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[[File:NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut B.jpg|thumb|280px|[[Fomalhaut]] is a star 25 light-years away with an exoplanet ([[Fomalhaut b]]) that has been directly imaged in 2013 by [[NASA]].]]
[[File:NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut B.jpg|thumb|280px|[[Fomalhaut]] is a star 25 light-years away with an exoplanet ([[Fomalhaut b]]) that has been directly imaged in 2013 by [[NASA]].]]


Astronomers have identified a total of 65 [[exoplanet]]s within 50 [[light-year]]s of the [[Solar System]],{{ref label|A|a|none}} but the existence of at least another 34 unconfirmed exoplanets has been proposed. This corresponds to only 35 stars with confirmed planetary systems (and six with only unconfirmed exoplanets) of the around 1,400 stars that are estimated to be located within 50 light-years.{{ref label|B|b|none}}<ref name=autogenerated2>{{cite web|url=http://www.atlasoftheuniverse.com/50lys.html |title=Stars within 50 light years |publisher=An Atlas of the Universe|first= Richard |last=Powell |year= 2006|accessdate=2014-05-17}}</ref> Of the around 133 nearby stars which are bright enough to be visible with the naked eye,{{ref label|C|c|none}}<ref name=autogenerated2 /> so far, only 18 have confirmed planetary systems.
Astronomers have identified a total of 65 [[exoplanet]]s within 50 [[light-year]]s of the [[Solar System]],{{ref label|A|a|none}} but the existence of at least another 34 unconfirmed exoplanets has been proposed. This corresponds to only 35 stars with confirmed planetary systems (and six with only unconfirmed exoplanets) of the around 1,400 stars that are estimated to be located within 50 light-years.{{ref label|B|b|none}}<ref name=autogenerated2>{{cite web|url=http://www.atlasoftheuniverse.com/50lys.html |title=Stars within 50 light years |publisher=An Atlas of the Universe|first= Richard |last=Powell |year= 2006|accessdate=2014-05-17}}</ref>
Of the around 133 nearby stars which are bright enough to be visible with the naked eye,{{ref label|C|c|none}}<ref name=autogenerated2 /> so far, only 18 have confirmed planetary systems.

==Earliest detections==


Reports of planetary systems first came in 1996 for three stars located over 40 light-years away: [[55 Cancri]],<ref name="Butler1997">{{cite doi |10.1086/310444}}</ref> Since 1999, more planets have been reported, including a total of five planets revolving around 55 Cancri, and four planets around [[Gliese 876]], Upsilon Andromedae. Eight star systems have three confirmed planetary partners, four other have only two planets, while the remaining 20 systems have only one confirmed planet. A total of seven planets have been suggested for [[Gliese 667 C]] (but only two have been confirmed), six around Gliese 581 and [[HD 40307]], and a total of five planets revolving around [[Tau Ceti]] (all unconfirmed).
Reports of planetary systems first came in 1996 for three stars located over 40 light-years away: [[55 Cancri]],<ref name="Butler1997">{{cite doi |10.1086/310444}}</ref> Since 1999, more planets have been reported, including a total of five planets revolving around 55 Cancri, and four planets around [[Gliese 876]], Upsilon Andromedae. Eight star systems have three confirmed planetary partners, four other have only two planets, while the remaining 20 systems have only one confirmed planet. A total of seven planets have been suggested for [[Gliese 667 C]] (but only two have been confirmed), six around Gliese 581 and [[HD 40307]], and a total of five planets revolving around [[Tau Ceti]] (all unconfirmed).


==Nearest confirmed planet==
⚫
The closest star with a confirmed exoplanet is [[Gliese 674]], 14.8 light-years away from our [[Solar System]]. Of the other [[List of nearest stars and brown dwarfs|41 star systems]] that are closer, the closest, [[Alpha Centauri]] (4.1 light-years away), has been suggested to contain [[Alpha Centauri Bb|a planetary companion]] that may be similar in size to Earth.<ref name = "Dumusque">{{cite doi|10.1038/nature11572 }}</ref> Of the 35 planetary systems located within 50 light-years, 20 are located within 40 light-years, 11 are within 30 light-years, and only four are within 20 light-years.

⚫
The closest star with a confirmed exoplanet is [[Kapteyn b]] which approximately 13 light years from Earth, followed by [[Gliese 674]], 14.8 light-years away from our [[Solar System]]. Of the other [[List of nearest stars and brown dwarfs|41 star systems]] that are closer, the closest, [[Alpha Centauri]] (4.1 light-years away), has been suggested to contain [[Alpha Centauri Bb|a planetary companion]] that may be similar in size to Earth.<ref name = "Dumusque">{{cite doi |10.1038/nature11572 }}</ref> Of the 35 planetary systems located within 50 light-years, 20 are located within 40 light-years, 11 are within 30 light-years, and only four are within 20 light-years.

==Planets with orbits close to their own suns==


Out of the 65 confirmed planets within 50 light-years, more than half were found to revolve around their star closer and complete an orbit faster than [[Mercury (planet)|Mercury]] does around the [[Sun]], and 18 have a more eccentric orbit than that of Mercury. Considering their [[minimum mass]]es, 46 exoplanets are expected to be [[gas giant]]s, and only 19 under ten times more massive than [[Earth]]. The smallest of these has minimum mass of 2.4 times that of Earth's and revolves around [[82 G. Eridani]], 20 light-years away. Only three exoplanets have had their radii measured from transit events with their host stars: [[Gliese 436 b]] at 0.365 [[Jupiter radius|''R''<sub>J</sub>]],<ref name=autogenerated11/> [[55 Cancri e]] at 0.178 ''R''<sub>J</sub><ref name=autogenerated19/> and [[GJ 1214 b]] at 0.238 ''R''<sub>J</sub>.<ref name=autogenerated6/>
Out of the 65 confirmed planets within 50 light-years, more than half were found to revolve around their star closer and complete an orbit faster than [[Mercury (planet)|Mercury]] does around the [[Sun]], and 18 have a more eccentric orbit than that of Mercury. Considering their [[minimum mass]]es, 46 exoplanets are expected to be [[gas giant]]s, and only 19 under ten times more massive than [[Earth]]. The smallest of these has minimum mass of 2.4 times that of Earth's and revolves around [[82 G. Eridani]], 20 light-years away. Only three exoplanets have had their radii measured from transit events with their host stars: [[Gliese 436 b]] at 0.365 [[Jupiter radius|''R''<sub>J</sub>]],<ref name=autogenerated11/> [[55 Cancri e]] at 0.178 ''R''<sub>J</sub><ref name=autogenerated19/> and [[GJ 1214 b]] at 0.238 ''R''<sub>J</sub>.<ref name=autogenerated6/>


==Inclusion criteria==
==Inclusion criteria==

===Official status===

There is no official organization that acknowledges reports for the existence of exoplanets, but the Working Group on Extrasolar Planets of the [[International Astronomical Union]] adopted in 2003 a working definition limiting the upper masses of exoplanets below that where thermonuclear fusion of [[deuterium]] occurs. This limit is calculated to be around 13 times the [[Mass_of_Jupiter#Mass|mass of Jupiter]], and above it, an object is classified as a [[brown dwarf]].<ref name=IAU>{{cite doi |10.1017/S1743921306004509}}</ref>
There is no official organization that acknowledges reports for the existence of exoplanets, but the Working Group on Extrasolar Planets of the [[International Astronomical Union]] adopted in 2003 a working definition limiting the upper masses of exoplanets below that where thermonuclear fusion of [[deuterium]] occurs. This limit is calculated to be around 13 times the [[Mass_of_Jupiter#Mass|mass of Jupiter]], and above it, an object is classified as a [[brown dwarf]].<ref name=IAU>{{cite doi |10.1017/S1743921306004509}}</ref>

===Criteria for this list===


For the purpose of this list, an exoplanet is regarded as unconfirmed when there is only a single (primary) report which presents its discovery, but there are no follow-up papers discussing their existence. There are a few examples where the existence of an [[exoplanet]] has been discussed in multiple papers, but there exists a minority of skeptics. For example, [[Alpha Centauri Bb]] has received criticism on the methods used to propose the existence of the planet.<ref name = "skyandtelescope">{{cite web| url = http://www.skyandtelescope.com/news/Planet-Found-in-Alpha-Centauri-System-174559561.html| title = Planet Found in Alpha Centauri System| publisher = Sky and Telescope| last = Carlisle|first = Camille|date = 2012-10-18|accessdate = 2012-10-18}}</ref> Several reports of nearby exoplanets have been made but these proposals have been widely disproven since, as was the case for [[Teegarden's star]]<ref>{{cite doi|10.1111/j.1365-2966.2012.21236.x}}</ref> and [[VB 10]].<ref>{{cite doi |10.1088/0004-637X/700/1/623 }}</ref><ref>{{cite web|url=http://exoplanet.eu/catalog/vb_10_b/ |title=The Extrasolar Planet Encyclopaedia — VB 10 b |publisher=Exoplanet.eu |accessdate=2014-05-20}}</ref>
For the purpose of this list, an exoplanet is regarded as unconfirmed when there is only a single (primary) report which presents its discovery, but there are no follow-up papers discussing their existence. There are a few examples where the existence of an [[exoplanet]] has been discussed in multiple papers, but there exists a minority of skeptics. For example, [[Alpha Centauri Bb]] has received criticism on the methods used to propose the existence of the planet.<ref name = "skyandtelescope">{{cite web| url = http://www.skyandtelescope.com/news/Planet-Found-in-Alpha-Centauri-System-174559561.html| title = Planet Found in Alpha Centauri System| publisher = Sky and Telescope| last = Carlisle|first = Camille|date = 2012-10-18|accessdate = 2012-10-18}}</ref> Several reports of nearby exoplanets have been made but these proposals have been widely disproven since, as was the case for [[Teegarden's star]]<ref>{{cite doi|10.1111/j.1365-2966.2012.21236.x}}</ref> and [[VB 10]].<ref>{{cite doi |10.1088/0004-637X/700/1/623 }}</ref><ref>{{cite web|url=http://exoplanet.eu/catalog/vb_10_b/ |title=The Extrasolar Planet Encyclopaedia — VB 10 b |publisher=Exoplanet.eu |accessdate=2014-05-20}}</ref>

===Partially measured planets===


Usually, nearby exoplanets have been discovered by measuring the changes in the [[radial velocity]] of the host star, which allows for a precise estimate of their orbital parameters, but does not allow for an estimate of their [[orbital inclination]] (''i''). Because of this challenge, only 17 of the 66 exoplanets have their masses measured, while for the others, only their [[minimum mass]]es (M<sub>real</sub>*sin(''i'')) are known. It is generally expected that most of these masses to be close to their [[true mass]]es, as there is only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.<ref name="cumming08">{{cite doi |10.1086/588487}}</ref> However, there have been a few cases where planetary candidates were suggested but later refinement showed that these were more than 13 times more massive than Jupiter, and thus are likely brown dwarfs. This has been the case for WISE 0458+6434 B,<ref>{{cite web|url=http://exoplanet.eu/catalog/wise_0458+6434_b/ |work = The Extrasolar Planet Encyclopaedia| title= WISE 0458+6434 b |publisher=Exoplanet.eu |date=2014-01-16 |accessdate=2014-05-17}}</ref> WISE 1217+16A B,<ref>{{cite web|url=http://exoplanet.eu/catalog/wise_1217+16a_b/ |work = The Extrasolar Planet Encyclopaedia|title= WISE 1217+16A b |publisher=Exoplanet.eu |accessdate=2014-05-17}}</ref> 2M 0746+20 B,<ref>{{cite web|url=http://exoplanet.eu/catalog/2m_0746+20_b/ |work = The Extrasolar Planet Encyclopaedia| title= 2M 0746+20 b |publisher=Exoplanet.eu |date=2012-01-20 |accessdate=2014-05-17}}</ref><ref>{{cite web|author=|url=http://www.openexoplanetcatalogue.com/system.html?id=2M%200746%2B20%20b |title=2M 0746+20 |publisher=Open Exoplanet Catalogue |accessdate=2014-05-17}}</ref> MOA-2008-BLG-379L B,<ref>{{cite web|author= |url=http://www.openexoplanetcatalogue.com/system.html?id=MOA-2008-BLG-379L%20b |title=MOA-2008-BLG-379L |publisher=Open Exoplanet Catalogue |accessdate=2014-05-17}}</ref> [[SDSS J1416+1348|SDSS 141624 B]],<ref>{{cite web|url=http://exoplanet.eu/catalog/sdss_141624_b/ |work = The Extrasolar Planet Encyclopaedia| title= SDSS 141624 b |publisher=Exoplanet.eu |date=2010-01-18 |accessdate=2014-05-20}}</ref> and [[HD 104304|HD 104304 B]].<ref>{{cite web|url=http://exoplanet.eu/catalog/hd_104304_b/ |work = The Extrasolar Planet Encyclopaedia| title= HD 104304 b |publisher=Exoplanet.eu |date=2010-05-05 |accessdate=2014-05-20}}</ref>
Usually, nearby exoplanets have been discovered by measuring the changes in the [[radial velocity]] of the host star, which allows for a precise estimate of their orbital parameters, but does not allow for an estimate of their [[orbital inclination]] (''i''). Because of this challenge, only 17 of the 66 exoplanets have their masses measured, while for the others, only their [[minimum mass]]es (M<sub>real</sub>*sin(''i'')) are known. It is generally expected that most of these masses to be close to their [[true mass]]es, as there is only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.<ref name="cumming08">{{cite doi |10.1086/588487}}</ref> However, there have been a few cases where planetary candidates were suggested but later refinement showed that these were more than 13 times more massive than Jupiter, and thus are likely brown dwarfs. This has been the case for WISE 0458+6434 B,<ref>{{cite web|url=http://exoplanet.eu/catalog/wise_0458+6434_b/ |work = The Extrasolar Planet Encyclopaedia| title= WISE 0458+6434 b |publisher=Exoplanet.eu |date=2014-01-16 |accessdate=2014-05-17}}</ref> WISE 1217+16A B,<ref>{{cite web|url=http://exoplanet.eu/catalog/wise_1217+16a_b/ |work = The Extrasolar Planet Encyclopaedia|title= WISE 1217+16A b |publisher=Exoplanet.eu |accessdate=2014-05-17}}</ref> 2M 0746+20 B,<ref>{{cite web|url=http://exoplanet.eu/catalog/2m_0746+20_b/ |work = The Extrasolar Planet Encyclopaedia| title= 2M 0746+20 b |publisher=Exoplanet.eu |date=2012-01-20 |accessdate=2014-05-17}}</ref><ref>{{cite web|author=|url=http://www.openexoplanetcatalogue.com/system.html?id=2M%200746%2B20%20b |title=2M 0746+20 |publisher=Open Exoplanet Catalogue |accessdate=2014-05-17}}</ref> MOA-2008-BLG-379L B,<ref>{{cite web|author= |url=http://www.openexoplanetcatalogue.com/system.html?id=MOA-2008-BLG-379L%20b |title=MOA-2008-BLG-379L |publisher=Open Exoplanet Catalogue |accessdate=2014-05-17}}</ref> [[SDSS J1416+1348|SDSS 141624 B]],<ref>{{cite web|url=http://exoplanet.eu/catalog/sdss_141624_b/ |work = The Extrasolar Planet Encyclopaedia| title= SDSS 141624 b |publisher=Exoplanet.eu |date=2010-01-18 |accessdate=2014-05-20}}</ref> and [[HD 104304|HD 104304 B]].<ref>{{cite web|url=http://exoplanet.eu/catalog/hd_104304_b/ |work = The Extrasolar Planet Encyclopaedia| title= HD 104304 b |publisher=Exoplanet.eu |date=2010-05-05 |accessdate=2014-05-20}}</ref>

===Rogue planets===


There are known examples of potential free-floating [[sub-brown dwarf]]s, sometimes referred as "[[rogue planet]]s", that are excluded from this list, such as [[WISE 0855–0714]]<ref name="NASA20140425">{{cite news |url=http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/ |title=NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun |work=[[NASA]].gov |first1=Whitney |last1=Clavin |first2=J. D. |last2=Harrington |date=2014-04-25| archiveurl=http://web.archive.org/web/20140426004939/http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425 |archivedate=2014-04-25 |deadurl=no}}</ref> and [[UGPS J072227.51-054031.2]].<ref name="Lucas2010">{{cite doi|10.1111.2Fj.1745-3933.2010.00927.x}}</ref>
There are known examples of potential free-floating [[sub-brown dwarf]]s, sometimes referred as "[[rogue planet]]s", that are excluded from this list, such as [[WISE 0855–0714]]<ref name="NASA20140425">{{cite news |url=http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425/ |title=NASA's Spitzer and WISE Telescopes Find Close, Cold Neighbor of Sun |work=[[NASA]].gov |first1=Whitney |last1=Clavin |first2=J. D. |last2=Harrington |date=2014-04-25| archiveurl=http://web.archive.org/web/20140426004939/http://www.nasa.gov/jpl/wise/spitzer-coldest-brown-dwarf-20140425 |archivedate=2014-04-25 |deadurl=no}}</ref> and [[UGPS J072227.51-054031.2]].<ref name="Lucas2010">{{cite doi|10.1111.2Fj.1745-3933.2010.00927.x}}</ref>

===Measurement uncertainties===


Notable uncertainties exist for the distances measured for some stars. Because of this, some sources regard some stars as being within the 50 light-years (ly) threshold, but these stars were not included in the current list: [[Mu Arae]] (50.59 ly), [[51 Pegasi]] (50.7 ly), [[Tau Boötis]] (50.9 ly).
Notable uncertainties exist for the distances measured for some stars. Because of this, some sources regard some stars as being within the 50 light-years (ly) threshold, but these stars were not included in the current list: [[Mu Arae]] (50.59 ly), [[51 Pegasi]] (50.7 ly), [[Tau Boötis]] (50.9 ly).
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==Notes==
==Notes==


{{ordered list|type=a
{{ordered list|type=d
| item1_value = 1 | 1 = {{note label|A|a|none}} Current list is compiled from the following databases:
| item1_value = 1 | 1 = {{note label|A|a|none}} Current list is compiled from the following databases:
:: {{cite web |url=http://exoplanet.eu/catalog-all.php?&munit=&runit=&punit=&mode=10&more=yes |title=The Extrasolar Planets Encyclopaedia |work=}}
:: {{cite web |url=http://exoplanet.eu/catalog-all.php?&munit=&runit=&punit=&mode=10&more=yes |title=The Extrasolar Planets Encyclopaedia |work=}}

Revision as of 05:38, 11 August 2014

Fomalhaut is a star 25 light-years away with an exoplanet (Fomalhaut b) that has been directly imaged in 2013 by NASA.

Astronomers have identified a total of 65 exoplanets within 50 light-years of the Solar System,[a] but the existence of at least another 34 unconfirmed exoplanets has been proposed. This corresponds to only 35 stars with confirmed planetary systems (and six with only unconfirmed exoplanets) of the around 1,400 stars that are estimated to be located within 50 light-years.[b][1]

Of the around 133 nearby stars which are bright enough to be visible with the naked eye,[c][1] so far, only 18 have confirmed planetary systems.

Earliest detections

Reports of planetary systems first came in 1996 for three stars located over 40 light-years away: 55 Cancri,[2] Since 1999, more planets have been reported, including a total of five planets revolving around 55 Cancri, and four planets around Gliese 876, Upsilon Andromedae. Eight star systems have three confirmed planetary partners, four other have only two planets, while the remaining 20 systems have only one confirmed planet. A total of seven planets have been suggested for Gliese 667 C (but only two have been confirmed), six around Gliese 581 and HD 40307, and a total of five planets revolving around Tau Ceti (all unconfirmed).

Nearest confirmed planet

The closest star with a confirmed exoplanet is Kapteyn b which approximately 13 light years from Earth, followed by Gliese 674, 14.8 light-years away from our Solar System. Of the other 41 star systems that are closer, the closest, Alpha Centauri (4.1 light-years away), has been suggested to contain a planetary companion that may be similar in size to Earth.[3] Of the 35 planetary systems located within 50 light-years, 20 are located within 40 light-years, 11 are within 30 light-years, and only four are within 20 light-years.

Planets with orbits close to their own suns

Out of the 65 confirmed planets within 50 light-years, more than half were found to revolve around their star closer and complete an orbit faster than Mercury does around the Sun, and 18 have a more eccentric orbit than that of Mercury. Considering their minimum masses, 46 exoplanets are expected to be gas giants, and only 19 under ten times more massive than Earth. The smallest of these has minimum mass of 2.4 times that of Earth's and revolves around 82 G. Eridani, 20 light-years away. Only three exoplanets have had their radii measured from transit events with their host stars: Gliese 436 b at 0.365 RJ,[4] 55 Cancri e at 0.178 RJ[5] and GJ 1214 b at 0.238 RJ.[6]

Inclusion criteria

Official status

There is no official organization that acknowledges reports for the existence of exoplanets, but the Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition limiting the upper masses of exoplanets below that where thermonuclear fusion of deuterium occurs. This limit is calculated to be around 13 times the mass of Jupiter, and above it, an object is classified as a brown dwarf.[7]

Criteria for this list

For the purpose of this list, an exoplanet is regarded as unconfirmed when there is only a single (primary) report which presents its discovery, but there are no follow-up papers discussing their existence. There are a few examples where the existence of an exoplanet has been discussed in multiple papers, but there exists a minority of skeptics. For example, Alpha Centauri Bb has received criticism on the methods used to propose the existence of the planet.[8] Several reports of nearby exoplanets have been made but these proposals have been widely disproven since, as was the case for Teegarden's star[9] and VB 10.[10][11]

Partially measured planets

Usually, nearby exoplanets have been discovered by measuring the changes in the radial velocity of the host star, which allows for a precise estimate of their orbital parameters, but does not allow for an estimate of their orbital inclination (i). Because of this challenge, only 17 of the 66 exoplanets have their masses measured, while for the others, only their minimum masses (Mreal*sin(i)) are known. It is generally expected that most of these masses to be close to their true masses, as there is only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.[12] However, there have been a few cases where planetary candidates were suggested but later refinement showed that these were more than 13 times more massive than Jupiter, and thus are likely brown dwarfs. This has been the case for WISE 0458+6434 B,[13] WISE 1217+16A B,[14] 2M 0746+20 B,[15][16] MOA-2008-BLG-379L B,[17] SDSS 141624 B,[18] and HD 104304 B.[19]

Rogue planets

There are known examples of potential free-floating sub-brown dwarfs, sometimes referred as "rogue planets", that are excluded from this list, such as WISE 0855–0714[20] and UGPS J072227.51-054031.2.[21]

Measurement uncertainties

Notable uncertainties exist for the distances measured for some stars. Because of this, some sources regard some stars as being within the 50 light-years (ly) threshold, but these stars were not included in the current list: Mu Arae (50.59 ly), 51 Pegasi (50.7 ly), Tau Boötis (50.9 ly).

List

Key to colors
° Mercury, Earth and Jupiter (for comparison purposes)
† Unconfirmed exoplanets
# Confirmed multiplanetary systems
Host star system Companion exoplanet (in order from star) References
Name Distance
(ly)
Apparent
magnitude
Mass
(M☉)
Temperature
(K)
Age
(Gyr)
Label Mass
(MJ)
Semi-major axis
(AU)
Orbital period
(days)
Eccentricity
Inclination
(°)
Discovery year
Sun° 0 −26.74 1.000 5,780 4.57 Mercury 0.00017 0.387 87.97 0.205 — — —
Earth 0.00314 1.0 365.26 0.0167 — — —
Jupiter 1 5.204 4,332.6 0.0488 — — —
Alpha Centauri 4.36 1.33 0.934 5,210 5.0 Bb† >0.00355 0.04185 3.24 ~0 — 2012 [22][23][24][25]
Luhman 16 6.59 23.0 ~0.04 ~1,300 <4.5 –† ~10 — — — — 2013 [26][27]
Epsilon Eridani 10.49 3.73 0.820 5,120 0.66 b† 1.55 3.38 2,500 0.25 30.1 2000 [28][29][30][31][32]
d† — ~20 — — — 2008 [33]
c† ~0.1 ~40 ~100,000 ~0.3 — 2002 [34]
Epsilon Indi 11.81 4.83 0.762 4,630 1.3 –† >0.97 8.57 >10,000 — — 2002 [32]
Tau Ceti 11.90 3.50 0.783 5,340 5.8 b† >0.0063 0.105 <12.7 0.16 — 2012 [35][36]
c† >0.0098 0.195 35.4 0.03 — 2012 [36][37]
d† >0.0113 0.374 94.1 0.08 — 2012 [36][38]
e† >0.0135 0.552 168 0.05 — 2012 [36][39][40]
f† >0.0208 1.35 642 0.03 — 2012 [36][40][41]
Kapteyn's star 12.76 8.85 0.281 3,550 8.0 b†[d] >0.015 0.168 48.6 0.21 – 2014 [42]
c†[d] >0.022 0.311 122 0.23 – 2014 [43]
Gliese 687 14.77 9.15 0.431 3,400 — b†[d] >0.058 0.1635 38.1 0.04 — 2014 [44]
Gliese 674 14.81 9.36 0.354 3,610 0.55 b >0.0349 0.0387 4.69 0.20 — 2007 [45][46]
Gliese 876# 15.29 10.2 0.334 3,350 2.5 d 0.0215 0.0208 1.938 0.21 50 2005 [47][48]
c 0.714 0.130 30.1 0.26 48.1 2000 [48][49]
b 2.276 0.208 61.1 0.032 48.9 2000 [48][50]
e 0.046 0.334 124 0.055 59.5 2010 [48][51]
Gliese 832 16.16 8.67 0.450 3,620 — c†[d] >0.157 0.162 35.7 0.03 — 2014 [52]
b >0.689 3.6 3,420 0.08 — 2008 [53][54][55]
82 G. Eridani# 19.71 4.26 0.701 5,490 6.1–12.7[56][57] b >0.0085 0.1207 18.3 — — 2011 [58][59]
c >0.0076 0.2036 40.1 — — 2011 [58][60]
d >0.015 0.3499 90.3 — — 2011 [58][61]
Gliese 581# 20.37 10.55 0.31 3,500 8.0 e >0.028 0.028 3.15 0.32 — 2009 [62][63]
b >0.05 0.041 5.37 0.031 — 2005 [62][64]
c >0.017 0.073 12.9 0.07 — 2007 [62][65]
g† >0.01 0.146 36.7 — — 2010 [66]
d† >0.019 0.22 66.6 0.21 — 2007 [62][67]
f† >0.023 0.758 430 — — 2010 [68]
Gliese 667# 23.60 10.22 0.33 3,600 >2.0 Cb >0.0178 0.050 7.20 0.122 — 2009 [69][70][71]
Ch† >0.0035 0.0893 17.0 0.06 — 2013 [69][70][72]
Cc >0.0117 0.125 28.1 0.133 — 2011 [69][70][73]
Cf† >0.0085 0.156 39.0 0.03 — 2013 [69][70][74]
Ce† >0.0085 0.213 62.2 0.02 — 2013 [69][70][75]
Cd† >0.0218 0.304 106 0.68 — 2012 [69][70][76]
Cg† >0.0145 0.549 256 0.08 — 2013 [69][70][77]
Fomalhaut 25.13 1.16 1.920 8,590 0.55 b >3.0 115 ~620,000 0.11 — 2008 [78][79]
61 Virginis# 27.90 4.74 0.942 5,530 8.96 b >0.016 0.0502 4.22 0.12 — 2009 [80][81]
c >0.0573 0.2175 38.0 0.14 — 2009 [80][81]
d >0.072 0.476 123 0.35 — 2009 [80][81]
HD 192310# 28.78 6.13 0.778 5,140 7.8 b >0.053 0.32 74.7 0.13 — 2010 [82][83]
c >0.075 1.18 526 0.32 — 2011 [84]
Gliese 433# 28.97 9.79 0.48 3,550 — b >0.0182 0.058 7.37 0.08 — 2009 [85][86]
c >0.14 3.6 3,700 0.17 — 2012 [87]
Gliese 849 29.67 10.42 0.490 3,600 — b >0.9 2.35 1,910 0.012 — 2006 [88][89]
c†[d] >0.77 ~5 7,050 0.218 — 2013 [90]
HD 102365 30.08 4.89 0.890 5,650 9.0 b >0.05 0.46 122 0.34 — 2011 [91][92]
Gliese 176 30.25 9.96 0.490 3,350 — b >0.0265 0.066 8.78 — — 2007 [93][94]
c† >0.044 0.18 40 — — 2009 [95]
Gliese 436 33.08 10.68 0.452 3,350 6.0 UCF-1.01† 0.0009 0.0185 1.37 — 86.7 2012 [96][97]
b 0.0724 0.0288 2.64 0.15 85.8 2004 [4][96]
UCF-1.02† >0.00085 — — — — 2012 [96][98]
Gliese 649# 33.74 9.62 0.542 3,700 — c >0.03 0.043 4.48 0.2 — 2013 [99][100]
b >0.328 1.135 598 0.3 — 2009 [99][101]
Pollux 33.79 1.15 2.080 4,670 0.72 b >2.9 1.69 589 0.02 — 2006 [102][103]
Gliese 86 35.17 6.17 0.796 5,350 2.03 b >4.0 0.11 15.8 0.046 — 2000 [104][105]
HIP 57050 35.88 11.9 0.340 3,190 — b >0.298 0.1635 41.4 0.31 — 2010 [106][107]
54 Piscium 36.07 5.8 0.882 5,220 5.1 Ac†[d] >0.09 0.186 31.0 0.04 — 2013 [108][109]
Ab 0.23 0.284 62.2 0.63 83 2003 [108][110]
HD 85512 36.37 7.67 0.687 4,720 5.6 b >0.011 0.26 58.4 0.11 — 2011 [111][112]
Gliese 179 40.1 11.96 0.357 3,370 — b >0.82 2.41 2,290 0.21 — 2010 [113][114]
55 Cancri# 40.25 5.95 0.905 5,200 10.2 e 0.0262 0.0156 0.737 <0.06 81 2004 [5]
b >0.8 0.1134 14.7 0.016 — 1996 [115][116]
c >0.169 0.240 44.3 0.053 — 2002 [117]
f >0.144 0.781 261 0.0002 — 2007 [118]
d 4.80 5.76 5,200 0.03 53 2002 [119]
HD 69830# 40.75 5.95 0.849 5,360 7.0 b 0.13 0.0785 8.67 0.1 13 2006 [120][121]
c 0.17 0.186 31.6 0.13 13 2006 [120][122]
d 0.26 0.63 197 0.07 13 2006 [120][123]
HD 147513 41.68 5.38 1.072 5,930 0.65 b >1.21 1.32 528 0.26 — 2003 [124][125]
GJ 1214 42.25 14.71 0.157 3,030 6.0 b 0.0203 0.0143 1.580 0.27 88.67 2009 [6][126]
HD 40307# 42.39 7.2 0.740 4,980 1.2 b >0.0126 0.0468 4.31 0.2 — 2008 [127][128]
c >0.0208 0.0799 9.62 0.06 — 2008 [127][129]
d >0.0299 0.1321 20.4 0.07 — 2008 [127][130]
e† >0.011 0.1886 34.6 0.15 — 2012 [127][131]
f† >0.0164 0.247 51.8 0.02 — 2012 [127][132]
g† >0.0223 0.6 198 0.29 — 2012 [127][133]
Upsilon Andromedae# 44.00 4.09 1.310 6,210 3.8 b 0.62–1.24 0.059 4.62 0.013 >30 1996 [134][135]
c ~14 0.861 238 0.24 8 1999 [30][134][136]
d 10.19 2.55 1,300 0.27 24 1999 [30][134][137]
e >1.059 5.25 3,850 0.0054 — 2010 [134][138]
47 Ursae Majoris# 45.87 5.10 1.063 5,880 7.4 b 2.53–7 2.1 1,078 0.032 — 1996 [139][140]
c >0.54 3.6 2,390 0.098 — 2001 [139][141]
d >1.64 11.6 14,000 0.16 — 2010 [139][142]
Gamma Cephei 46.00 3.23 1.26 4,760 6.6 Ab 1.85–19 2.05 903 0.049 5.7 2003 [143][144]
HIP 79431 46.96 11.34 0.491 3,190 — b >2.1 0.36 112 0.29 — 2010 [145][146]
Nu2 Lupi# 48.27 5.65 0.91 5,660 10.4 b >0.0166 0.0933 11.6 0.18 — 2011 [147]
c >0.0358 0.1665 27.6 0.16 — 2011 [148]
d >0.03 0.411 107 0.43 — 2011 [149]
Gliese 163# 48.92 11.3 0.40 3,500 3.0 b >0.0334 0.0607 8.63 0.0106 — 2012 [150][151]
e† >0.012 0.10 19.5 0.32 — 2013 [152]
c >0.0228 0.1254 25.6 0.094 — 2013 [150][153]
f† >0.023 0.33 108 0.41 — 2013 [152]
d >0.0695 1.027 601 0.40 — 2012 [150][154]
HD 176051 48.89 5.22 0.71 6,000 8.1 Bb >1.5 1.76 1,020 — — 2010 [155]
Gliese 317 49.2 12.0 0.42 3,510 — b 1.8–3.6 1.15 692 0.11 >25 2007 [156][157][158]
c† >2.0 ~30 >10,000 0.81 — 2007 [159]
HD 38858 49.6 5.97 0.886 5,660 6.2 b >0.0961 1.038 407 0.27 — 2011 [160]

Statistics

Planetary systems

Template:Multicol

Systems by planet count
Confirmed
exoplanets 		No. of
systems 		Systems
5 1 55 Cancri
4 2 Gliese 876, Upsilon Andromedae
3 8 82 G. Eridani, Gliese 581, 61 Virginis, HD 69830, HD 40307, 47 Ursae Majoris, Nu2 Lupi, Gliese 163
2 4 Gliese 667, HD 192310, Gliese 433, Gliese 649
1 20 —
Total 35
0 7 —

Template:Multicol-break

Systems by distance
Distance Confirmed
systems 		Unconfirmed
systems
< 10 light-years 0 2
10–20 light-years 4 5
20–30 light-years 7 0
30–40 light-years 9 0
40–50 light-years 15 0
Systems visible with the naked eye[161]
Visible host star? Confirmed
systems 		Unconfirmed
systems
Yes (V < 6.5) 18 4
No (V > 6.5) 17 3

Template:Multicol-end

Exoplanets

Template:Multicol

Exoplanets by mass
Type Subtype[162] Mass range[162] Confirmed Unconfirmed
Terrestrial Sub-terran <0.0015 MJ (<0.5 ME) 0 2
Terran 0.0015–0.006 MJ (0.5–2 ME) 0 2
Super-terran 0.006–0.03 MJ (2–10 ME) 19 20
Gas giant Neptunian 0.03–0.15 MJ (10–50 ME) 18 4
Jovian 0.15–1.8 MJ (50–600 ME) 17 3
Super-jovian >1.8 MJ (>600 ME) 11 2
Total 65 33
Exoplanets by orbital radius
Orbital radius Confirmed Unconfirmed Notes
< 0.4 AU 39 21 Mercury orbits at 0.39 AU
0.4–1.0 AU 6 4 Earth orbits at 1.0 AU
1.0–5.0 AU 16 3
>5.0 AU 4 4 Jupiter orbits at 5.2 AU
Exoplanets by orbital period
Orbital period Confirmed Unconfirmed Notes
< 90 days 36 17 Mercury takes 88 days
90–365 days 9 7
1–12 years 17 3 Jupiter takes 11.9 years
>12 years 3 4
Exoplanets by orbital eccentricity
Orbital eccentricity Confirmed Unconfirmed Notes
< 0.02 6 1 Earth's is 0.0167
0.02–0.20 36 14
> 0.20 18 11 Mercury's is 0.205

Template:Multicol-break

Exoplanets by discovery year
Year Confirmed Unconfirmed
1996 3 0
1999 2 0
2000 3 1
2001 1 0
2002 2 2
2003 3 0
2004 2 0
2005 2 0
2006 5 0
2007 5 2
2008 5 1
2009 8 1
2010 8 2
2011 11 0
2012 3 12
2013 2 9
2014 0 4
Total 65 34

Template:Multicol-end

See also

Notes

  1. ^ Current list is compiled from the following databases:
    "The Extrasolar Planets Encyclopaedia".
    "Exoplanets Data Explorer".
    "Open Exoplanet Catalogue".
    "NASA Exoplanet Archive".
  2. ^ For reference, the 99th and 100th closest known star systems as of 2012, HR 8832 and LHS 3003 (Proxima Hydrae), are about 21 light-years away from the Solar System.[163]
  3. ^ According to the Bortle scale, an astronomical object visible to the naked eye under "typical" dark-sky conditions in a rural area if it has an apparent magnitude smaller than +6.5. To the unaided eye, the limiting magnitude is +7.6 to +8.0 under "excellent" dark-sky conditions (with effort).[161]
  4. ^ This recently-discovered exoplanet is regarded as unconfirmed as there is only a single (primary) report discussing its existence.

References

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  3. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1038/nature11572 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1038/nature11572 instead.
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  24. ^ Star's age taken from: Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1111/j.1365-2966.2012.21818.x, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1111/j.1365-2966.2012.21818.x instead.
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  28. ^ "epsilon Eri b". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  32. ^ a b Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1051/0004-6361/201116551, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1051/0004-6361/201116551 instead.
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  34. ^ Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1086/344708 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1086/344708 instead.
  35. ^ "tau Cet b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-12-19. Retrieved 2014-05-20.
  36. ^ a b c d e Open Exoplanet Catalogue. "tau Ceti". Open Exoplanet Catalogue. Retrieved 2014-05-17.
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  38. ^ "tau Cet d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-12-19. Retrieved 2014-05-20.
  39. ^ "tau Cet e". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-12-19. Retrieved 2014-05-20.
  40. ^ a b Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1073/pnas.1309107110, please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1073/pnas.1309107110 instead.
  41. ^ "tau Cet f". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-12-19. Retrieved 2014-05-20.
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  44. ^ "Gl 687 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
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  47. ^ "Gliese 876 d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2010-12-14. Retrieved 2014-05-17.
  48. ^ a b c d Attention: This template ({{cite doi}}) is deprecated. To cite the publication identified by doi:10.1088/0004-637X/719/1/890 , please use {{cite journal}} (if it was published in a bona fide academic journal, otherwise {{cite report}} with |doi=10.1088/0004-637X/719/1/890 instead.
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  111. ^ "HD 85512 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  113. ^ "GJ 179 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  115. ^ "55 Cnc e". Exoplanets Data Explorer. Retrieved 2014-05-17.
  116. ^ "55 Cnc b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-06-07. Retrieved 2014-05-17.
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  118. ^ "55 Cnc f". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-06-07. Retrieved 2014-05-17.
  119. ^ "55 Cnc d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-06-07. Retrieved 2014-05-17.
  120. ^ a b c "HD 69830 c". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  124. ^ "HD 147513 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  126. ^ "GJ 1214 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
  127. ^ a b c d e f "HD 40307 c". Exoplanets Data Explorer. Retrieved 2014-05-17.
  128. ^ "HD 40307 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2008-10-14. Retrieved 2014-05-17.
  129. ^ "HD 40307 c". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2008-10-14. Retrieved 2014-05-17.
  130. ^ "HD 40307 d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2008-10-14. Retrieved 2014-05-17.
  131. ^ "HD 40307 e". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-11-08. Retrieved 2014-05-17.
  132. ^ "HD 40307 f". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-11-08. Retrieved 2014-05-17.
  133. ^ "HD 40307 g". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2012-11-08. Retrieved 2014-05-17.
  134. ^ a b c d "upsilon And b". Exoplanets Data Explorer. Retrieved 2014-05-17.
  135. ^ "ups And b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  136. ^ "ups And c". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  137. ^ "ups And d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  138. ^ "ups And e". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
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  140. ^ "47 Uma b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2010-03-10. Retrieved 2014-05-17.
  141. ^ "47 Uma c". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  142. ^ "47 Uma d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  143. ^ "gamma Cep b". Exoplanets Data Explorer. Retrieved 2014-05-17.
  144. ^ "gamma Cephei b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  145. ^ "HIP 79431 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
  146. ^ "HIP 79431 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2010-01-11. Retrieved 2014-05-17.
  147. ^ "HD 136352 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-09-12. Retrieved 2014-05-17.
  148. ^ "HD 136352 c". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-09-12. Retrieved 2014-05-17.
  149. ^ "HD 136352 d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-09-12. Retrieved 2014-05-17.
  150. ^ a b c "GJ 163 c". Exoplanets Data Explorer. Retrieved 2014-05-17.
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  154. ^ "Gj 163 d". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. Retrieved 2014-05-17.
  155. ^ "HD 176051 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2010-10-22. Retrieved 2014-05-17.
  156. ^ "GJ 317 b". Exoplanets Data Explorer. Retrieved 2014-05-17.
  157. ^ "GJ 317 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-11-14. Retrieved 2014-05-17.
  158. ^ "Gliese 317". Open Exoplanet Catalogue. Retrieved 2014-05-17.
  159. ^ "GJ 317 c". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-11-14. Retrieved 2014-05-17.
  160. ^ "HD 38858 b". The Extrasolar Planet Encyclopaedia. Exoplanet.eu. 2011-09-12. Retrieved 2014-05-17.
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External links

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