Daftar eksoplanet ekstrem: Perbedaan antara revisi

| [[SWEEPS-11]] / [[SWEEPS-04]]

| SWEEPS J175902.67−291153.5

|-

| Terdekat

| {{nowrap|[[Proxima Centauri]]}}

| 4.22 tahun cahaya

|-

| Terlihat secara langsung paling jauh

| [[CVSO 30]]

| 1,200 [[light year|tahun cahaya]]

|-

| Terlihat secara langsung paling tidak jauh

| [[Proxima Centauri]]

| 4.22 [[tahun cahaya]]

|-

| 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>

| 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>

 

| [[GU Piscium b]]

| [[GU Piscium]]

| 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.

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|-

| Paling masif

|-

| Jari-jari terbesar

| [[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

|-

| Jari-jari terpendek

|[[SDSS J1228+1040 b]]

|

|-

|-

| Paling tidak rapat

| [[Kepler-51]]<ref name="Masuda" />

| ~ 0.03 g/cm³<ref name="Masuda" />

| [[Kepler-10b]]{{citation needed|date=March 2014}}

| [[Kepler-10]]

|

|-

| {{nowrap|[[TrES-2b]]}}

| {{nowrap|[[GSC 03549-02811]]}}

| Best-fit model for albedo gives 0.04% (0.0004)<ref name=darkest/>

|-

|[[Proplyd 133-353]]

|[[Proplyd 133-353]]

|-

| Tertua

| {{nowrap| [[PSR B1620-26 b]] }}

| {{nowrap| [[PSR B1620-26]] }}

| 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>

|}

| [[2MASS J2126-8140]]

| [[TYC 9486-927-1]]

| [[GU Piscium b]] previously held record at<!---... days--> 163,000 years.

|-

| {{nowrap|[[SWIFT J1756.9-2508 b]]}}

| {{nowrap|[[SWIFT J1756.9-2508]]}}

|-

| [[Eksentrisitas orbit|Orbit tereksentrik]]

| [[HD 20782]]

| {{val|0.956|0.004}}

|-

<!-- "Least eccentric" makes no sense: there are *many* planets with e = 0 measurements

| {{nowrap|[[DT Virginis]]}}

| 1,168 AU

|-

| Orbit terbesar di sekitar sebuah bintang tunggal dalam sistem bintang ganda

| [[FW Tau AB]]

| ≈11 AU

|-

| Orbit terdekat antara bintang dengan sebuah planet yang mengorbit salah satu bintang

| {{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>

|-

| Perbedaan sumbu semi-mayor terkecil antara planet berturut-turut

| [[Kepler-70]]

| 0.0016 AU (about 240,000&nbsp;km)

|-

| Rasio sumbu semi-mayor terkecil antara planet berturut-turut

| [[Kepler-36]]

| 11%

|-

| Perbedaan sumbu semi-mayor terbesar antara planet berturut-turut

| [[CVSO 30]]

| ~662 AU (about 99,000,000,000&nbsp;km)

|-

| Rasio sumbu semi-mayor terbesar antara planet berturut-turut

| [[CVSO 30]]

| 7,900,000%

|}

 

| {{nowrap|[[HD 126614|HD 126614 A]]}}

| +0.56&nbsp;[[logarithm|dex]]

|-

| Metalisitas terendah

| {{nowrap|[[HD 13189]]}}<ref name=XPE13189-2010-11-28/>

| {{Solar mass|link=y|4.5±2.5}}<ref name=XPE13189-2010-11-28/>

[[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.

| {{nowrap|[[2MASS J1119–1137 ]]}}

| {{Solar mass|0.0033}}

 

The least massive main sequence star with known planets is [[OGLE-2016-BLG-1195L]], at 0.078 {{Solar_mass}}.

| [[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>

|-

| Jari-jari bintang terkecil (bintang deret utama)

|-

| Jari-jari bintang terkecil (katai cokelat)

| [[2M 0746+20]]

| {{Solar radius|0.089 (± 0.003)}}

|-

| Jari-jari bintang terkecil (pulsar)

| {{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 deret utama terpanas dengan sebuah planet

|}

 

{| class="wikitable"

|-

|7

|1

|-

| Sistem dengan bintang terbanyak

 

{{DEFAULTSORT:Daftar Keekstreman Planet Ekstrasurya}}