti yang nilainya diketahui secara terpercaya.

== Ekstrem dari sudut pandang Bumi ==
{| class="wikitable"
|-
! Judul
! Planet
! Bintang
! Data
! Catatan
|-
| Paling jauh ditemukan
| [[SWEEPS-11]] / [[SWEEPS-04]]
| SWEEPS J175902.67−291153.5
| 27,710 tahun cahaya.<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>
| Sebuah analisis kurva cahaya dari peristiwa pelensaan mikro [[PA-99-N2]] menunjukkan adanya sebuah planet yang mengorbit bintang di [[Galaksi Andromeda]] (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> Pada akhir Januari 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> sebuah tim ilmuwan yang dipimpin oleh Xinyu Dai mengklaim telah menemukan kumpulan sekitar 2.000 [[planet pengembara]] di mikrolensa [[kuasar]] [[RX J1131-1231]], yang berjarak 3,8 miliar tahun cahaya. Massa benda-benda tersebut berkisar dari Bulan hingga beberapa massa Jupiter.<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" /> 
Planet paling jauh yang berpotensi dapat dihuni yang dikonfirmasi adalah Kepler-443b, pada jarak 2.540 tahun cahaya,<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> meskipun planet [[KOI-5889.01]] yang belum dikonfirmasi berjarak lebih dari 5.000 tahun cahaya.
|-
| Terdekat
| {{nowrap|[[Proxima Centauri b]]}} dan c
| {{nowrap|[[Proxima Centauri]]}}
| 4.22 tahun cahaya
| Proxima Centauri b adalah eksoplanet berbatu terdekat dan [[Daftar eksoplanet yang berpotensi laik huni|eksoplanet terdekat yang berpotensi dihuni]], dan c adalah super-Bumi terdekat dan planet yang berpotensi memiliki cincin. Karena Proxima Centauri adalah bintang terdekat dengan Matahari (dan akan tetap demikian selama 25.000 tahun ke depan), ini adalah sebuah rekor mutlak.
|-
| Terlihat secara langsung paling jauh
| [[CVSO 30]] c
| [[CVSO 30]]
| 1,200 [[light year|tahun cahaya]]
| Juga pertama kali mencitrakan planet secara langsung dalam sistem dengan sebuah planet transit.
|-
| Terlihat secara langsung paling tidak jauh
| [[Proxima Centauri c]]
| [[Proxima Centauri]]
| 4.22 [[tahun cahaya]]
| Dikonfirmasi pada 2020 menggunakan data arsip Hubble dari tahun 1995+.
|-
| Bintang dengan [[magnitudo tampak]] paling terang dengan sebuah 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>
| Magnitudo tampak adalah 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>

<!-- --uncomment this when this is filled out--
| Star with the faintest apparent magnitude with a planet
| //planet name here//
| //star name here//
| //number here//
| //notes here//
-->
|-
| Pemisahan [[jarak sudut]] terbesar dari bintang induknya
| [[GU Piscium b]]
| [[GU Piscium]]
| 42 detik ark<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--
| Smallest angular distance separation from its parent star
| //planet name here//
| //star name here//
| //number here//
| //notes here//
-->
|}

==Karakteristik keplanetan==
{| class="wikitable"
|-
! Judul
! Planet
! Bintang
! Data
! Catatan
|-

| Paling tidak masif
|[[WD 1145+017 b]]
|[[WD 1145+017]] 
| 0.00067&nbsp;[[Earth mass|M<sub>Earth</sub>]]<ref name=":0">{{Cite web|url=http://exoplanet.eu/catalog/|title=The Extrasolar Planet Encyclopaedia — Catalog Listing|website=exoplanet.eu|access-date=2019-05-04}}</ref>
| 
|-
| Paling masif
| colspan="4" |Kandidat planet paling masif masih diperdebatkan, karena sulit untuk menentukan antara sebuah planet yang sangat masif dan sebuah [[katai coklat]]. Planet terbesar diperkirakan berukuran sekitar selusin massa [[Jupiter]].
|-
| Jari-jari terbesar
| [[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
| Eksoplanet terbesar dalam [[NASA Exoplanet Archive]], meskipun karena fluks dari planet dan cakram yang ditumpangkan, ukuran pasti planet tersebut tidak dapat ditentukan dan wilayah pemancarannya memiliki ukuran tersebut, terdiri dari planet dan termasuk cakramnya, bukan untuk disalahartikan sebagai sebuah jari-jari planet tunggal. Seiring waktu, planet tersebut akan menyusut menjadi seukuran Jupiter. 20 MJ; kemungkinan adalah sebuah katai coklat.
|-
| Jari-jari terpendek
|[[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>
|
|-
| Paling rapat
|[[K2-38b]]
|[[K2-38]]
| {{val|17.5|+8.5|-6.2}} g/cm<sup>3</sup><ref>{{Cite web|title=K2-38 b|url=https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=K2-38+b&type=CONFIRMED_PLANET|access-date=2020-06-14|website=exoplanetarchive.ipac.caltech.edu}}</ref>
| 
|-
| Paling tidak rapat
| [[Kepler-51c]], [[Kepler-51b|b]] dan/atau kemungkinan [[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
| {{nowrap| [[Kepler-70b]] }}
| {{nowrap| [[Kepler-70]] }}
| >7,000 [[Kelvin|K]]<ref name=HottestExoplanet>{{cite journal | last=Charpinet | first=S. | last2=Fontaine | first2=G. | last3=Brassard | first3=P. | last4=Green | first4=E. M. | last5=Grootel | first5=V. Van | last6=Randall | first6=S. K. | last7=Silvotti | first7=R. | last8=Baran | first8=A. S. | author9= stensen | last10=Kawaler | first10=S. D. | last11=Telting | first11=J. H. | title=A compact system of small planets around a former red-giant star | journal=Nature | volume=480 | issue=7378 | date=21 December 2011 | issn=1476-4687 | doi=10.1038/nature10631 |pmid=22193103|pages=496–499|bibcode = 2011Natur.480..496C |display-authors=1}}</ref>
| 
|-
| Terdingin
| {{nowrap| [[OGLE-2016-BLG-1195Lb]] }}
| {{nowrap| [[OGLE-2016-BLG-1195L]] }}
| 31&nbsp;[[Kelvin|K]]
| 
|-
| [[Albedo]] terbesar
| [[Kepler-10b]]{{citation needed|date=March 2014}}
| [[Kepler-10]]
| 0.5–0.6 (albedo geometrik)
|
|-
| Albedo terendah
| {{nowrap|[[TrES-2b]]}}
| {{nowrap|[[GSC 03549-02811]]}}
| [[Albedo geometrik]] {{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
|[[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>
|Batas massa yang lebih tinggi (13 massa Jupiter) dapat menjadikannya katai coklat.
|-
| Tertua
| {{nowrap| [[PSR B1620-26 b]] }}
| {{nowrap| [[PSR B1620-26]] }}
| 13&nbsp;[[Gigatahun|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==
{| class="wikitable" style="text-align:left;"
|-
! style="background:#efefef;"| Title
! style="background:#efefef;"| Planet
! style="background:#efefef;"| Star
! style="background:#efefef;"| Data
! style="background:#efefef;"| Notes
|-
| Periode [[orbit]] terlama <br/> <small>(Tahun terlama)</small>
| [[2MASS J2126-8140]]
| [[TYC 9486-927-1]]
| <!---... days-->~1,000,000 tahun
| [[GU Piscium b]] previously held record at<!---... days--> 163,000 years.
|-
| Periode orbit terpendek<br/> <small>(Tahun terpendek)</small>
| {{nowrap|[[SWIFT J1756.9-2508 b]]}}
| {{nowrap|[[SWIFT J1756.9-2508]]}}
| {{nowrap|48 menit, 56.5 detik}}<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]] memiliki orbit terpendek di sekitar sebuah bintang deret utama (katai M) pada 4,31 jam.<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]]
| {{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
| Least eccentric orbit
| {{nowrap|[[HD 209458 b]]}}
| {{nowrap|[[HD 209458]]}}
| eccentricity of 0.014±0.009
-->
|-
<!-- --uncomment this when this is filled out--
| Most inclined retrograde orbit
| //planet name here//
| //star name here//
| //orbital inclination here//
| //notes here//
-->
|-
<!-- --uncomment this when this is filled out--
| Most inclined prograde orbit
| //planet name here//
| //star name here//
| //orbital inclination here//
| //notes here//
|-
-->
<!-- --uncomment this when this is filled out--
| Least inclined retrograde orbit
| //planet name here//
| //star name here//
| //orbital inclination here//
| //notes here//
-->
|-
<!-- --uncomment this when this is filled out--
| Least inclined prograde orbit
| //planet name here//
| //star name here//
| //orbital inclination here//
| //notes here//
-->
|-
| Orbit terbesar di sekitar sebuah bintang tunggal
| {{nowrap|[[2MASS J2126-8140]]}}
| {{nowrap|[[TYC 9486-927-1]]}}
| ~5,800&nbsp;AU
| 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
| {{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]]}}
| 0.0021 AU
| 
|-
| Orbit terkecil di sekitar bintang biner
| {{nowrap|[[Kepler-47b]]}}
| {{nowrap|[[Kepler-47]]AB}}
| ≃0.3 AU
|<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>
|-
| Rasio terkecil [[sumbu semi-mayor]] dari sebuah planet yang mengorbit dengan orbit bintang biner
| {{nowrap|[[Kepler-16b]]}}
| {{nowrap|[[Kepler-16]]AB}}
| 3.14 ± 0.01
|<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
| {{nowrap|[[DT Virginis c]]}}
| {{nowrap|[[DT Virginis]]}}
| 1,168 AU
| Sistem bintang tersebut juga dikenal sebagai Ross 458 AB. Planet tersebut akhirnya dipastikan berada di bawah batas pembakaran deuterium tetapi asal pembentukannya tidak diketahui.
|-
| Orbit terbesar di sekitar sebuah bintang tunggal dalam sistem bintang ganda
| {{nowrap|[[Fomalhaut b]]}}
| {{nowrap|[[Fomalhaut]]}}
| 115 AU
| 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
| [[FW Tauri AB b]]
| [[FW Tau AB]]
| ≈11 AU
| FW Tauri AB b mengorbit pada jarak 150-300 SA.<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>
|-
| Orbit terdekat antara bintang dengan sebuah planet yang mengorbit salah satu bintang
| {{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 adalah 0,7 SA.<ref name="Gould Udalski Shin Porritt pp. 46–49" />
|-
| Perbedaan sumbu semi-mayor terkecil antara planet berturut-turut
| [[Kepler-70b]] and [[Kepler-70c]]<ref name=HottestExoplanet />
| [[Kepler-70]]
| 0.0016 AU (about 240,000&nbsp;km)
| Selama pendekatan terbesarnya, Kepler-70c akan muncul 5 kali ukuran Bulan di langit Kepler-70b.
|-
| Rasio sumbu semi-mayor terkecil antara planet berturut-turut
| [[Kepler-36b]] and [[Kepler-36c]]
| [[Kepler-36]]
| 11%
| Kepler-36b dan c masing-masing memiliki sumbu semi-mayor 0,1153 AU dan 0,1283 SA, c berjarak 11% lebih jauh dari bintang daripada b.
|-
| Perbedaan sumbu semi-mayor terbesar antara planet berturut-turut
| PTFO 8-8695 / [[CVSO 30]] b and [[CVSO 30]] c
| [[CVSO 30]]
| ~662 AU (about 99,000,000,000&nbsp;km)
| Saat ini c adalah setidaknya 127 kali pemisahan Matahari-Jupiter dari b atau 22 kali Matahari-Neptunus (planet tata surya bagian luar)
|-
| Rasio sumbu semi-mayor terbesar antara planet berturut-turut
| PTFO 8-8695 b / [[CVSO 30]] b and [[CVSO 30]] c
| [[CVSO 30]]
| 7,900,000%
| PTFO 8-8695 b / [[CVSO 30]] b dan CVSO 30 c masing-masing memiliki sumbu semi-mayor 0,0084 AU dan 662 AU. c adalah 78.998 kali lebih jauh dari bintangnya daripada b.
|}

==Karakteristik bintang==
{| class="wikitable" style="text-align:left;"
|-
! style="background:#efefef;"| Title
! style="background:#efefef;"| Planet
! style="background:#efefef;"| Star
! style="background:#efefef;"| Data 
! style="background:#efefef;"| Notes
|-
| [[Metalisitas]] terbesar
| {{nowrap|[[HD 126614 Ab]]}}
| {{nowrap|[[HD 126614|HD 126614 A]]}}
| +0.56&nbsp;[[logarithm|dex]]
| Terletak dalam sebuah sistem bintang tripel.
|-
| Metalisitas terendah
| [[Kapteyn b]]
| [[Kapteyn's Star]]
| −0.99±0.04&nbsp;[[logarithm|dex]]
| [[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
| {{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)
| {{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)
|[[VHS 1256-1257 b]]
|[[VHS 1256-1257]]
|{{Solar mass|0.07}}
|
|-
| Massa bintang terendah (katai cokelat)
| {{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/>
| {{Solar mass|0.02}}<ref name=XPE2mj0-2010-11-28/>
|
|-
| Jari-jari bintang terbesar
| [[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]].
|-
| Jari-jari bintang terkecil (bintang deret utama)
|[[VB 10 b]]
|[[VB 10]]
| {{Solar radius|0.102}}<ref>{{Cite journal|last=Linsky|first=Jeffrey L.|last2=Wood|first2=Brian E.|last3=Brown|first3=Alexander|last4=Giampapa|first4=Mark S.|last5=Ambruster|first5=Carol|date=December 1995|title=Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10|journal=The Astrophysical Journal|volume=455|pages=670|doi=10.1086/176614|issn=0004-637X|bibcode=1995ApJ...455..670L|hdl=2060/19970022983|hdl-access=free}}</ref>
|
|-
| Jari-jari bintang terkecil (katai cokelat)
| [[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)}}
| Massa planet sangat tidak menentu pada 30,0 (± 25,0) Mjup.
|-
| Jari-jari bintang terkecil (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]] 
| {{Solar radius|0.04}}
| 
|-
| Bintang tertua
| {{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 miliar tahun<ref name=HD_164922 />
|  
|-
| Bintang terpanas dengan sebuah 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
| Bintang tersebut adalah sebuah [[bintang subkatai B]] dan memiliki pasangan katai merah 0,14 massa matahari dengan sumbu semi-mayor sedikit di bawah 4 juta kilometer dari komponen utama. Sistem [[NN Serpentis]] memiliki dua eksoplanet (NN Serpentis c dan NN Serpentis d), dengan bintang pada ~57.000K.
|-
| Bintang deret utama terpanas dengan 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 memiliki suhu permukaan 10.500K, tetapi tidak pasti apakah pendamping yang mengorbitnya adalah sebuah katai coklat atau planet.
|-
| Bintang terdingin dengan sebuah planet
| [[TRAPPIST-1b]], [[TRAPPIST-1c|c]], [[TRAPPIST-1d|d]], [[TRAPPIST-1e|e]], [[TRAPPIST-1f|f]], [[TRAPPIST-1g|g]], dan [[TRAPPIST-1h|h]].
| [[TRAPPIST-1]] 
| 2,511 K
| Secara teknis [[Oph 162225-240515 b|Oph 162225-240515]], [[CFBDSIR J145829+101343 b|CFBDSIR J145829+101343]], dan [[WISE 1217+1626 b|WISE 1217+1626]] lebih dingin, tetapi mereka diklasifikasikan sebagai katai coklat.
|}

==Karakteristik sistem==
{| class="wikitable"
|-
! Title
! System(s)
! Planet(s)
! Star(s)
! Notes
|-
| Sistem dengan planet terbanyak
|[[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
| Bintang HD 10180 memiliki 7 planet yang dikonfirmasi dan 2 planet yang belum terkonfirmasi.<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
|[[TRAPPIST-1]]
|7
|1
|Tiga planet dalam sistem tersebut (''e'', ''f'' dan ''g'') mengorbit dalam [[zona laik huni]].<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
| Kepler 64
| [[PH1b]] (Kepler 64b)
| 4
| PH1 memiliki sebuah orbit lingkar bintang.
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terkecil (planet yang terdekat dengan bintangnya)
| 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, dan d masing-masing memiliki sumbu semimayor hanya 0,0116, 0,006, dan 0,0154 AU.<br>Kepler-70 b, c, dan d (belum dikonfirmasi) masing-masing memiliki sumbu semimayor hanya 0,006, 0,0076, dan ~0,0065 AU.
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terbesar (planet yang terjauh dari bintangnya)
| [[HR 8799]]
| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]
| 1
| HR 8799 b, c, d, dan e masing-masing memiliki sumbu semimayor 68, 38, 24, dan 14.5 AU.
|-
| Sistem multiplanet dengan jarak sumbu semi-mayor terkecil (perbedaan terkecil antara planet terdekat dari bintang dan planet terjauh)
| Kepler-70
| [[Kepler-70b|b]], [[Kepler-70c|c]], d?
| 1
| Kepler-70 b, c, dan d (belum dikonfirmasi) masing-masing memiliki sumbu semimayor hanya 0,006, 0,0076, dan ~0,0065 AU. Jarak antara yang terdekat dan terjauh hanya 0,0016 AU.
|-
| Sistem multiplanet dengan jarak sumbu semi-mayor terbesar (perbedaan terbesar antara planet terdekat dari bintang dan planet terjauh)
| [[HR 8799]]
| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]
| 1
| HR 8799 b, c, d, dan e masing-masing memiliki sumbu semimayor 68, 38, 24, dan 14.5 SA. Jarak antara yang terdekat dan terjauh adalah 53,5 SA.
|-
| Sistem multiplanet dengan perbedaan rata-rata terkecil dalam sumbu semi-mayor antar planet tetangga (jarak orbit paling dekat satu sama lain)
|  
| 
| 
| 
|-
| Sistem multiplanet dengan sumbu semi-mayor rata-rata terbesar di antara planet-planet tetangga (orbit paling tersebar satu sama lain)
|  
| 
| 
| 
|-
| Sistem dengan massa planet total terkecil
| [[Kepler-444]]
| b, c, d, e, f
| 1
| 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
| Kepler-52?
| b, c, d
| 1
| Kepler-52 b dan c masing-masing memiliki massa 8,7 dan 10,41 Massa Jupiter. Massa Kepler-52 d tidak diketahui.
|-
| Sistem dengan rasio massa planet total terkecil  terhadap massa bintang
|  
| 
| 
| 
|-
| Sistem dengan rasio massa planet total terbesar terhadap massa bintang
|  
| 
| 
| 
|-
| Sistem multiplanet dengan rata-rata massa planet terkecil
| [[Kepler-444]]
| b, c, d, e, f
| 1
| Planet-planet dalam sistem [[Kepler-444]] masing-masing memiliki jari-jari 0,4, 0,497, 0,53, 0,546, dan 0,741 jari-jari Bumi. Karena ukuran dan kedekatannya dengan Kepler-444, mereka dipastikan planet berbatu, dengan massa yang mendekati [[Mars]]. Sebagai perbandingan, Mars memiliki massa 0,105 massa Bumi dan radius 0,53 jari-jari Bumi.
|-
| Sistem multiplanet dengan rasio massa planet rata-rata terkecil terhadap massa bintang
|  
| 
| 
| 
|-
| Sistem multiplanet dengan rata-rata massa planet terbesar
| Kepler-52?
| b, c, d
| 1
| Kepler-52 b dan c masing-masing memiliki massa 8,7 dan 10,41 Massa Jupiter. Massa Kepler-52 d tidak diketahui.
|-
| Multiplanetary system with largest ratio of mean planetary mass to stellar mass 
|  
| 
| 
| 
|-
| Sistem multiplanet dengan jarak terkecil dalam massa planet, skala log (perbedaan proporsional terkecil antara planet paling masif dan paling kecil)
| [[Bintang Teegarden]]
| b, c
| 1
| [[Teegarden b]] dan [[Teegarden c|c]] diperkirakan memiliki massa masing-masing 1,05 dan 1,11 massa Bumi.
|-
| Sistem multiplanet dengan jarak terbesar dalam massa planet, skala log (perbedaan proporsional terbesar antara planet paling masif dan paling kecil)
| [[Tata Surya]]
| Merkurius, Jupiter
| 1
| [[Merkurius]] dan [[Jupiter]] memiliki rasio massa 5,750 banding 1. [[Kepler-37]] d dan b kemungkinan memiliki rasio massa antara 500 dan 1000, dan [[Gliese 676]] c dan d memiliki rasio massa 491.
|}

==Lihat pula==
* [[Keesktreman di Bumi]]
* [[Daftar daftar eksoplanet]]
* [[Daftar bintang dengan proplid]]
* [[Metode pendeteksian eksoplanet]]
* [[Eksoplanet paling serupa Bumi|Eksoplanet kebumian]]

==Catatan==
{{reflist|group=note}}

==Referensi==
{{reflist}}

==Pranala luar==
* WiredScience, [https://www.wired.com/wiredscience/2009/01/top-exoplanets/ Top 5 Most Extreme Exoplanets],  Clara Moskowitz, 21 January 2009

{{exoplanet}}

{{DEFAULTSORT:Daftar Keekstreman Planet Ekstrasurya}}
[[Kategori:Sistem keplanetan|*Keesktreman planet]]
[[Kategori:Daftar bintang|Keekstreman planet ekstrasurya]]
[[Kategori:Daftar superlatif dalam astronomi|Planet ekstrasurya ekstrem]]
[[Kategori:Daftar eksoplanet|Ekstrem]]
[[Kategori:Daftar titik ekstrem|eksoplanet]]