Daftar eksoplanet ekstrem: Perbedaan antara revisi

 

{| class="wikitable"

|-

! Planet

! Data

|-

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

| SWEEPS J175902.67−291153.5

|-

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

|-

| [[CVSO 30]] c

| [[CVSO 30]]

|-

| [[Proxima Centauri c]]

| [[Proxima Centauri]]

|-

| [[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.

<!-- --uncomment this when this is filled out--

|}

 

{| class="wikitable"

|-

! Planet

! Data

|-

 

|[[WD 1145+017 b]]

|[[WD 1145+017]]

|

|-

|-

| [[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

|-

|[[SDSS J1228+1040 b]]

|

|-

|[[K2-38b]]

|[[K2-38]]

|

|-

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

| ~ 0.03 g/cm³<ref name="Masuda" />

| The densities of Kepler-51 b and c have been constrained to be below 0.05 g/cm³ (expected value 0.03 g/cm³ for each). The density of Kepler-51d is determined to be 0.046±0.009 g/cm³.<ref name="Masuda" />

|-

| {{nowrap| [[Kepler-70b]] }}

| {{nowrap| [[Kepler-70]] }}

|

|-

| {{nowrap| [[OGLE-2016-BLG-1195Lb]] }}

| {{nowrap| [[OGLE-2016-BLG-1195L]] }}

|

|-

| [[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]]

|-

| {{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>

|}

 

{| class="wikitable" style="text-align:left;"

|-

! style="background:#efefef;"| Notes

|-

| [[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]]}}

|-

| {{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}}

|-

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

-->

|-

| {{nowrap|[[2MASS J2126-8140]]}}

| {{nowrap|[[TYC 9486-927-1]]}}

| 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

|-

| {{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]]}}

|

|-

| {{nowrap|[[Kepler-47b]]}}

| {{nowrap|[[Kepler-47]]AB}}

|<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>

|-

| {{nowrap|[[Kepler-16b]]}}

| {{nowrap|[[Kepler-16]]AB}}

|<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>

|-

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

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

| 1,168 AU

|-

| {{nowrap|[[Fomalhaut b]]}}

| {{nowrap|[[Fomalhaut]]}}

| 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.

|-

| [[FW Tauri AB b]]

| [[FW Tau AB]]

| ≈11 AU

|-

| {{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>

|-

| [[Kepler-70b]] and [[Kepler-70c]]<ref name=HottestExoplanet />

| [[Kepler-70]]

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

|-

| [[Kepler-36b]] and [[Kepler-36c]]

| [[Kepler-36]]

| 11%

|-

| PTFO 8-8695 / [[CVSO 30]] b and [[CVSO 30]] c

| [[CVSO 30]]

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

|-

| PTFO 8-8695 b / [[CVSO 30]] b and [[CVSO 30]] c

| [[CVSO 30]]

| 7,900,000%

|}

 

{| class="wikitable" style="text-align:left;"

|-

! style="background:#efefef;"| Notes

|-

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

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

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

|-

| [[Kapteyn b]]

| [[Kapteyn's Star]]

| [[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>

|-

| {{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/>

[[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]]}}

| {{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}}.

|-

|[[VHS 1256-1257 b]]

|[[VHS 1256-1257]]

|

|-

| {{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/>

|

|-

| [[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>

|-

|[[VB 10 b]]

|[[VB 10]]

|

|-

| [[2M 0746+20]]

| {{Solar radius|0.089 (± 0.003)}}

|-

| [[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]]

|

|-

| {{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>

|

|-

| {{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

|-

| {{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

|-

| [[TRAPPIST-1]]

| 2,511 K

|}

 

{| class="wikitable"

|-

! Notes

|-

|[[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

|-

|[[TRAPPIST-1]]

|7

|1

|-

| Kepler 64

| [[PH1b]] (Kepler 64b)

| 4

|-

| Kepler 42<br>Kepler 70

| b, [[Kepler-42c|c]], d<br>[[Kepler-70b|b]], [[Kepler-70c|c]], d?

| 1<br>1

|-

| [[HR 8799]]

| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]

| 1

|-

| Kepler-70

| [[Kepler-70b|b]], [[Kepler-70c|c]], d?

| 1

|-

| [[HR 8799]]

| [[HR 8799 b|b]], [[HR 8799 c|c]], [[HR 8799 d|d]], [[HR 8799 e|e]]

| 1

|-

|

|

|

|-

|

|

|

|-

| [[Kepler-444]]

| b, c, d, e, f

| 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.

|-

| Kepler-52?

| b, c, d

| 1

|-

|

|

|

|-

|

|

|

|-

| [[Kepler-444]]

| b, c, d, e, f

| 1

|-

|

|

|

|-

| Kepler-52?

| b, c, d

| 1

|-

| Multiplanetary system with largest ratio of mean planetary mass to stellar mass

|

|-

| b, c

| 1

|-

| 1

|}

 

* [[Daftar bintang dengan proplid]]

* [[Metode pendeteksian eksoplanet]]

 

==Catatan==

 

{{DEFAULTSORT:Daftar Keekstreman Planet Ekstrasurya}}