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List of potentially habitable exoplanets

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The following list includes some of the potentially habitable exoplanets discovered so far. It is mostly based on estimates of habitability by the Habitable Worlds Catalog (HWC), and data from the NASA Exoplanet Archive. The HWC is maintained by the Planetary Habitability Laboratory at the University of Puerto Rico at Arecibo.[1] There is also a speculative list being developed of superhabitable planets.

Surface planetary habitability is thought to require an orbit at the right distance from the host star for liquid surface water to be present, in addition to various geophysical and geodynamical aspects, atmospheric density, radiation type and intensity, and the host star's plasma environment.[2]

List

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This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by adding missing items with reliable sources.

This is a list of exoplanets within the circumstellar habitable zone that are either under 10 Earth masses or smaller than 2.5 Earth radii, and thus have a chance of being rocky.[3][1] Note that inclusion on this list does not guarantee habitability, and in particular the larger planets are more unlikely to have a rocky composition.[4] Earth is included for both comparison and reference, while Venus and Mars are included for reference only.

Note that mass and radius values prefixed with "~" have not been measured, but are estimated from a mass-radius relationship.

Object Star Star type Mass (M⊕) Radius (R⊕) Density (g/cm3) Flux (F⊕) Teq (K) Period (days) Distance (ly) Refs/Notes
Earth
(reported for reference)		 Sun G2V 1.00 1.00 5.514 1.00 255 365.25 0 Only planet known to support life.
Venus
(reported for reference)		 Sun G2V 0.815 0.950 5.243 1.911 244.261 224.70 0.0000042 [5]
Mars
(reported for reference)		 Sun G2V 0.107 0.533 3.934 0.431 209.8 686.98 0.0000058 - 0.000042 [6]
82 G. Eridani d 82 G. Eridani G8V ≥5.82 647.6 19.7 [7]
Gliese 12 b Gliese 12 M4V 0.88+0.39
−0.26		 1.03±0.11 4.44 1.6±0.2 315 12.7 40 [8]
Gliese 163 c Gliese 163 M3V ≥6.80 — — 1.25 277 25.6 49 [1]
Gliese 180 c Gliese 180 M2V ≥6.40 — — 0.78 239 24.3 39 Not confirmed[1][9]
Gliese 180 d Gliese 180 M2V ≥7.56 — — 0.26 106.3 39 [1]
Gliese 229 Ac Gliese 229 A M1V ≥8.57 — — 0.44 216 121.9 18.8
Gliese 357 d Gliese 357 M2V ≥6.10 — — 0.38 200 55.7 31
Gliese 433 d Gliese 433 M2V ≥5.22 — — 1.06 36.1 29.6 [1]
Gliese 514 b Gliese 514 M1V ≥5.20 — — 0.28 (0.114−0.79) 202 140.4 25 Highly eccentric[10]
Gliese 555 b Gliese 555 M4V ≥5.46 — — 0.5 214 [11] 36.2 20.4 Probably a mini-Neptune or an ocean planet[12]
Gliese 625 b Gliese 625 M2V ≥2.82 — — 14.628 21.1 Only in HZ if very optimistic models used[13][14][15]
Gliese 667 Cc Gliese 667 C M1V ≥3.81 ~1.54 — 0.88 277 28.1 23.62 [16][1]
Gliese 1002 b Gliese 1002 M5V ≥1.08 ~1.03 — 0.67 231 10.3 15.8 [17]
Gliese 1002 c Gliese 1002 M5V ≥1.36 1.1 — 0.26 182 21.2 15.8 [17][18]
GJ 1061 c GJ 1061 M5V ≥1.74 ~1.18 — 1.45 275 6.7 12
GJ 1061 d GJ 1061 M5V ≥1.64 ~1.16 — 0.69 218 13.0 12
GJ 3293 d GJ 3293 M2V ≥7.60 — — 0.59 223 48.1 66 [1]
HD 40307 g HD 40307 K2V ≥7.09 — — 0.67 226 197.8 42 Not confirmed[1][19]
HD 216520 c HD 216520 K0V ≥9.44 — — 1.28 154.4 64 [1]
HIP 38594 b HIP 38594 M0V ≥8.10 — — 1.34 60.7 58 [1]
K2-9b K2-9 M2V — 2.25 — 1.45 279 18.4 270 [1][20]
K2-72e K2-72 M?V ~2.21 1.29 — 1.30 261 24.2 217 [21]
K2-332b K2-332 M?V — 2.20 — 1.17 17.7 402 [1]
K2-288Bb K2-288 B M3V 4.27 1.91 — 0.44 207 31.4 214 [22]
Kepler-22b Kepler-22 G5V — 2.38 — 1.10 261 289.9 635 [1][23]
Kepler-62e Kepler-62 K2V 4.5+14.2
−2.6		 1.61 — 1.15 264 122.4 981 [1][24]
Kepler-62f Kepler-62 K2V 2.8+0.4
−0.4		 1.41 — 0.41 204 267.3 981 [1][25]
Kepler-155c Kepler-155 M0V — 2.24 — 1.05 52.7 957 [1]
Kepler-174d Kepler-174 K3V — 2.19 — 0.59 206 247.4 1254 [1]
Kepler-186f Kepler-186 M1V 1.44+2.33
−1.12		 1.17 — 0.29 188 129.9 579 [1]
Kepler-283c Kepler-283 K5V — 1.82 — 0.89 248 92.7 1526 [1]
Kepler-296e Kepler-296 K7V 2.96 1.52 — 1.41 276 34.1 737 [1][26][27]
Kepler-296f Kepler-296 K7V — 1.80 — 0.44 225 63.3 737 [1][28]
Kepler-442b Kepler-442 K5V 2.36+5.9
−1.3		 1.35 — 0.70 233 112.3 1193 [1]
Kepler-440b Kepler-440 K6V — 1.91 — 1.44 273 101.1 981 [1]
Kepler-443b Kepler-443 K3V — 2.35 — 0.89 247 177.7 2615 [1]
Kepler-452b Kepler-452 G2V ~5 1.63 — 1.11 261 384.8 1799 Not confirmed[1][29][30][31][32]
Kepler-705b Kepler-705 M?V — 2.11 — 0.77 243 56.1 903
Kepler-1229b Kepler-1229 M?V 2.540 1.40 — 0.32 213 86.8 865 [1]
Kepler-1410b Kepler-1410 K?V — 1.78 — 1.07 274 60.9 1196
Kepler-1540b Kepler-1540 K?V — 2.49 — 0.78 250 125.4 799
Kepler-1544 b Kepler-1544 K2V — 1.78 — 0.84 248 168.8 1092 [1]
Kepler-1606b Kepler-1606 G?V — 2.07 — 1.64 277 196.4 2710 [33]
Kepler-1649c Kepler-1649 M5V 1.20 1.06 — 0.75 237 19.5 301 [34]
Kepler-1652b Kepler-1652 M?V — 1.60 — 0.84 244 38.1 822
Kepler-1653b Kepler-1653 K?V — 2.17 — 1.04 258 140.3 2461
Kepler-1701b Kepler-1701 K?V — 2.22 — 1.42 275 169.1 1904 [1][35]
L 98-59 f L 98-59 M3V ≥2.46 — — >1 ~280 23.15 34.6 Not confirmed[36]
LHS 1140 b LHS 1140 M4V 5.60 1.73 5.9±0.3 0.43 226 24.7 49 Likely ocean world or dense mini-Neptune[37]
LP 890-9 c LP 890-9 M6V — 1.37 — 0.91 272 8.46 105 [38]
Luyten b Luyten's Star M3V ≥2.89 ~1.35 — 1.06 258 18.65 12.3 [39]
Proxima Centauri b Proxima Centauri M5V ≥1.07 [40]: 16  1.17±0.23 — 0.70 228 11.186 4.25 Affected by solar flare, possibly affected by high radiation[41]
Ross 128 b Ross 128 M4V ≥1.40 ~1.80 — 1.48 280 9.87 11.0 [42]
Ross 508 b Ross 508 M4V ≥4.00 — — 1.32 10.8 37 [43]
Teegarden's Star b Teegarden's Star M7V ≥1.05 ~1.02 — 1.15 264 4.91 12.5 Radius is estimated[44][45]
Teegarden's Star c Teegarden's Star M7V ≥1.11 ~1.04 — 0.37 199 11.4 12.5 [44]
TOI-700 d TOI-700 M2V ~1.72 1.14 — 0.87 246 37.4 101
TOI-700 e TOI-700 M2V 0.82 0.95 — 1.27[46] 273 27.8 101 [47]
TOI-715 b TOI-715 M4V 3.02 1.55 — 0.67 234 19.29 137 [48] [49]
TOI-2257 b TOI-2257 M3V 5.712+4.288
−2.311 		2.20 — 0.57 (0.26−2.25) 256+61
−17		 35.2 188 Highly eccentric[1][50]
TRAPPIST-1d TRAPPIST-1 M8V 0.39 0.78 3.39 1.12 258 4.05 41 Confirmed to be rocky[51][52]
TRAPPIST-1e TRAPPIST-1 M8V 0.69 0.92 5.65 0.65 230 6.1 41 Confirmed to be rocky[51][52]
TRAPPIST-1f TRAPPIST-1 M8V 1.04 1.04 3.3 ± 0.9 0.37 200 9.2 41 Confirmed to be rocky[51][52]
TRAPPIST-1g TRAPPIST-1 M8V 1.32 1.13 4.186 0.25 182 12.4 41 Confirmed to be rocky[51][52]
Wolf 1069 b Wolf 1069 M5V ≥1.26 ~1.08 — 0.65 250 15.6 31.2 [53]
Wolf 1061c Wolf 1061 M3V ≥3.41 ~1.60 — 1.30 271 17.9 13.8 [1]

Previous candidates

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Some exoplanet candidates detected by radial velocity that were originally thought to be potentially habitable were later found to most likely be artifacts of stellar activity. These include Gliese 581 d & g,[54][55][56] Gliese 667 Ce & f,[16][57] Gliese 682 b & c,[9] Kapteyn b,[58][59] and Gliese 832 c.[60]

HD 85512 b was initially estimated to be potentially habitable,[61][62] but updated models for the boundaries of the habitable zone placed the planet interior to the HZ,[63][64] and it is now considered non-habitable.[1] Kepler-69c has gone through a similar process; though initially estimated to be potentially habitable,[65] it was quickly realized that the planet is more likely to be similar to Venus,[66] and is thus no longer considered habitable.[1] Several other planets, such as Gliese 180 b, also appear to be examples of planets once considered potentially habitable but later found to be interior to the habitable zone.[1]

Similarly, Tau Ceti e and f were initially both considered potentially habitable,[67] but with improved models of the circumstellar habitable zone, as of 2022 PHL does not consider either planet potentially habitable.[1][failed verification] Kepler-438b was also initially considered potentially habitable; however, it was later found to be a subject of powerful flares that can strip a planet of its atmosphere, so it is now considered non-habitable.[1]

K2-3d and K2-18b were originally considered potentially habitable, and the latter remains listed in the HEC,[1] but recent studies have shown them to be gaseous sub-Neptunes and thus unlikely to be habitable.[68][69][70][71][72][73]

KOI-1686.01 was also considered a potentially habitable exoplanet after its detection in 2011, until proven a false positive by NASA in 2015.[74] Several other KOIs, like Kepler-577b and Kepler-1649b, were considered potentially habitable prior to confirmation, but with new data are no longer considered habitable.

See also

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References

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