List of nearest exoplanets
![](http://upload.wikimedia.org/wikipedia/commons/thumb/e/eb/NASA%27s_Hubble_Reveals_Rogue_Planetary_Orbit_For_Fomalhaut_B.jpg/280px-NASA%27s_Hubble_Reveals_Rogue_Planetary_Orbit_For_Fomalhaut_B.jpg)
![](http://upload.wikimedia.org/wikipedia/commons/thumb/2/29/Distances_to_nearest_confirmed_exoplanets_in_light_years.png/450px-Distances_to_nearest_confirmed_exoplanets_in_light_years.png)
There are 7,026 known exoplanets, or planets outside the Solar System that orbit a star, as of July 24, 2024; only a small fraction of these are located in the vicinity of the Solar System.[3] Within 10 parsecs (32.6 light-years), there are 106 exoplanets listed as confirmed by the NASA Exoplanet Archive.[note 1][4] Among the over 500 known stars and brown dwarfs within 10 parsecs,[5][note 2] around 60 have been confirmed to have planetary systems; 51 stars in this range are visible to the naked eye,[note 3][7] eight of which have planetary systems.
The first report of an exoplanet within this range was in 1998 for a planet orbiting around Gliese 876 (15.3 light-years (ly) away), and the latest as of 2024 is one around GJ 1289 (27.3 ly). The closest exoplanets are those found orbiting the star closest to the Solar System, which is Proxima Centauri 4.25 light-years away. The first confirmed exoplanet discovered in the Proxima Centauri system was Proxima Centauri b, in 2016. HD 219134 (21.6 ly) has six exoplanets, the highest number discovered for any star within this range.
Most known nearby exoplanets orbit close to their stars. A majority are significantly larger than Earth, but a few have similar masses, including planets around YZ Ceti, Gliese 367, and Proxima Centauri which may be less massive than Earth. Several confirmed exoplanets are hypothesized to be potentially habitable, with Proxima Centauri b and GJ 1002 b (15.8 ly) considered among the most likely candidates.[8] The International Astronomical Union has assigned proper names to some known extrasolar bodies, including nearby exoplanets, through the NameExoWorlds project. Planets named in the 2015 event include the planets around Epsilon Eridani (10.5 ly) and Fomalhaut,[note 4][11] while planets named in the 2022 event include those around Gliese 436, Gliese 486, and Gliese 367.[12]
Exoplanets within 10 parsecs
[edit]° | Mercury, Earth and Jupiter (for comparison purposes) |
# | Confirmed multiplanetary systems |
↑ | Exoplanets believed to be potentially habitable[8] |
Host star system | Companion exoplanet (in order from star) | Notes and additional planetary observations | |||||||||||
---|---|---|---|---|---|---|---|---|---|---|---|---|---|
Name | Distance (ly) |
Apparent magnitude (V) |
Mass (M☉) |
Label [note 5] |
Mass (ME)[note 6] |
Radius (R🜨) |
Semi-major axis (AU) |
Orbital period (days) |
Eccentricity |
Inclination (°) |
Discovery method |
Discovery year | |
Sun° | 0.000016 | −26.7 | 1 | Mercury | 0.055 | 0.3829 | 0.387 | 88.0 | 0.205 | — | — | — | — |
Earth | 1 | 1 | 1 | 365.3 | 0.0167 | — | — | — | |||||
Jupiter | 317.8 | 10.973 | 5.20 | 4,333 | 0.0488 | — | — | — | |||||
Proxima Centauri# | 4.2465 | 11.13 | 0.123 | d | ≥0.26 | — | 0.0289 | 5.122 | 0.04 | — | RV | 2022 | [14][15] one disputed candidate (c)[16][17][18][19] |
b↑ | ≥1.07 | — | 0.0486 | 11.19 | 0.02 | — | RV | 2016 | |||||
Lalande 21185# | 8.304 | 7.52 | 0.46 | b | ≥2.69 | — | 0.0788 | 12.94 | 0.06 | — | RV | 2019 | 1 candidate[20] |
c | ≥13.6 | — | 2.94 | 2,946 | 0.13 | — | RV | 2021 | |||||
Epsilon Eridani | 10.489 | 3.73 | 0.781 | Ægir | 242 | — | 3.53 | 2,689 | 0.26 | 166.5 | RV | 2000 | 1 inferred planet, 1 or possibly 2 inner debris discs, and an outer disc[21][22] |
Lacaille 9352# | 10.724 | 7.34 | 0.489 | b | ≥4.2 | — | 0.068 | 9.262 | 0.03 | — | RV | 2019 | 1 candidate[23][24] |
c | ≥7.6 | — | 0.120 | 21.79 | 0.03 | — | RV | 2019 | |||||
Ross 128 | 11.007 | 11.1 | 0.168 | b↑ | ≥1.40 | — | 0.0496 | 9.866 | 0.12 | — | RV | 2017 | [25] |
Groombridge 34 A# | 11.619 | 8.1 | 0.38 | b | ≥3.03 | — | 0.072 | 11.44 | 0.09 | ~54? | RV | 2014 | [26][27] |
c | ≥36 | — | 5.4 | 7,600 | 0.27 | ~54? | RV | 2018 | |||||
Epsilon Indi A | 11.867 | 4.83 | 0.762 | b | 941 | — | 11.08 | 15,700 | 0.42 | 98.7 | RV | 2018 | [28][22] |
Tau Ceti# | 11.912 | 3.50 | 0.78 | g | ≥1.75 | — | 0.133 | 20.0 | 0.06 | ~35? | RV | 2017 | 4 disputed candidates [29][30][8][31][32][33] |
h | ≥1.8 | — | 0.243 | 49.4 | 0.23 | ~35? | RV | 2017 | |||||
e | ≥3.9 | — | 0.538 | 163 | 0.18 | ~35? | RV | 2017 | |||||
f | ≥3.9 | — | 1.33 | 640 | 0.16 | ~35? | RV | 2017 | |||||
GJ 1061# | 11.984 | 7.52 | 0.113 | b | ≥1.37 | — | 0.021 | 3.204 | <0.31 | — | RV | 2019 | two solutions for d's orbit[34] |
c↑ | ≥1.74 | — | 0.035 | 6.689 | <0.29 | — | RV | 2019 | |||||
d↑ | ≥1.64 | — | 0.054 | 13.03 | <0.53 | — | RV | 2019 | |||||
YZ Ceti# | 12.122 | 12.1 | 0.130 | b | ≥0.70 | — | 0.0163 | 2.021 | 0.06 | — | RV | 2017 | [35] |
c | ≥1.14 | — | 0.0216 | 3.060 | 0.0 | — | RV | 2017 | |||||
d | ≥1.09 | — | 0.0285 | 4.656 | 0.07 | — | RV | 2017 | |||||
Luyten's Star# | 12.348 | 11.94 | 0.29 | c | ≥1.18 | — | 0.0365 | 4.723 | 0.10 | — | RV | 2017 | [36][23] |
b↑ | ≥2.89 | — | 0.0911 | 18.65 | 0.17 | — | RV | 2017 | |||||
d | ≥10.8 | — | 0.712 | 414 | 0.17 | — | RV | 2019 | |||||
e | ≥9.3 | — | 0.849 | 542 | 0.03 | — | RV | 2019 | |||||
Teegarden's Star# | 12.497 | 15.40 | 0.08 | b↑ | ≥1.16 | — | 0.0259 | 4.906 | 0.03 | — | RV | 2019 | [37][38] |
c↑ | ≥1.05 | — | 0.0455 | 11.42 | 0.04 | — | RV | 2019 | |||||
d | ≥0.82 | — | 0.0791 | 26.13 | 0.07 | — | RV | 2024 | |||||
Wolf 1061# | 14.050 | 10.1 | 0.25 | b | ≥1.91 | — | 0.0375 | 4.887 | 0.15 | — | RV | 2015 | [36] |
c↑ | ≥3.41 | — | 0.0890 | 17.87 | 0.11 | — | RV | 2015 | |||||
d | ≥7.7 | — | 0.470 | 217 | 0.55 | — | RV | 2015 | |||||
TZ Arietis | 14.578 | 12.30 | 0.14 | b | ≥67 | — | 0.88 | 771 | 0.46 | — | RV | 2019 | 2 refuted candidates[23][39][40] |
Gliese 687# | 14.839 | 9.15 | 0.41 | b | ≥17.2 | — | 0.163 | 38.14 | 0.17 | — | RV | 2014 | [23][39] |
c | ≥16.0 | — | 1.165 | 728 | 0.40 | — | RV | 2019 | |||||
Gliese 674 | 14.849 | 9.38 | 0.35 | b | ≥11.1 | — | 0.039 | 4.694 | 0.20 | — | RV | 2007 | [41] |
Gliese 876# | 15.238 | 10.2 | 0.33 | d | 6.68 | — | 0.0210 | 1.938 | 0.04 | 56.7 | RV | 2005 | [42] |
c | 235 | — | 0.1309 | 30.10 | 0.26 | 56.7 | RV | 2000 | |||||
b | 749 | — | 0.2098 | 61.10 | 0.03 | 56.7 | RV | 1998 | |||||
e | 16 | — | 0.3355 | 123.6 | 0.05 | 56.7 | RV | 2010 | |||||
GJ 1002# | 15.806 | 13.84 | 0.12 | b↑ | ≥1.08 | — | 0.0457 | 10.35 | — | — | RV | 2022 | [43] |
c↑ | ≥1.36 | — | 0.0738 | 21.2 | — | — | RV | 2022 | |||||
Gliese 832 | 16.200 | 8.67 | 0.45 | b | 315 | — | 3.7 | 3,853 | 0.05 | 51 or 134 | RV | 2008 | 1 refuted candidate[44][45] |
GJ 3323# | 17.531 | 12.2 | 0.164 | b | ≥2.0 | — | 0.0328 | 5.36 | 0.2 | — | RV | 2017 | [36] |
c | ≥2.3 | — | 0.126 | 40.5 | 0.2 | — | RV | 2017 | |||||
Gliese 251 | 18.215 | 9.65 | 0.372 | b | ≥4.0 | — | 0.0818 | 14.2 | 0.10 | — | RV | 2020 | [46] |
Gliese 229 A# | 18.791 | 8.14 | 0.58 | c↑ | ≥7.3 | — | 0.339 | 122 | 0.19 | — | RV | 2020 | Ab not confirmed until 2020[47] |
b | ≥8.5 | — | 0.898 | 526 | 0.10 | — | RV | 2014 | |||||
Gliese 752 A | 19.292 | 9.13 | 0.46 | b | ≥12.2 | — | 0.343 | 106 | 0.10 | — | RV | 2018 | [48][49] |
82 G. Eridani# | 19.704 | 4.26 | 0.85 | b | ≥2.0 | — | 0.13 | 18.3 | 0.09 | — | RV | 2011 | 5 disputed candidates [50][51][52][53] |
d | ≥4.7 | — | 0.37 | 89.6 | 0.13 | — | RV | 2011 | |||||
Gliese 555 | 20.395 | 11.32 | 0.29 | b | ≥5.5 | — | 0.142 | 36.1 | 0.08 | — | RV | 2023 | 1 candidate[54] |
EQ Pegasi A | 20.400 | 10.38 | 0.436 | b | 718 | — | 0.643 | 284 | 0.35 | 69.2 | Astrometry | 2022 | [55] |
Gliese 581# | 20.549 | 10.5 | 0.295 | e | 2.5 | — | 0.0280 | 3.15 | 0.01 | 47 | RV | 2009 | 3 refuted candidates and a disc[56] |
b | 20.5 | — | 0.0399 | 5.37 | 0.03 | 47 | RV | 2005 | |||||
c | 6.8 | — | 0.0718 | 12.9 | 0.03 | 47 | RV | 2007 | |||||
Gliese 338 B | 20.658 | 7.0 | 0.64 | b | ≥10.3 | — | 0.141 | 24.5 | 0.11 | — | RV | 2020 | [57] |
Gliese 625 | 21.131 | 10.2 | 0.30 | b | ≥2.8 | — | 0.0784 | 14.6 | ~0.1 | — | RV | 2017 | [58] |
HD 219134# | 21.336 | 5.57 | 0.78 | b | 4.7 | 1.60 | 0.0388 | 3.09 | ~0 | 85.05 | RV | 2015 | [59][60][61] |
c | 4.4 | 1.51 | 0.065 | 6.77 | 0.062 | 87.28 | RV | 2015 | |||||
d | ≥16 | — | 0.237 | 46.9 | 0.138 | ~87? | RV | 2015 | |||||
f | ≥7.3 | — | 0.146 | 22.7 | 0.148 | ~87? | RV | 2015 | |||||
g | ≥11 | — | 0.375 | 94.2 | 0 | ~87? | RV | 2015 | |||||
h (e) | ≥108 | — | 3.11 | 2,247 | 0.06 | ~87? | RV | 2015 | |||||
LTT 1445 A# | 22.387 | 10.53 | 0.26 | c | 1.54 | 1.15 | 0.0266 | 3.12 | <0.22 | 87.43 | Transit | 2021 | 1 candidate[62][63][64] |
b | 2.87 | 1.30 | 0.0381 | 5.36 | <0.11 | 89.68 | Transit | 2019 | |||||
Gliese 393 | 22.953 | 8.65 | 0.41 | b | ≥1.71 | — | 0.0540 | 7.03 | 0.00 | — | RV | 2019 | [23][65] |
Gliese 667 C# | 23.623 | 10.2 | 0.33 | b | ≥5.4 | — | 0.049 | 7.20 | 0.13 | ~52? | RV | 2009 | 5 dubious candidates [66][8][67][68][23] |
c↑ | ≥3.9 | — | 0.1251 | 28.2 | 0.03 | ~52? | RV | 2011 | |||||
Gliese 514 | 24.878 | 9.03 | 0.53 | b | ≥5.2 | — | 0.421 | 140 | 0.45 | — | RV | 2022 | [69] |
GJ 1151 | 26.231 | 14.01 | 0.164 | c | ≥10.6 | — | 0.571 | 390 | — | — | RV | 2023 | 1 refuted candidate[70][71][72][73] |
Gliese 486 | 26.351 | 11.395 | 0.32 | Su | 2.8 | 1.31 | 0.0173 | 1.47 | <0.05 | 88.4 | Transit | 2021 | [74] |
Gliese 686 | 26.613 | 9.58 | 0.42 | b | ≥7.1 | — | 0.097 | 15.5 | 0.04 | — | RV | 2019 | [75][23] |
GJ 1289 | 27.275 | 12.67[76] | 0.21 | b | ≥6.3 | — | 0.27 | 112 | 0 | — | RV | 2024 | [77] |
61 Virginis# | 27.836 | 4.74 | 0.95 | b | ≥6.1 | — | 0.05 | 4.22 | 0.05 | ~77? | RV | 2009 | a debris disc[53] |
c | ≥17.9 | — | 0.22 | 38.1 | 0.06 | ~77? | RV | 2009 | |||||
d | ≥10.5 | — | 0.47 | 123 | 0.12 | ~77? | RV | 2009 | |||||
CD Ceti | 28.052 | 14.001 | 0.161 | b | ≥3.95 | — | 0.0185 | 2.29 | 0 | — | RV | 2020 | [78] |
Gliese 785# | 28.739 | 6.13 | 0.78 | b | ≥17 | — | 0.32 | 75 | 0.13 | — | RV | 2010 | [79] |
c | ≥24 | — | 1.18 | 530 | ~0.3 | — | RV | 2011 | |||||
Gliese 849# | 28.750 | 10.4 | 0.49 | b | ≥270 | — | 2.26 | 1,910 | 0.05 | — | RV | 2006 | [80][23] |
c | ≥300 | — | 4.82 | 5,520 | 0.087 | — | RV | 2006 | |||||
Gliese 433# | 29.605 | 9.79 | 0.48 | b | ≥6.0 | — | 0.062 | 7.37 | 0.04 | — | RV | 2009 | [81][23][47] |
d | ≥5.2 | — | 0.178 | 36.1 | 0.07 | — | RV | 2020 | |||||
c | ≥32 | — | 4.82 | 5,090 | 0.12 | — | RV | 2012 | |||||
HD 102365 A | 30.396 | 4.89 | 0.85 | b | ≥16 | — | 0.46 | 122 | 0.34 | — | RV | 2010 | [82] |
Gliese 367# | 30.719 | 9.98 | 0.45 | Tahay | 0.63 | 0.70 | 0.0071 | 0.322 | 0.06 | 79.89 | Transit | 2021 | [83][84] |
c | ≥4.1 | — | 0.077 | 11.5 | 0.09 | ~80? | RV | 2023 | |||||
d | ≥6.0 | — | 0.159 | 34.4 | 0.14 | ~80? | RV | 2023 | |||||
Gliese 357# | 30.776 | 10.9 | 0.34 | b | 6.1 | 1.17 | 0.035 | 3.93 | 0.02 | 88.92 | Transit | 2019 | [85][23] |
c | ≥3.6 | — | 0.061 | 9.13 | 0.04 | ~89? | RV | 2019 | |||||
d↑ | ≥7.7 | — | 0.204 | 55.7 | 0.03 | ~89? | RV | 2019 | |||||
Gliese 176 | 30.937 | 10.1 | 0.45 | b | ≥8.0 | — | 0.066 | 8.77 | 0.08 | — | RV | 2007 | 1 disputed candidate[86][87][23] |
GJ 3512# | 30.976 | 13.11 | 0.123 | b | ≥147 | — | 0.338 | 204 | 0.44 | — | RV | 2019 | [88] |
c | ≥54 | — | >1.2 | >1390 | — | — | RV | 2019 | |||||
Wolf 1069 | 31.229 | 13.99 | 0.167 | b↑ | ≥1.26 | — | 0.0672 | 15.6 | — | — | RV | 2023 | [89] |
AU Microscopii# | 31.683 | 8.63 | 0.50 | b | 17 | 4.38 | 0.0645 | 8.463 | 0.10 | 89.03 | Transit | 2020 | 2 candidates[90][91][92][93] |
c | <28 | 3.51 | 0.1101 | 18.86 | 0 | 88.62 | Transit | 2020 | |||||
Gliese 436 | 31.882 | 10.67 | 0.41 | Awohali | 21.4 | 4.33 | 0.0280 | 2.64 | 0.15 | 85.8 | RV | 2004 | [94][95] |
Gliese 49 | 32.158 | 8.9 | 0.57 | b | ≥16.4 | — | 0.106 | 17.3 | 0.03 | — | RV | 2019 | [96] |
GJ 3988 | 32.316 | 13.6 | 0.184 | b | ≥3.7 | — | 0.0405 | 6.944 | 0 | — | RV | 2023 | [97] |
HD 260655# | 32.608 | 9.77 | 0.439 | b | 2.14 | 1.240 | 0.0293 | 2.780 | 0.039 | 87.35 | Transit | 2022 | [98] |
c | 3.09 | 1.533 | 0.0475 | 5.706 | 0.038 | 87.79 | Transit | 2022 |
Excluded objects
[edit]Unlike for bodies within the Solar System, there is no clearly established method for officially recognizing an exoplanet. According to the International Astronomical Union, an exoplanet should be considered confirmed if it has not been disputed for five years after its discovery.[99] There have been examples where the existence of exoplanets has been proposed, but even after follow-up studies their existence is still considered doubtful by some astronomers. Such cases include Wolf 359 (7.9 ly, in 2019),[23] LHS 288 (15.8 ly, in 2007),[100] and Gliese 682 (16.3 ly, in 2014).[47] There are also several instances where proposed exoplanets were later disproved by subsequent studies, including candidates around Alpha Centauri B (4.36 ly),[101] Barnard's Star (5.96 ly),[102][103] Kapteyn's Star (12.8 ly),[104] Van Maanen 2 (14.1 ly),[105] Groombridge 1618 (15.9 ly),[106] AD Leonis (16.2 ly),[107] 40 Eridani A (16.3 ly),[108][109] VB 10 (19.3 ly),[110] and Fomalhaut (25.1 ly).[2]
In 2021, a candidate planet was detected around Vega, though it has yet to be confirmed.[111] Another candidate planet, Candidate 1, was directly imaged around Alpha Centauri A, though it may also be a clump of asteroids or an artifact of the discovery mechanism.[112] Candidate planets around Luyten 726-8 (8.77 ly)[113] and GJ 3378 (25.2 ly) were reported in 2024.[77]
The Working Group on Extrasolar Planets of the International Astronomical Union adopted in 2003 a working definition on the upper limit for what constitutes a planet: not being massive enough to sustain thermonuclear fusion of deuterium. Some studies have calculated this to be somewhere around 13 times the mass of Jupiter, and therefore objects more massive than this are usually classified as brown dwarfs.[114] Some proposed candidate exoplanets have been shown to be massive enough to fall above the threshold, and thus are likely brown dwarfs, as is the case for: SCR 1845-6357 B (13.1 ly),[115] SDSS J1416+1348 B (30.3 ly),[116] and WISE 1217+1626 B (30 ly).[117]
Excluded from the current list are known examples of potential free-floating sub-brown dwarfs, or "rogue planets", which are bodies that are too small to undergo fusion yet they do not revolve around a star. Known such examples include: WISE 0855−0714 (7.4 ly),[118] UGPS 0722-05, (13.4 ly)[119] WISE 1541−2250 (18.6 ly),[120] and SIMP J01365663+0933473 (20.0 ly).[121]
See also
[edit]Notes
[edit]- ^ Listed values are primarily taken from NASA Exoplanet Archive,[4] but other databases include a few additional exoplanet entries tagged as "Confirmed" that have yet to be compiled into the NASA archive. Such databases include:
- "Exoplanet Catalog". Extrasolar Planets Encyclopaedia. 1995. Full table.
- "Exoplanets Data Explorer". Exoplanet Orbit Database. California Planet Survey. Click the "+" button to visualize additional parameters.
- "Open Exoplanet Catalogue". Click the "Show options" to visualize additional parameters. Archived from the original on 2017-09-02. Retrieved 2015-02-14.
- ^ For reference, the 100th closest known star system in April 2021 was EQ Pegasi (20.4 ly).[5]
- ^ According to the Bortle scale, an astronomical object is 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).[6]
- ^ The star Epsilon Eridani was named Ran (after Rán, the Norse goddess of the sea), and the planet Epsilon Eridani b was named AEgir (after Ægir, Rán's husband),[9] while the planet Fomalhaut b was named Dagon (after Dagon, an ancient Syrian “fish god”[10]).[11]
- ^ Exoplanet naming convention assigns uncapitalized letters starting from b to each planet based on chronological order of their initial report, and in increasing order of distance from the parent star for planets reported at the same time. Omitted letters signify planets that have yet to be confirmed, or planets that have been retracted altogether.
- ^ Most reported exoplanet masses have very large error margins (typically, between 10% and 30%). The mass of an exoplanet has generally been inferred from measurements on changes in the radial velocity of the host star, but this kind of measurement only allows for an estimate on the exoplanet's orbital parameters, but not on their orbital inclination (i). As such, most exoplanets only have an estimated minimum mass (Mreal*sin(i)), where their true masses are statistically expected to come close to this minimum, with only about 13% chance for the mass of an exoplanet to be more than double its minimum mass.[13]
References
[edit]- ^ Harrington, J. D.; Villard, Ray (2013-08-01). "NASA's Hubble Reveals Rogue Planetary Orbit For Fomalhaut". NASA. Archived from the original on 2015-11-06. Retrieved 2015-09-18.
- ^ a b Gáspár, András; Rieke, George H. (April 20, 2020). "New HST data and modeling reveal a massive planetesimal collision around Fomalhaut". PNAS. 117 (18): 9712–9722. arXiv:2004.08736. Bibcode:2020PNAS..117.9712G. doi:10.1073/pnas.1912506117. PMC 7211925. PMID 32312810. S2CID 215827666.
- ^ Schneider, Jean (1995). "Interactive Extra-solar Planets Catalog". Extrasolar Planets Encyclopaedia. Archived from the original on 2012-02-12. Retrieved 2018-03-20.
- ^ a b c "NASA Exoplanet Archive—Confirmed Planetary Systems". NASA Exoplanet Science Institute. California Institute of Technology. Retrieved 2023-08-18.
- ^ a b Reylé, Céline; Jardine, Kevin; Fouqué, Pascal; Caballero, Jose A.; Smart, Richard L.; Sozzetti, Alessandro (30 April 2021). "The 10 parsec sample in the Gaia era". Astronomy & Astrophysics. 650: A201. arXiv:2104.14972. Bibcode:2021A&A...650A.201R. doi:10.1051/0004-6361/202140985. S2CID 233476431. Data available at https://gruze.org/10pc/
- ^ Bortle, John E. (2001). "Light Pollution And Astronomy: The Bortle Dark-Sky Scale". Sky & Telescope. Archived from the original on 2009-03-23. Retrieved 2014-05-20.
- ^ Powell, Richard (2006). "Stars within 50 light years". An Atlas of the Universe. Archived from the original on 2014-06-27. Retrieved 2014-05-17.
- ^ a b c d "The Habitable Exoplanets Catalog". Planetary Habitability Laboratory. University of Puerto Rico in Arecibo. 2015-09-01. Archived from the original on 2016-01-09. Retrieved 2015-09-17.
- ^ "epsilon Eridani". NameExoWorlds. International Astronomical Union. Archived from the original on 2018-02-15. Retrieved 2018-05-14.
- ^ "Fomalhaut (alpha Piscis Austrini)". Nameexoworlds. International Astronomical Union. Archived from the original on 2017-04-30. Retrieved 2018-05-14.
- ^ a b "Final Results of NameExoWorlds Public Vote Released" (Press release). International Astronomical Union. 2015-12-15. Archived from the original on 2018-05-15. Retrieved 2018-03-17.
- ^ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
- ^ Cumming, Andrew; Butler, R. Paul; Marcy, Geoffrey W.; et al. (2008). "The Keck Planet Search: Detectability and the Minimum Mass and Orbital Period Distribution of Extrasolar Planets". Publications of the Astronomical Society of the Pacific. 120 (867): 531–554. arXiv:0803.3357. Bibcode:2008PASP..120..531C. doi:10.1086/588487. S2CID 10979195.
- ^ Anglada-Escudé, Guillem; Amado, Pedro J.; Barnes, John; et al. (2016). "A terrestrial planet candidate in a temperate orbit around Proxima Centauri". Nature. 536 (7617): 437–440. arXiv:1609.03449. Bibcode:2016Natur.536..437A. doi:10.1038/nature19106. PMID 27558064. S2CID 4451513.
- ^ Faria, J. P.; Suárez Mascareño, A.; et al. (January 4, 2022). "A candidate short-period sub-Earth orbiting Proxima Centauri" (PDF). Astronomy & Astrophysics. 658. European Southern Observatory: 17. arXiv:2202.05188. Bibcode:2022A&A...658A.115F. doi:10.1051/0004-6361/202142337.
- ^ Damasso, Mario; Del Sordo, Fabio; Anglada-Escudé, Guillem; et al. (15 January 2020). "A low-mass planet candidate orbiting Proxima Centauri at a distance of 1.5 AU". Science Advances. 6 (3). eaax7467. Bibcode:2020SciA....6.7467D. doi:10.1126/sciadv.aax7467. PMC 6962037. PMID 31998838.
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External links
[edit]- "Extrasolar Planets". The Planetary Society. Planetary.org.
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- "PHL's Exoplanets Catalog". Planetary Habitability Laboratory. UPR Arecibo. 2018-03-02.
- Onsi Fakhouri. "Exoplanet Orbit Database". Exoplanet Data Explorer. Exoplanets.org.
- "NASA Exoplanet Archive". Caltech.
- "Stars Within 20 Light Years". Atlas of the Universe.