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List of exoplanets discovered in 2024
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This list of exoplanets discovered in 2024 is a list of confirmed exoplanets that were first reported in 2024. For exoplanets detected only by radial velocity, the listed value for mass is a lower limit. See Minimum mass for more information.
| Name | Mass (MJ) | Radius (RJ) | Period (days) | Semi-major axis (AU) | Temp. (K) | Discovery method | Distance (ly) | Host star mass (M☉) | Host star temp. (K) | Remarks |
|---|---|---|---|---|---|---|---|---|---|---|
| 20 Leonis Minoris b | 0.02882+0.00173 −0.00176 |
31.15 | 0.1916±0.0007 | radial vel. | 48.64±0.07 | 0.967±0.01 | 5610±46 | [1] | ||
| 82 G. Eridani d | 0.01831±0.00179 | 647.6+2.5 −2.7 |
1.354±0.007 | radial vel. | 19.7 | 0.813+0.018 −0.012 |
5490±70 | Orbiting within the habitable zone of its host star.[2][3] | ||
| 2MASS J05581644–4501559 b | 6–12 | 1043 | imaging | 94.5 | 0.259±0.02[4] | 3218±158[4] | [5] | |||
| Barnard's Star b | 0.00116±0.00016 | 3.153 | 0.0229 | ~400 | radial vel. | 5.9629±0.0004 | 0.162±0.007 | 3195±28 | The closest exoplanet around a solitary star. Also located in the second closest star system to the Sun, after Alpha Centauri.[6] Not to be confused with the disproved planet Barnard's Star b of 2018, which shared the same name. | |
| BD+00 444b | 0.0151±0.0035 | 0.2108±0.0059 | 15.669 | 0.105±0.025 | 519±6 | transit | 77.99±0.036 | 0.642±0.026 | 4375±65 | [7] |
| BD-10 47 b | 0.0133±0.005 | 0.1529±0.0007 | 13.476 | 0.0943±0.0016 | 493±12 | transit | 65.89 | 0.616±0.032 | 4026±14 | Also known as TOI-260 b[8] |
| BD-14 3065 b | 12.11+0.95 −0.91 |
1.926±0.094 | 4.3 | 0.0646±0.0026 | 3520±130 | transit | 1847.4[9][a] | 1.4±0.06 | 6985±90 | Located in a triple star system. It orbits the primary component of the system (BD-14 3065 A), a subgiant star. Also known as TOI-4987 b[10] |
| BX Trianguli b | 7.5 | 3923 | 4.5 | timing | 192±7 | 0.51±0.02 (combined) | 3735±100 | [11] | ||
| CI Tauri c | 3.6±0.3 | 25.2±1.8 | 0.17 | radial vel. | 522.6±1.3 | 0.9±0.02 | 4250±50 | Highly eccentric orbit (e = 0.58). Cited as confirmed by NASA Exoplanet Archive and exoplanet.eu.[12][13] | ||
| CWISE J054129.32–745021.5 b | 1.8 | 6576 | imaging | 111 | Orbits a young red dwarf.[5] | |||||
| Gaia-4 b | 11.8+0.73 −0.66 |
571.3+1.4 −1.3 |
astrometry + radial vel. | 239.2±0.4 | 0.644+0.025 −0.023 |
4034±77 | [14] | |||
| Gaia20eae b | 6 | 0.062 | disk thermal instability | 9226+3130 −2021[15] |
1.15 | 4330±300[15] | First object detected by this method[16] | |||
| Gaia22dkvLb | 0.15 to 5.67+0.39 −0.38 |
219+47 −29 to 964+99 −106 |
0.48+0.01 −0.07 to 2.08+0.16 −0.18 |
microlensing | 3097±130 to 5477+326 −391 |
0.219+0.056 −0.039 to 1.3+0.04 −0.05 |
[17] | |||
| Gliese 12 b | 0.002769+0.00123 −0.0008 |
0.0892±0.0089[b] | 12.7 | 0.066±0.002 | 315±5 | transit | 39.65 | 0.241±0.006 | 3253±55 | [18] |
| Gliese 238 b | 0.05049±0.0012 | 1.74 | 0.02123+0.00016 −0.00017 |
758+16 −15 |
transit | 49.6 | 0.419±0.01 | 3485±140 | Mars-sized exoplanet, one of the smallest exoplanets currently known[19] | |
| Gliese 341 b | 0.00227±0.00044 | 0.0821±0.045 | 7.577 | 540 | transit | 33.9 | 0.506 | 3745 | Also known as TOI-741 b[20] | |
| Gliese 900 b | 10.5 | 460,000,000[21] | 12,000 | imaging | 68[22] | 1.08 (combined) | 3976[23] | Located in a three-star system.[24] It has the longest orbital time of any exoplanet so far at 1.4 million years.[25] | ||
| Gliese 1289 b | 0.01655+0.002958 −0.003052 |
111.74 | 0.27±0.01 | 150 | radial vel. | 28.88 | 0.21±0.02 | 3296±30 | [26] | |
| Gliese 4256 b | 0.00453±0.00044 | 0.0962±0.0058 | 0.238 | 0.0107[c] | 1340±60 | transit | 66.46±0.03 | 0.353±0.015 | 3421±70 | An ultra-short period planet orbiting close to the host star's Roche limit. It is expected to undergo tidal disruption in the next hundred million years. Also known as TOI-6255 b[27] |
| HD 21520 b | 0.02486+0.01007 −0.00944 |
0.2409±0.008 | 25.13 | 0.1726±0.0071 | 637+13 −12 |
transit | 258 | 1.09±0.07 | 5871±62 | [28] |
| HD 28185 c | 6.0±0.6 | 9088.5+474.5 −401.5 |
8.50+0.29 −0.26 |
astrometry + radial vel. | 127.8±0.1 | 0.974±0.018 | 5602±36 | Already known to exist in 2022, but was found to be an exoplanet—as opposed to a brown dwarf, in 2024.[29] | ||
| HD 48948 b | 0.0154±0.000661 | 7.34013±0.00040 | 0.0652±0.0005 | 715±10 | radial vel. | 54.915±0.0228 | 0.686+0.020 −0.013 |
4593±60 | [30] | |
| HD 48948 c | 0.0229±0.00220 | 37.920+0.026 −0.024 |
0.1951±0.0016 | 413±6 | radial vel. | [30] | ||||
| HD 48948 d | 0.0333±0.00315 | 150.95+0.45 −0.41 |
0.4894±0.0042 | 262±4 | radial vel. | Closest Super Earth in habitable zone around a K-dwarf star.[30] | ||||
| HD 63433 d | 0.09573±0.0141 | 4.21 | 0.0503±0.0027 | 1040±40 | transit | 71.7 | 0.99±0.03 | 5688±28 | Hot Earth-sized exoplanet[31] | |
| HD 73344 b | 0.00939+0.00787 −0.00599 |
0.2573+0.0073 −0.0064 |
15.6 | 0.131 | 911±7 | transit | 114.7+0.1 −0.0[32] |
1.20±0.02[32] | 6028±110[32] | The dayside temperature can be as high as 1,066 K if the planet is tidally locked.[33] |
| HD 73344 c | 0.367+0.022 −0.021 |
65.936 | 0.3388+0.0042 −0.0043 |
562±4[33] | radial vel. | |||||
| HD 73344 d | 2.55+0.56 −0.46 |
5746+120 −150 |
6.70+0.25 −0.26 |
radial vel. | True mass revealed using astrometry.[32] | |||||
| HD 75898 c | 8.49±0.65 | 6717±40 | 7.39±0.05 | astrometry + radial vel. | 263 | 1.28±0.13 | 6021±50 | [34] | ||
| HD 77946 b | 0.02637±0.00415 | 0.24133+0.00767 −0.0071 |
6.527 | 0.072±0.0012 | 1248+40 −38 |
transit | 322.7±1 | 1.17±0.06 | 6046.0±50.0 | Also known as TOI-1778 b[35] |
| HD 104067 c | 0.0415 | 13.8992+0.0047 −0.0037 |
0.1058±0.0013 | radial vel. | 66.34±0.03 | 0.82±0.03 | 4952±100 | [36] | ||
| HD 111520 b | ≥1 | 1,285,900 | ≥200 | disk kinematics | 352.6±0.7 | 1.350±0.215[37] | 6542±131[37] | [38] | ||
| HD 118203 c | 11.1+1.3 −1 |
5070 | 6.2±0.2 | 146±3 | astrometry + radial vel. | 300±0.5 | 1.353±0.006 | 5872±20 | [39] | |
| HD 128717 b | 12.8 | 1089.2 | 2.18 | astrometry | 240±0.5 | 1.17+0.06 −0.16 |
6158±115 | [40][41] | ||
| HD 134606 e | 0.00726+0.00113 −0.0011 |
4.32 | 0.0527±0.0012 | radial vel. | 87.4±0.068 | 1.046+0.07 −0.059 |
5576+86 −85 |
[42] | ||
| HD 134606 f | 0.01737+0.00232 −0.00229 |
26.915 | 0.1784±0.004 | radial vel. | 87.4±0.068 | 1.046+0.07 −0.059 |
5576+86 −85 |
[42] | ||
| HD 148193 Ab | 0.0894±0.0135 | 0.7476±0.017 | 20.38 | 0.1577 | transit | 626±3 | 1.261±0.183 | 6351±119 | The host star is orbited by two red dwarfs 157 and 1950 AU away.[43] Also known as TOI-1836 Ab | |
| HD 148193 Ac | 0.025 | 0.232+0.01972 −0.01285 |
1.773 | 0.03089±0.0005 | 2007.6+35.85 −29 |
transit | Also known as TOI-1836 Ac[44] | |||
| HD 156141 b | 0.0305±0.0060 | 0.211±0.005 | 21.269 | 0.154±0.003 | 694.1+11.2 −11.0 |
transit | 237.726+0.390 −0.389 |
1.09+0.034 −0.033 |
5814±137 | Also known as TOI-1742 b.[45] |
| HD 222237 b | 5.19±0.58 | 14,890+2120 −1643 |
10.8+1.1 −1.0 |
astrometry | 37.31±0.0 | 0.76±0.09 | 4751±139 | [46] | ||
| HD 278878 b | 0.6963±0.0242 | 0.9225±0.0571 | 8.71 | 0.08258 | transit | 520.8±4.9 | 0.989±0.126 | 5597±147 | [47] | |
| HIP 39017 b | 23.6+9.1 −7.4 |
0.87 | 30681+18627.8 −9496.5 |
22.1+8.0 −4.9 |
imaging | 214.9±0.3 | 1.52+0.28 −0.26 |
7201+142 −112[48] |
May be a brown dwarf. Estimates of the mass vary from 13.8 MJ to 30+31 −12 MJ.[49] | |
| HIP 67522 c | 0.731+0.055 −0.057 |
14.335 | 0.1235 | 915+22 −19 |
transit | 414[50] | 1.2±0.05[50] | 5675±75[50] | [51] | |
| HS Piscium b | 1.44+0.56 −0.44 |
3.986 | 0.0435±0.0017 | radial vel. | 122.79+0.12 −0.14 |
0.69±0.07 | 4203±116 | [52] | ||
| IRAS 04125+2902 b | 0.3 | 0.955 | 8.83 | transit | 520[53] | 0.7 | 3720[54] | [55] The youngest transiting exoplanet discovered to date.[56] | ||
| Kepler-51e | 0.01572 | 260 | timing | 2610±50 | 1.04 | 6018 | Assuming the 2:1 resonance solution, which is the best-fit one, Kepler-51e has a mass of about 5 ME and a period of 260 days.[57] | |||
| Kepler-158d | 0.038±0.004 | 0.645088±0.000002 | transit | 1028±7 | 0.656+0.073 −0.049 |
4895.97 | [58] | |||
| Kepler-879c | 0.04±0.01 | 0.646716±0.000003 | transit | 2618+36 −35 |
0.974+0.127 −0.104 |
5456.75 | [58] | |||
| Kepler-963c | 0.05±0.02 | 0.919783±0.000003 | transit | 2516+42 −40 |
0.821+0.120 −0.065 |
5169.47 | [58] | |||
| Kepler-1489c | 0.045±0.007 | 0.680741±0.000004 | transit | 4185+118 −111 |
0.977+0.050 −0.062 |
5565.53 | [58] | |||
| Kepler-2003b | 0.06±0.01 | 0.941967±0.000003 | transit | 3054+85 −81 |
0.859+0.126 −0.065 |
5050.28 | Also known as KOI-4978 b.[58] | |||
| K2-360 b | 0.02413±0.00236 | 0.01435±0.00072 | 0.87724±0.00004 | 0.0177±0.0003 | 2038±39 | transit | 762.59±19.05 | 0.958±0.048 | 5679+60 −39 |
Ultra-dense super-Earth.[59] |
| K2-360 c | 0.0479±0.0024 | 9.797±0.030 | 0.0883±0.0016 | 912±18 | radial vel. | [59] | ||||
| K2-419 Ab | 0.617±0.047 | 0.941±0.034 | 20.358 | 0.1208+0.0016 −0.0017 |
377±11 | transit | 860±8 | 0.562±0.024 | 3711±88 | [60] |
| KMT-2016-BLG-2321Lb | 3.58±1.22 | 3.58±0.81 | microlensing | 11,670±3980 | 0.73±0.28 | [61] | ||||
| KMT-2017-BLG-0849Lb | 0.0201+0.0245 −0.0097 |
2.73+0.68 −0.62 |
microlensing | 23,540+2670 −3220 |
0.19+0.23 −0.09 |
[62] | ||||
| KMT-2017-BLG-1057Lb | 0.0739+0.0472 −0.0378 |
2.36+0.69 −0.62 |
microlensing | 21,190+2640 −5280 |
0.57+0.37 −0.29 |
[62] | ||||
| KMT-2017-BLG-2331Lb | 0.538+0.431 −0.277 |
2.14+0.48 −0.42 |
microlensing | 26,180+2740 −3420 |
0.4+0.32 −0.21 |
[62] | ||||
| KMT-2020-BLG-0157Lb | 10.71+6.17 −5.61 |
11.54+1.61 −2.25 |
microlensing | 21,744+3032 −4238 |
0.58+0.33 −0.30 |
[63] | ||||
| KMT-2021-BLG-2609Lb | 0.032+0.044 −0.018 or 0.112+0.152 −0.061 |
2.30+0.32 −0.36 |
microlensing | 24,380+3420 −3810 |
0.20+0.27 −0.11 |
[64] | ||||
| KMT-2022-BLG-0303Lb | 0.513+0.410 −0.275 |
4.81+0.65 −0.76 |
microlensing | 21,400+2900 −3400 |
0.368+0.294 −0.197 |
[64] | ||||
| KMT-2022-BLG-0732Lb | 1.12±0.65 | 4.11+0.74 −1.14 |
microlensing | 21,712+3879 −6000 |
0.54±0.31 | [63] | ||||
| KMT-2022-BLG-1787Lb | 6.64+4.98 −3.64 |
6.3+0.75 −1.08 |
microlensing | 24,613+2901 −4038 |
0.42+0.32 −0.23 |
[63] | ||||
| KMT-2022-BLG-1852Lb | 4.98+5.42 −2.94 |
5.03+0.72 −0.92 |
microlensing | 20,440+2934 −3749 |
0.32+0.34 −0.19 |
[63] | ||||
| KMT-2023-BLG-0416Lb | 6.15+3.03 −3.2 |
3.73+0.56 −0.8 |
microlensing | 20,640+3100 −4400 |
0.61+0.3 −0.32 |
The mass of the planet can be as low as 0.042+0.021 −0.022 MJ.[65] | ||||
| KMT-2023-BLG-0469Lb | 0.124+0.092 −0.067 |
2.37±0.9 | microlensing | 23,050+3260 −3910 |
0.47±0.36 | [66] | ||||
| KMT-2023-BLG-0735Lb | 0.12±0.07 | 2.75±1 | microlensing | 20,830+3910 −3260 |
0.61±0.34 | [66] | ||||
| KMT-2023-BLG-1431Lb | 0.0428+0.0261 −0.0217 |
2.3±0.5 or 3.2+0.7 −0.8 |
microlensing | 22,500+2610 −5540 |
0.57+0.33 −0.29 |
[67] | ||||
| KMT-2023-BLG-1454Lb | 0.63+0.71 −0.34 |
1.18+0.17 −0.18 |
microlensing | 23,540+3460 −3590 |
0.17+0.19 −0.09 |
Estimates of the planet's mass varies between 0.3+0.34 −0.16 MJ and 0.77+0.87 −0.42 MJ[65] | ||||
| KMT-2023-BLG-1642Lb | 1.08+1.53 −0.58 |
1.41+0.22 −0.27 |
microlensing | 22,750+3550 −4370 |
0.17+0.24 −0.09 |
[65] | ||||
| KMT-2023-BLG-1866Lb | 0.00828+0.00132 −0.00214 |
2.63+0.37 −0.34 |
microlensing | 20,240+2840 −1100 |
0.51+0.08 −0.13 |
Super-Earth planet detected by microlensing.[68] | ||||
| KMT-2023-BLG-2669 | 0.02517 | microlensing | Candidate rogue planet. Might have a mass ranging from sub-Neptune to Saturn-mass, depending on its distance.[69] | |||||||
| KMT-2024-BLG-1044L | 0.0244+0.0378 −0.0127 or 0.0430+0.0479 −0.0211 |
microlensing | 21,900+3200 −3400 or 23,300±3100 |
0.069+0.080 −0.036 or 0.131+0.146 −0.064 |
Host star is either a brown dwarf or a red dwarf.[70] | |||||
| LHS 1678 d | 0.00289+0.00208 −0.00107 |
0.08752±0.0062 | 4.965 | 0.04+0.0018 −0.0017 |
transit | 65 | 0.345±0.014 | 3490±50 | [71] | |
| M62H b | 2.83 | <0.683 [d][e] | 0.133 | 0.004908 | timing | 21,500[72] | 1.4 | Pulsar planet located in the globular cluster Messier 62.[73] Second shortest orbit of any confirmed exoplanet after PSR J1719-1438 b.[74] | ||
| MOA-2016-BLG-526Lb | 6.93±0.75 | 2.07±0.35 | microlensing | 22,490 | 0.4 | [61] | ||||
| MOA-2022-BLG-563Lb | 0.4+0.31 −0.25 |
2.25±0.25 | microlensing | 21,290+3650 −5220 |
0.48+0.36 −0.3 |
[66] | ||||
| NGTS-26 b | 0.29+0.07 −0.06 |
1.33+0.06 −0.05 |
4.52 | 0.0490+0.0038 −0.0032 |
1331+85 −72 |
transit | 3610±100 | 0.96+0.04 −0.03 |
5550±100 | Highly inflated planet (density = 0.153 g/cm3)[75] |
| NGTS-27 b | 0.593+0.095 −0.072 |
1.396+0.038 −0.035 |
3.37 | 0.0446+0.0026 −0.0036 |
1783+104 −88 |
transit | 3185±55 | 1.07±0.06 | 5700±80 | [75] |
| NGTS-29 b | 0.393 | 0.857 | 69.33 | 0.347 | 414 | transit | 487±1 | 1.034±0.032 | 5730±80 | [76] |
| NGTS-30 b | 0.96 | 0.93 | 98.3 | 0.408 | 390 | transit | 762.5 | 0.94 | 5455 | Also known as TOI-4862 b[77] |
| NGTS-33 b | 3.6±0.3 | 1.64±0.07 | 2.828 | 0.048±0.02 | 1991±21 | transit | 1430±23 | 1.60±0.11 | 7437±72 | [78] |
| OGLE-2014-BLG-0221Lb | 4.35+1.65 −1.91 |
3.76+0.96 −1.07 |
microlensing | 12,000+3690 −3780 |
0.69+0.26 −0.30 |
[79] | ||||
| OGLE-2016-BLG-1598Lb | 5.91±1.74 | 2.5±0.88 | microlensing | 19,270±5670 | 0.55±0.32 | [61] | ||||
| OGLE-2016-BLG-1800Lb | 2.59±1.46 | 1.88±0.51 | microlensing | 21,100±3360 | 0.41±0.22 | [61] | ||||
| OGLE-2017-BLG-0364Lb | 0.0642+0.106 −0.034 to 0.805+0.554 −0.437 |
1.27+0.49 −0.3 |
microlensing | 22,300 to 29,300 | 0.1+0.16 −0.05 to 0.55+0.38 −0.3 |
[62] Assuming the largest distance, it would be the most distant confirmed exoplanet, surpassing SWEEPS-04/11.[74] | ||||
| OGLE-2017-BLG-0380Lb A | 10.5 | microlensing | 6,980 | A pair of rogue planets.[80] | ||||||
| OGLE-2017-BLG-0380Lb B | 3.08 | microlensing | 6,980 | |||||||
| OGLE-2017-BLG-0640Lb | 1.62+1.64 −0.94 |
1.14±0.38 | microlensing | 21,600+3550 −4730 |
0.32+0.32 −0.18 |
[81] | ||||
| OGLE-2017-BLG-1237Lb | 3.8+2.49 −1.99 |
2.53+0.5 −0.64 |
microlensing | 19,660+3060 −4990 |
0.46+0.3 −0.24 |
[81] | ||||
| OGLE-2017-BLG-1275Lb | 5.9±2.2 | 1.19±0.36 | microlensing | 25,070±2930 | 0.63±0.23 | Another solution suggests a larger semi-major axis, of 2.09±0.63 AU.[81] | ||||
| OGLE-2023-BLG-0836Lb | 4.36+2.35 −2.2 |
3.7+1 −1.2 |
microlensing | 16,690+4430 −5250 |
[f] | The planet is located in a binary star system, and is likely to be orbiting both stars in the system.[82] | ||||
| S1429 b | 1.8±0.2 | 77.51±0.2 | 0.384±0.4 | 683±9 | radial vel. | 2836±26 | 1.26±0.04 | 6000±40 | Located in the open cluster Messier 67.[83] | |
| SGR 1935+2154 b | 0.0318 – 0.0573 | 0.125 – 0.223 | 238 or 398 | 0.85 or 1.19 | x-ray bursts | 21,500[84]–28,400 | 1.4 | Has a highly-eccentric orbit (0.992) and is tidally disrupted.[85] | ||
| SPECULOOS-3 b | 0.08716 | 0.719 | 0.00733 | 553 | transit | 57.9 | 0.1 | 2800 | Ultra-short period planet[86] | |
| Struve 2398 Ab | 0.00875±0.0011 | 0.107–0.178 | 11.2201±0.0051 | 0.068±0.001 | radial vel. | 11.4 | 0.330±0.008 | 3470±31 | [87] | |
| Teegarden's Star d | 0.00258±0.00053 | 26.13 | 0.0791 ±0.0027 | 159±3 | radial vel. | 12.5 | 0.097±0.01 | 3034±45 | Orbits beyond the habitable zone of its star. Another planet in the system is suspected.[88] | |
| TIC 4672985 b | 12.74±1.01 | 1.026+0.065 −0.067 |
69.05 | 0.33±0.019 | 517.2+11.3 −11.2 |
transit | 823.4[89][a] | 1.01±0.03 | 5757+72 −65 |
[90] |
| TIC 46432937 b | 3.2±0.11 | 1.188±0.03 | 1.44 | 0.1951±0.0051 | 872±14 | transit | 295.5±0.3 | 0.563±0.029 | 3572±57 | [91] |
| TIC 139270665 b | 0.463 | 0.645 | 23.624 | 0.163 | 700 | transit | 618 | 1.035+0.052 −0.062 |
5844+84 −82 |
[92][93] |
| TIC 139270665 c | 4.89+0.66 −0.37 |
1010+780 −220 |
2+0.93 −0.31 |
200+18 −35 |
radial vel. | [93] | ||||
| TIC 241249530 b | 4.98+0.16 −0.18 |
1.19±0.04 | 165.772 | transit | 1.271+0.061 −0.068 |
A planet on a highly-eccentric (e=0.94) and retrograde orbit.[94] | ||||
| TIC 393818343 b | 4.34±0.15 | 1.087+0.023 −0.021 |
16.25 | 0.129±0.002 | 805.5+9.6 −9.4 |
transit | 306.3±1.1 | 1.082+0.055 −0.056 |
5756+57 −66 |
Highly eccentric orbit (e=0.6058)[95] Also known as TOI-6883 b[96] |
| TIC 393818343 c | 0.357±0.132 | 0.792±0.018 | 7.8458±0.0023 | 0.079±0.011 | 1027.2089± 0.3717 | transit | [97] | |||
| TIC 434398831 b | 0.3131+0.0196 −0.0187 |
3.6855 | 0.04641±0.00017 | 1250±11 | transit | 698±6 | 0.992+0.014 −0.018 |
5638±50 | Young exoplanet located in the Theia 116 association.[98] | |
| TIC 434398831 c | 0.5023+0.0259 −0.025 |
6.21 | 0.06572±0.00024 | 1050±10 | transit | |||||
| TOI-128 b | 0.198 | 4.94 | 0.054 | 1345 | transit | 0.85 | 6086 | [99] | ||
| TOI-238 c | 0.0211±0.0035 | 0.1945±0.0161 | 8.466 | 0.0749±0.0013 | 696±15 | transit | 261.328±0.312 | 0.79±0.022 | 5059±89 | [100] |
| TOI-261 b | 0.271 | 3.36 | 0.035 | 1722 | transit | 0.50 | 5890 | [99] | ||
| TOI-286 b | 0.01425±0.00245 | 0.1267±0.0089 | 4.512 | 0.0503±0.001 | 979±31 | transit | 193 | 0.832±0.049 | 5152±12 | There are three available models to explain the disagreement between the radial velocity and transit measurements.[g][8] |
| TOI-286 c | 0.01171±0.00698 | 0.1677±0.0107 | 39.36 | 0.213±0.004 | 475±15 | transit | 193 | 0.832±0.049 | 5152±12 | [8] |
| TOI-329 b | 0.1271 | 5.71 | 0.064 | transit | 927.1 | 0.98 | 5560 | Radius of the host star is significantly larger compared to mass (1.61 R☉)[101] | ||
| TOI-406 b | 0.00654+0.00072 −0.00069 |
0.1178±0.0107 | 3.307 | 0.0322±0.0013 | 584±22 | transit | 101±0.7 | 0.408+0.046 −0.042 |
3392±44 | [102] |
| TOI-406 c | 0.02067±0.003 | 0.1846±0.0143 | 13.18 | 0.0809±0.003 | 368±14 | transit | 101±0.7 | 0.408+0.046 −0.042 |
3392±44 | [102] |
| TOI-480 b | 0.0654 | 6.866 | transit | 177.8 | 1.2 | 6,212 | [103] | |||
| TOI-603 b | 0.1495±0.0431 | 0.7075±0.018 | 16.18 | 0.1281 | transit | 671.3±5.15 | 1.072±0.136 | 5901±130 | [104] | |
| TOI-654 b | 0.211 | 1.53 | 0.021 | 749 | transit | 0.53 | 3433 | [99] | ||
| TOI-663 b | 0.0140±0.00204 | 0.203±0.00892 | 2.599 | 0.0295±0.0011 | 674±30 | transit | 209.490±0.587 | 0.514±0.012 | 3681±70 | [105] |
| TOI-663 c | 0.0115±0.00305 | 0.202±0.00892 | 4.696 | 0.0437±0.0016 | 553±24 | transit | ||||
| TOI-663 d | <0.0164 | 0.171±0.0116 | 7.103 | 0.0576+0.0021 −0.0022 |
482±21 | transit | ||||
| TOI-757 b | 0.033±0.007 | 0.223±0.001 | 17.468 | 0.122±0.002 | 641±10 | transit | 196.9+1 −0.7 |
0.8±0.04 | 5278±63 | [106] |
| TOI-762 Ab | 0.251±0.042 | 0.744±0.017 | 3.472 | 0.03418 | 555±6 | transit | 322±0.7 | 0.442±0.025 | 3266±36 | Located in a binary star system.[91] |
| TOI-782 b | <0.06 | 0.244±0.008 | 8.024 | 0.0578±0.0018 | 398±6–435±6[h] | transit | 170.2±0.2 | 0.397±0.01 | 3370+29 −32 |
[107] |
| TOI-815 b | 0.0239±0.0047 | 0.2622±0.0044 | 11.197 | 0.0903+0.0018 −0.0019 |
686+13 −14 |
transit | 193.76±0.15 | 0.776±0.036 | 4869±77 | The host star is part of a binary star system with a red dwarf companion[108] |
| TOI-815 c | 0.0739±0.00755 | 0.2337+0.0089 −0.008 |
34.976 | 0.193±0.004 | 469±9 | transit | ||||
| TOI-880 b | 0.248 | 2.57 | 0.034 | 1163 | transit | 0.81 | 4935 | [99] | ||
| TOI-907 b | 0.858 | 4.58 | 0.055 | 1847 | transit | 1.07 | 6272 | [99] | ||
| TOI-1011 b | 0.01271±0.00186 | 0.1294±0.0045 | 2.47 | 0.0346 | transit | 0.92±0.03 | 5475±84 | [109] | ||
| TOI-1135 b | 0.062+0.033 −0.031 |
0.805±0.02 | 5.13±0.27 | 0.082±0.003 | 1198.9±21.3 | transit | 371.4±0.5 | 1.125±0.032 | 6122±25 | [110] |
| TOI-1173 Ab | 0.08213±0.00598 | 0.723±0.015 | 7.064 | 0.0702±0.0012 | 863.9±9.8 | transit | 430.85[111][a] | 0.911+0.028 −0.03 |
5350±340 | Low-density planet located in a wide binary system.[112] |
| TOI-1184 b | 0.021±0.007 | 0.215+0.009 −0.013 |
5.748 | 0.056±0.001 | 715.5+13.7 −14.1 |
transit | 191.110±0.254 | 0.73+0.024 −0.025 |
4616±104 | [45] |
| TOI-1199 b | 0.239±0.02 | 0.938±0.025 | 3.671 | 0.04988±0.0009 | 1486±20 | transit | 805±2.6 | 1.23±0.07 | 5710±40 | [113] |
| TOI-1224 b | 0.1877+0.0084 −0.0081 |
4.178 | 0.0355+0.0017 −0.0034 |
541+26 −14 |
transit | 121.5 | 0.4±0.01 | 3326±66 | Located in the MELANGE-5 association, which is 200 Myr old. The host star may be binary.[114] | |
| TOI-1224 c | 0.2573±0.0087 | 17.945 | transit | |||||||
| TOI-1248 b | 0.0862+0.0113 −0.0110 |
0.607+0.0104 −0.0107 |
4.360 | 0.051±0.001 | 952.1+13.5 −14.3 |
transit | 550.340+1.963 −1.947 |
0.90±0.03 | 5205±120 | [45] |
| TOI-1249 b | 0.0374+0.0164 −0.0160 |
0.2918+0.0274 −0.0167 |
13.079 | 0.109±0.002 | 727+12 −11 |
transit | 455.0+1.8 −1.7 |
0.952+0.167 −0.082 |
5453+76 −160 |
[115] |
| TOI-1266 d | 0.01158+0.00330 −0.00349 |
32.5 | 0.1513±0.0024 | 288±5 | radial vel. + timing | 117.4±0.1 | 0.437±0.021 | 3563±77 | [116] | |
| TOI-1269 b | 0.020±0.009 | 0.2142+0.0134 −0.0066 |
4.253 | 0.0496+0.0009 −0.0010 |
1005+15 −14 |
transit | 561.4±2.3 | 0.969+0.154 −0.104 |
5517+107 −143 |
[117] |
| TOI-1273 b | 0.222±0.015 | 0.99±0.2 | 4.631 | 0.0549±0.001 | 1211±15 | transit | 574±1.3 | 1.06±0.06 | 5690±40 | [113] |
| TOI-1279 b | 0.0334±0.0079 | 0.237+0.0123 −0.0095 |
9.61419±0.00004 | 0.085±0.002 | 759+11.8 −11.7 |
transit | 349.167+0.933 −0.926 |
0.88±0.03 | 5457±127 | [45] |
| TOI-1294 b | 0.1957±0.016 | 0.8199±0.0277 | 3.915 | 0.0489 | transit | 1052±7 | 1.02±0.13 | 5714±126 | [118] | |
| TOI-1294 c | 0.467±0.053 | 160.1±2.5 | 0.581 | radial vel. | 1052±7 | 1.02±0.13 | 5714±126 | [119] | ||
| TOI-1347 b | 0.0349±0.0038 | 0.161±0.009 | 0.847 | 1400±40 | transit | 480.8±2 | 0.913±0.033 | 5464±100 | Ultra-short period planet[120] | |
| TOI-1347 c | 0.0088±0.0072 | 0.143±0.009 | 4.842 | 1000±25 | transit | [120] | ||||
| TOI-1386 b | 0.148+0.019 −0.018 |
0.54+0.018 −0.016 |
25.838 | 0.1732+0.0027 −0.0033 |
676.4+10 −8.3 |
transit | 478.8±2.2 | 1.038+0.05 −0.058 |
5793+76 −73 |
[121] |
| TOI-1386 c | 0.309±0.038 | 227.6+4.6 −4 |
0.739+0.015 −0.016 |
327.4+5.3 −4.6 |
radial vel. | 478.8±2.2 | 1.038+0.05 −0.058 |
5793+76 −73 |
[121] | |
| TOI-1408 c | 0.0239±0.0006 | 0.1981±0.0054 | 2.1664±0.0001 | 0.3587±0.0008 | timing | 435.6±0.7 | 1.31±0.01 | 6117±31 | [122] | |
| TOI-1410 b | 0.262 | 1.22 | 0.020 | 1396 | transit | 0.72 | 4635 | [99] | ||
| TOI-1437 b | 0.0302+0.0123 −0.0104 |
0.200+0.021 −0.020 |
18.841 | 0.140+0.018 −0.017 |
794±14[123] | transit + radial vel. | 336 | 1.10±0.10 | 6008±113 | [124] |
| TOI-1439 b | 0.121±0.018 | 0.379+0.021 −0.015 |
27.644 | 0.192±0.004 | 748.4+10.9 −13.1 |
transit | 751.158+7.691 −7.537 |
1.24 | 5857±60 | [125] |
| TOI-1443 b | <0.0944 | 0.2055+0.0113 −0.0090 |
23.541 | 0.147±0.003 | 521+14 −12 |
transit | 279.9±0.7 | 0.89+0.14 −0.09 |
5236+111 −140 |
[126] |
| TOI-1448 b | <0.0613 | 0.245±0.006 | 8.112 | 0.0567±0.0015 | 389±5–426±6[h] | transit | 240±0.3 | 0.372±0.009 | 3412+28 −32 |
[107] |
| TOI-1450 Ab | 0.00396±0.0004 | 0.1±0.004 | 2.04 | 722±35 | transit | 73.2±0.1 | 0.48±0.024 | 3437±86 | Located in a binary star system. It is the second-lowest mass transiting planet with a high-precision mass measurement.[127] | |
| TOI-1450 Ac | 0.0048±0.0006 | 5.07 | 533±26 | radial vel. | Located in a binary system, its true mass could be similar to the minimum mass assuming coplanarity with TOI-1450 Ab.[127] | |||||
| TOI-1451 b | 0.0478±0.0088 | 0.233+0.0120 −0.0092 |
16.538 | 0.127±0.003 | 723.3+12.4 −12.2 |
transit | 299.856+0.710 −0.707 |
1.00+0.04 −0.03 |
5800±139 | [45] |
| TOI-1472 b | 0.0519±0.0160 | 0.371+0.0140 −0.0113 |
6.36381±0.00091 | 0.065±0.001 | 811.1+11.2 −10.8 |
transit | 397.389+4.341 −4.250 |
0.92±0.02 | 5103+119 −144 |
[45] |
| TOI-1669 b | <0.0409 | 0.2049+0.0091 −0.0080 |
2.68 | 0.0376±0.0007 | 1285+22 −21 |
transit | 362.9±1.2 | 1.00±0.05 | 5542±100 | [128] |
| TOI-1683 b | 0.236 | 3.06 | 0.037 | 929 | transit | 0.69 | 4402 | [99] | ||
| TOI-1691 b | 0.0459+0.0170 −0.0167 |
0.3181+0.0096 −0.0078 |
16.737 | 0.126±0.003 | 703+13 −12 |
transit | 363.5±1.2 | 1.031+0.159 −0.127 |
5759+209 −165 |
[129] |
| TOI-1723 b | 0.2937+0.0127 −0.0114 |
13.72641±0.00046 | 0.114±0.002 | 783+15 −14 |
transit | 328.5±1.0 | 1.035+0.147 −0.107 |
5777+149 −101 |
[130] | |
| TOI-1751 b | 0.0538±0.0101 | 0.2489±0.0259 | 37.468 | 0.2115±0.0024 | 820 | transit | 370.3±0.3 | 1.15±0.17 | 6116±22 | The host star is metal-poor ([Fe/H] = –0.40 dex).[131] |
| TOI-1753 b | 0.0522±0.0164 | 0.221+0.009 −0.007 |
5.385 | 0.059±0.001 | 1005.4+18.3 −17.6 |
transit | 739.302+8.907 −8.699 |
0.95±0.03 | 5620±134 | [45] |
| TOI-1758 b | 0.3174+0.0203 −0.0127 |
20.705 | 0.138±0.003 | 551+9 −8 |
transit | 315.1±1.1 | 0.88+0.12 −0.09 |
5169+95 −148 |
[132] | |
| TOI-1775 b | 0.302±0.047 | 0.718+0.0128 −0.0114 |
10.241 | 0.080±0.002 | 707.9+8.6 −8.3 |
transit | 486.736+3.108 −3.072 |
0.92+0.01 −0.02 |
5283±116 | [45] |
| TOI-1776 b | 0.1085+0.0080 −0.0069 |
2.8 | 0.0378+0.0007 −0.0008 |
1269±21 | transit | 146 | 1.02+0.11 −0.14 |
5724±105 | [133] | |
| TOI-1798 b | 0.126 | 0.44 | 0.011 | 2122 | transit | 369.147+1.008 −1.005 |
0.86 | 5165 | [99] | |
| TOI-1798 c | 0.018+0.003 −0.002 |
0.125+0.006 −0.005 |
0.438 | 0.0107±0.0002 | 1935.8+25.2 −25.9 |
transit | [45] | |||
| TOI-1799 b | 0.013+0.005 −0.006 |
0.1269+0.0932 −0.0880 |
7.085738±0.000083 | 0.071±0.001 | 923+15 −14 |
transit[ | 203 | 1.01+0.14 −0.12 |
5690+121 −124 |
[134] |
| TOI-1806 b | 0.304 | 15.15 | 0.088 | 337 | transit | 0.39 | 3272 | [99] | ||
| TOI-1823 b | 0.212+0.025 −0.026 |
0.673+0.030 −0.022 |
38.80±0.01 | 0.212±0.004 | 423.6+10.4 −8.7 |
transit | 233.677+0.375 −0.374 |
0.84±0.03 | 4926±113 | [45] |
| TOI-1824 b | 0.0582±0.01 | 0.2346±0.0133 | 22.8 | 0.149±0.003 | 577±19 | transit | 192.3 | 0.85±0.05 | 5180±110 | High-density planet, situated in the small group of "overdense sub-Neptunes". TOI-1824 has also a red dwarf companion named TIC 142387022.[135] |
| TOI-1828 b | 0.1841±0.012 | 0.769±0.017 | 9.09 | 0.0859 | transit | 1208±8 | 1.04±0.13 | 5809±127 | [136] | |
| TOI-1855 b | 1.133±0.096 | 1.65+0.52 −0.37 |
1.364 | 0.02398+0.00037 −0.00036 |
1700±20 | transit + radial vel. | 576.3±4.6 | 0.987+0.058 −0.045 |
5359+89 −83 |
[137] |
| TOI-1883 b | 0.4953±0.0460 | 4.506 | 524.9 | transit | 376±3 | 0.492±0.02 | 3477±157 | [138][139] | ||
| TOI-1885 b | 1.624±0.103 | 1.219±0.037 | 6.544060±0.000006 | transit | 1826.773+21.464 −20.982 |
6527±98 | [125] | |||
| TOI-1898 b | 0.4059+0.0220 −0.0252 |
0.838+0.021 −0.028 |
45.52 | 0.269±0.005 | 674.5+11.6 −11.8 |
transit | 259.7±1.4 | 1.24+0.22 −0.16 |
6304+139 −144 |
[140] |
| TOI-2019 b | 0.109±0.0132 | 0.505±0.0250 | 15.3444±0.0055 | transit | 645.812+2.684 −2.665 |
5590 | [125] | |||
| TOI-2107 b | 0.83±0.11 | 1.211±0.035 | 2.454 | 0.0315+0.0006 −0.00067 |
1397±20 | transit + radial vel. | 767.4+6.2 −5.9 |
0.961+0.049 −0.054 |
5627+94 −93 |
[137] |
| TOI-2120 b | <0.02139 | 0.1893±0.0056 | 5.8 | 0.0377±0.0013 | 351±6–384±6[h] | transit | 104.9 | 0.211±0.005 | 3131±30 | [107] |
| TOI-2128 b | 0.014±0.006 | 0.186+0.008 −0.007 |
16.341 | 0.127±0.003 | 780.5+14.8 −14.4 |
transit | 119.2±0.1 | 1.1+0.15 −0.12 |
5991+114 −90 |
[141] |
| TOI-2266 b | 0.1374±0.008 | 2.326 | 0.02±0.002 | 550±47 | transit | 168.6±0.2 | 0.23±0.02 | 3240±160 | [142] | |
| TOI-2274 b | 2.679 | 771 | transit | 159.9±0.2 | 0.612±0.02 | 3943±157 | [143][139] | |||
| TOI-2368 b | 0.65±0.18 | 0.967+0.036 −0.031 |
5.175 | 0.05649±0.001 | 1000+44 −30 |
transit | 685±3.9 | 0.897+0.048 −0.049 |
5360+230 −170 |
[137] |
| TOI-2373 b | 9.3±0.2 | 0.93±0.02 | 13.337 | 0.112±0.001 | 860±10 | transit | 1617±33 | 1.041+0.032 −0.028 |
5651±180 | [144] |
| TOI-2374 b | 0.1782+0.011 −0.0134 |
0.6075±0.0268 | 4.314 | 0.0471 | <885±22 | transit | 439±3 | 0.75±0.01 | 4802±97 | [145] |
| TOI-2379 b | 5.76±0.20 | 1.046±0.023 | 5.4693827±0.0000023 | 0.05263±0.00091 | 624±12 | transit | 689.5±3.6 | 0.645±0.033 | 3707±58 | [146] |
| TOI-2384 b | 1.966±0.059 | 1.025±0.021 | 2.13570304±0.00000038 | 0.02793±0.00023 | 889.7±5.0 | transit | 609.9±4.9 | 0.635±0.016 | 3943±14 | [146] |
| TOI-2416 b | 3+0.1 −0.09 |
0.88±0.02 | 8.275 | 0.0831±0.0007 | 1080±10 | transit | 1767±261 | 1.118+0.029 −0.027 |
5808±80 | [144] |
| TOI-2420 b | 0.927+0.085 −0.079 |
1.340+0.074 −0.072 |
5.8426 | 0.0684+0.0067 −0.0059 |
1571.6+60.8 −64 |
transit | 1450[a] | 1.158±0.098 | [147] | |
| TOI-2485 b | 2.412+0.088 −0.087 |
1.083±0.045 | 11.235 | 0.1093+0.0055 −0.0057 |
1134+27 −25 |
transit | 1296[a] | 1.163±0.053 | [147] | |
| TOI-2524 b | 0.64±0.04 | 1+0.02 −0.03 |
7.186 | 0.073±0.0007 | 1100±20 | transit | 1399±36 | 1.007+0.032 −0.029 |
5831±80 | [144] |
| TOI-2529 b | 2.34±0.2 | 1.03±0.05 | 64.5949±0.0003 | 0.327±0.02 | 636±15.7 | transit | 965.8+14 −13.7 |
1.11+0.02 −0.02 |
5802+60 −52 |
[90] |
| TOI-2714 b | 0.717+0.104 −0.101 |
1.224+0.0625 −0.0598 |
2.499 | 0.036±0.002 | 1603±65 | transit | 1930±16 | 1.07±0.06 | 5665±115 | [148] |
| TOI-2768 b | 0.2688±0.0313 | 1.508 | 855 | transit | 255.8±0.6 | 0.63+0.06 −0.10 |
4008+124 −137 |
[149][139] | ||
| TOI-2981 b | 2.007±0.104 | 1.1955±0.0375 | 3.602 | 0.048±0.002 | 1358±39 | transit | 1741±16 | 1.03±0.06 | 5940±75 | [148] |
| TOI-3071 b | 0.2146±0.011 | 0.6388+0.0509 −0.0455 |
1.267 | 0.0249 | <2155±40 | transit | 1582±29 | 1.29±0.02 | 6177±62 | [145] |
| TOI-3261 b | 0.0953±0.0076 | 0.3408+0.0375 −0.0312 |
0.883 | 0.01714 | 1722+26 −18 |
transit | 972.3+2.3 −3.1 |
0.861+0.02 −0.03 |
4995±47 | Ultra-hot Neptune[150] |
| TOI-3321 b | 0.554±0.076 | 1.388+0.070 −0.064 |
3.652 | 0.047±0.001 | 1616±30 | transit | 928+10.8 −10.4 |
1.041+0.084 −0.068 |
5850±140 | [137] |
| TOI-3353 b | 0.238 | 4.67 | 0.060 | 1264 | transit | 1.33 | 6365 | [99] | ||
| TOI-3568 b | 0.083±0.003 | 0.473±0.024 | 4.42 | 0.0485±0.0004 | 899±12 | transit | 645±2 | 0.78±0.02 | 4969±45 | [151] |
| TOI-3894 b | 0.85±0.15 | 1.358+0.054 −0.052 |
4.335 | 0.0543±0.0014 | 1519±22 | transit | 1343+12.7 −12.4 |
1.138+0.089 −0.075 |
6000±110 | [137] |
| TOI-3919 b | 3.88±0.023 | 1.1±0.05 | 7.433 | 0.0795±0.0016 | 1200±15 | transit | 1973+28.7 −28.4 |
1.208+0.067 −0.07 |
6100±110 | [137] |
| TOI-4153 b | 1.15±0.38 | 1.438±0.045 | 4.617 | 0.06311+0.00084 −0.00096 |
1670+30 −40 |
transit | 1366±11.4 | 1.572+0.064 −0.071 |
6860+150 −180 |
[137] |
| TOI-4336 Ab | 0.017+0.013 −0.007 |
0.1891 | 16.337 | 0.0872+0.0013 −0.0014 |
308±9 | transit | 73.15 | 0.331±0.015 | 3298+75 −73 |
Located in a triple hierarchical stellar system.[152] |
| TOI-4364 b | 0.1793+0.0089 −0.0082 |
5.424 | 0.04753+0.00053 −0.00054 |
488±4 | transit | 142.9±0.1 | 0.487+0.017 −0.016 |
3528+33 −20 |
Located in the Hyades.[153] | |
| TOI-4379 b | 1.113±0.071 | 1.489±0.079 | 3.254 | transit | 2013+38 −39 |
1.372+0.037 −0.105 |
6020±100 | [154] | ||
| TOI-4438 b | 0.017±0.0035 | 0.2248±0.0116 | 7.44 | 0.0534±0.009 | 400±50 | transit | 98 | 0.368±0.021 | 3422±81 | [155] |
| TOI-4443 b | 0.153 | 1.85 | 0.030 | 1639 | transit | 1.05 | 5834 | [99] | ||
| TOI-4495 b | 0.324 | 5.18 | 0.062 | 1383 | transit | 1.17 | 6156 | [99] | ||
| TOI-4527 b | 0.0812 | 0.40 | 0.008 | 1363 | transit | 0.48 | 3702 | [99] | ||
| TOI-4562 c | 5.77+0.37 −0.56 |
3990+201 −192 |
5.219±0.002 | timing | 1131±12[156] | 1.218+0.054 −0.048[156] |
6096±32[156] | [157] | ||
| TOI-4602 b | 0.227 | 3.98 | 0.051 | 1380 | transit | 1.12 | 6012 | [99] | ||
| TOI-4633 c | 0.15+0.087 −0.075 |
0.285+0.018 −0.017 |
271.94 | 0.847±0.061 | 290 | transit | 310.4±0.78 | 1.05±0.06 or 1.1±0.06[i] | 5600±50 or 5800±50 [i] | Habitable-zone planet located in a binary star system. The temperature reaches 420 K when the stars are at periastron.[158] |
| TOI-4914 b | 0.714±0.041 | 1.1482±0.0321 | 10.6 | 0.098±0.003 | 894±20 | transit | 951±5 | 1.03±0.06 | 5805±62 | [148] |
| TOI-5005 b | 0.103±0.018 | 0.558±0.021 | 6.309 | 0.06614±0.0045 | 1040±20 | transit | 685±2 | 0.97±0.02 | 5749±61 | [159] |
| TOI-5076 b | 0.0503±0.00629 | 0.285±0.00892 | 23.445±0.001 | 615±20 | transit | 270.057±0.326 | 0.80±0.07 | 5070±143 | [160] | |
| TOI-5082 b | 0.227 | 4.24 | 0.051 | 1165 | transit | 1.00 | 5670 | [99] | ||
| TOI-5218 b | 0.799+0.393 −0.359 |
0.879±0.034 | 4.291 | 0.0469±0.0006 | 783±21 | transit | 1243±11 | 0.739±0.03 | 4230±88 | [60] |
| TOI-5232 b | 2.34±0.16 | 1.14+0.05 −0.045 |
4.097 | 0.0599±0.001 | 1772+40 −45 |
transit | 1985+28 −27 |
1.389+0.068 −0.075 |
6500+180 −190 |
[137] |
| TOI-5301 b | 3.65±0.4 | 1.18+0.08 −0.07 |
5.859 | 0.0726+0.0013 −0.0024 |
1655±40 | transit | 1914+59 −55 |
1.483+0.081 −0.14 |
6240±160 | [137] |
| TOI-5319 b | 0.33427±0.0551 | 4.079 | 695 | transit | 199.4±0.7 | 0.5±0.1 | 3580+107 −141 |
[161][139] | ||
| TOI-5388 b | 0.169 | 2.59 | 0.024 | 601 | transit | 0.29 | 3495 | [99] | ||
| TOI-5616 b | 0.802+0.371 −0.384 |
0.961+0.048 −0.042 |
2.003 | 0.0272±0.0003 | 939±27 | transit | 1249±14 | 0.666±0.025 | 3996±88 | [60] |
| TOI-5634 Ab | 0.576+0.406 −0.346 |
0.923+0.056 −0.050 |
2.2035 | 0.0272±0.0003 | 837±34 | transit | 1051+20 −18 |
0.556±0.022 | 3896±88 | [60] |
| TOI-5688 Ab | 0.390+0.074 −0.077 |
0.920+0.053 −0.062 |
2.948 | 0.03379+0.00046 −0.00045 |
742±18 | transit | 735.8+4.2 −4.9 |
0.60±0.02 | 3713±59 | [162] |
| TOI-5713 b | 0.0135+0.0053 −0.0035 |
0.1579+0.0152 −0.0125 |
10.44 | 0.06008±0.00046 | 347±3 | transit | 133.7[a] | 0.265±0.006 | 3228±41 | [163] |
| TOI-5720 b | 0.0041+0.0029 −0.0015 |
0.0972±0.0062 | 1.434 | 0.0183±0.0003 | 708±19 | transit | 116.9±0.1 | 0.383±0.019 | 3325±75 | [164] |
| TOI-6002 b | 0.0119+0.005 −0.0031 |
0.1454+0.0107 −0.017 |
10.905 | 0.05722±0.00044 | 321+7 −5 |
transit | 104.6[a] | 0.21 | 3241+80 −60 |
[163] |
| TOI-6008 b | 0.00346+0.0023 −0.0011 |
0.0919±0.0045 | 0.858 | 0.0108±0.0002 | 707±19 | transit | 75.05±0.03 | 0.23±0.011 | 3075±75 | Ultra-short period planet[164] |
| TOI-6029 b | 1.635±0.032 | 1.284±0.098 | 5.7987±0.0004 | transit | 1946+37 −36 |
1.548+0.027 −0.085 |
6223±100 | [154] | ||
| TOI-6034 b | 0.798±0.075 | 1.063±0.042 | 2.576 | 0.02949+0.00043 −0.00044 |
714±21 | transit | 385 | 0.514+0.025 −0.022 |
3635±88 | [60] |
| TOI-6086 b | 0.00346+0.00362 −0.00176 |
0.1053±0.0062 | 1.389 | 0.0154±0.0002 | 634±16 | transit | 102.6 | 0.254±0.013 | 3200±75 | [164] |
| TOI-6383 Ab | 1.04±0.094 | 1.008+0.036 −0.033 |
1.791 | 0.02292±0.00037 | 745±23 | transit | 561+3.0 −2.7 |
0.458±0.011 | 3444±88 | [165] |
| TOI-6651 b | 0.1919+0.0239 −0.0249 |
0.4541+0.0241 −0.0232 |
5.057 | 0.06330+0.00078 −0.00072 |
1493+14 −15 |
transit | 690±3[166][a] | 1.323+0.050 −0.045 |
5940±110 | [167] |
| TOI-7041 b | 0.36±0.16 | 1.02±0.03 | 9.691±0.006 | transit | 1431±10 | 1.12±0.02 | 4640±10 | [168] | ||
| V808 Aurigae b | 6.8±0.7 | 4109±362 | timing | 698±13 | 0.9±0.1 | The planet's host star is a polar. The mass value for the planet is only a minimum mass.[169] | ||||
| VHS J183135.58-551355.9 | 6.5±1.5 | 1.42+0.04 −0.03 |
1085±60 | imaging | 180.6±17.9 | Free-floating planet[170] | ||||
| WASP-132d | 5.16±0.52 | 1816.6±44.4 | 2.71±0.12 | 107+11 −18 |
radial vel. | 401.53±1.86 | 0.789±0.039 | 4686±99 | [171] | |
| Wolf 327 b | 0.00796±0.00145 | 0.1106±0.0054 | 0.573 | 0.01 | 996±22 | transit | 92.9 | 0.405±0.019 | 3542±70 | Ultra-short period planet[172] |
Specific exoplanet lists
[edit]- List of directly imaged exoplanets
- List of exoplanet extremes
- List of exoplanet firsts
- List of exoplanets discovered by the Kepler space telescope
- List of exoplanets observed during Kepler's K2 mission
- List of extrasolar candidates for liquid water
- List of hottest exoplanets
- List of coolest exoplanets
- List of multiplanetary systems
- List of nearest exoplanets
- List of nearest terrestrial exoplanet candidates
- List of potentially habitable exoplanets
- List of proper names of exoplanets
- List of largest exoplanets
- List of smallest exoplanets
- List of transiting exoplanets
- List of exoplanets and planetary debris around white dwarfs
Lists of exoplanets by year of discovery
[edit]- List of exoplanets discovered before 2000 (31)
- List of exoplanets discovered between 2000–2009 (377)
- List of exoplanets discovered in 2010 (109)
- List of exoplanets discovered in 2011 (179)
- List of exoplanets discovered in 2012 (149)
- List of exoplanets discovered in 2013 (151)
- List of exoplanets discovered in 2014 (870)
- List of exoplanets discovered in 2015 (149)
- List of exoplanets discovered in 2016 (1497)
- List of exoplanets discovered in 2017 (158)
- List of exoplanets discovered in 2018 (303)
- List of exoplanets discovered in 2019 (172)
- List of exoplanets discovered in 2020 (249)
- List of exoplanets discovered in 2021 (257)
- List of exoplanets discovered in 2022 (313)
- List of exoplanets discovered in 2023 (307)
- List of exoplanets discovered in 2024 (239)
Notes
[edit]- ^ a b c d e f g h Distance calculated from parallax
- ^ The radius is the same as that of the Earth, with an uncertainty of 10%
- ^ Calculated using a/R⋆ (ratio between Semi-major axis and host star radius)
- ^ Radius calculated with mass and lower limit in density in the equation d=(1.89813*10^(30)*m)/((4/3)*π*r3), where d is density (in g/cm3), m is the mass (in MJ and r is the radius (in centimeters). Should be divided by 7.1492×109 to convert from centimeters to RJ
- ^ Since the density is only a lower limit, the radius is an upper limit.
- ^ The planet is located in a two-star system, with masses of 0.78+0.38
−0.36 M☉ and 0.56+0.3
−0.28 M☉. There is a large chance that it is orbiting both stars in the system, so the "host star mass" would be 0.78+0.38
−0.36 M☉ + 0.56+0.3
−0.28 M☉. However, there is a small chance that is orbiting only one of the stars in the system. - ^ The transit observations of TOI-286 indicate periodic transit signals of 4.5 and 39.4 days. While this, radial velocity measurements with ESPRESSO do not immediately show evidence for periodic signals at either periods.
- ^ a b c Assuming albedos of 0.3 and 0 respectively.
- ^ a b It is not known which of the stars the planet orbits.
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- ^ Korth, Judith; Chaturvedi, Priyanka; Parviainen, Hannu; Carleo, Ilaria; Endl, Michael; Guenther, Eike W.; Nowak, Grzegorz; Persson, Carina; MacQueen, Phillip J. (25 July 2024). "TOI-1408: Discovery and Photodynamical Modeling of a Small Inner Companion to a Hot Jupiter Revealed by Transit Timing Variations". The Astrophysical Journal Letters. 971 (2): L28. arXiv:2407.17798. Bibcode:2024ApJ...971L..28K. doi:10.3847/2041-8213/ad65fd.
- ^ "TOI-1437 Overview". NASA Exoplanet Archive.
- ^ Pidhorodetska, Daria; Gilbert, Emily A.; Kane, Stephen R.; Barclay, Thomas; Polanski, Alex S.; Hill, Michelle L.; Stassun, Keivan G.; Giacalone, Steven; Ciardi, David R.; Boyle, Andrew W.; Howell, Steve B.; Lillo-Box, Jorge; MacDougall, Mason G.; Fetherolf, Tara; Batalha, Natalie M. (1 September 2024). "The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437". The Astronomical Journal. 168 (3): 135. arXiv:2405.12448. Bibcode:2024AJ....168..135P. doi:10.3847/1538-3881/ad6901. ISSN 0004-6256.
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- ^ a b Brady, M.; Bean, J.; Seifahrt, A.; Kasper, D.; Luque, R.; Stefánsson, G.; Stürmer, J.; Charbonneau, D.; Collins, K. (16 May 2024), "Early Results from the HUMDRUM Survey: A Small, Earth-mass Planet Orbits TOI-1450A", The Astronomical Journal, 168 (2): 67, arXiv:2405.10400, Bibcode:2024AJ....168...67B, doi:10.3847/1538-3881/ad500a
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- ^ "TOI-1883 Overview". NASA Exoplanet Archive.
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- ^ "TOI-2274 Overview". NASA Exoplanet Archive.
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- ^ a b Hacker, Alejandro; et al. (43) (8 June 2024). "TOI-2374 b and TOI-3071 b: two metal-rich sub-Saturns well within the Neptunian desert". Monthly Notices of the Royal Astronomical Society. 532 (2): 1612–1634. arXiv:2406.12996. doi:10.1093/mnras/stae1420.
- ^ a b Bryant, Edward M.; et al. (34) (29 August 2024). "TOI-2379 b and TOI-2384 b: two super-Jupiter mass planets transiting low-mass host stars". Monthly Notices of the Royal Astronomical Society. 533 (4): 3893–3906. doi:10.1093/mnras/stae2034. Retrieved 28 September 2024.
- ^ a b Carleo, Ilaria; Barrágan, Oscar; Persson, Carina M.; Fridlund, Malcolm; Lam, Kristine W. F.; Messina, Sergio; Gandolfi, Davide; Smith, Alexis M. S.; Johnson, Marshall C. (10 August 2024). "Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b". Astronomy and Astrophysics. 690: A18. arXiv:2408.05612. Bibcode:2024A&A...690A..18C. doi:10.1051/0004-6361/202451313.
- ^ a b c Mantovan, G.; Wilson, T. G.; Borsato, L.; Zingales, T.; Biazzo, K.; Nardiello, D.; Malavolta, L.; Desidera, S.; Marzari, F. (11 September 2024). "The inflated, eccentric warm Jupiter TOI-4914 b orbiting a metal-poor star, and the hot Jupiters TOI-2714 b and TOI-2981 B". Astronomy & Astrophysics. 691: A67. arXiv:2409.07520. doi:10.1051/0004-6361/202451841.
- ^ "TOI-2768 Overview". NASA Exoplanet Archive.
- ^ Nabbie, Emma; et al. (2024). "Surviving in the Hot Neptune Desert: The Discovery of the Ultra-Hot Neptune TOI-3261b". arXiv:2407.04225v1 [astro-ph.EP].
- ^ Martioli, E.; Petrucci, R. P.; Jofre, E.; Hebrard, G.; Ghezzi, L.; Chew, Y. Gomez Maqueo; Diaz, R. F.; Perottoni, H. D.; Garcia, L. H. (5 September 2024). "TOI-3568 b: a super-Neptune in the sub-Jovian desert". Astronomy and Astrophysics. 690: A312. arXiv:2409.03704. Bibcode:2024A&A...690A.312M. doi:10.1051/0004-6361/202450334.
- ^ Timmermans, M.; Dransfield, G.; Gillon, M.; Triaud, A. H. M. J.; Rackham, B. V.; Aganze, C.; Barkaoui, K.; Briceño, C.; Burgasser, A. J. (19 April 2024), "TOI-4336 a b: A temperate sub-Neptune ripe for atmospheric characterization in a nearby triple M-dwarf system", Astronomy & Astrophysics, 687: A48, arXiv:2404.12722, Bibcode:2024A&A...687A..48T, doi:10.1051/0004-6361/202347981
- ^ Distler, Adam; Soares-Furtado, Melinda; Vanderburg, Andrew; Schulte, Jack; Becker, Juliette; Mann, Andrew W.; Howell, Steve B.; Kraus, Adam L.; Barkaoui, Khalid (16 October 2024). "TESS Hunt for Young and Maturing Exoplanets (THYME) XII: A Young Mini-Neptune on the Upper Edge of the Radius Valley in the Hyades Cluster". arXiv:2410.11990 [astro-ph.EP].
- ^ a b Saunders, Nicholas; Grunblatt, Samuel K.; Chontos, Ashley; Dai, Fei; Huber, Daniel; Zhang, Jingwen; Stefansson, Gudmundur; van Saders, Jennifer L.; Winn, Joshua N.; Hey, Daniel; Howard, Andrew W.; Fulton, Benjamin; Isaacson, Howard; Beard, Corey; Giacalone, Steven (1 August 2024). "TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence". The Astronomical Journal. 168 (2): 81. arXiv:2407.21650. Bibcode:2024AJ....168...81S. doi:10.3847/1538-3881/ad543b. ISSN 0004-6256.
- ^ Martin, Pierre-Yves (2024). "Planet TOI-4438 b". exoplanet.eu. Retrieved 6 March 2024.
- ^ a b c Heitzmann, Alexis; Zhou, George; Quinn, Samuel N.; Huang, Chelsea X.; Dong, Jiayin; Bouma, Luke G.; Dawson, Rebekah I.; Marsden, Stephen C.; Wright, Duncan; Petit, Pascal; Collins, Karen A.; Barkaoui, Khalid; Wittenmyer, Robert A.; Gillen, Edward; Brahm, Rafael (1 March 2023). "TOI-4562 b: A highly eccentric temperate Jupiter analog orbiting a young field star". The Astronomical Journal. 165 (3): 121. arXiv:2208.10854. Bibcode:2023AJ....165..121H. doi:10.3847/1538-3881/acb5a2. ISSN 0004-6256.
- ^ Fermiano, V.; Saito, R. K.; Ivanov, V. D.; Caceres, C.; Almeida, L. A.; Aires, J.; Beamin, J. C.; Minniti, D.; Ferreira, T. (10 September 2024). "The young exoplanetary system TOI-4562: Confirming the presence of a third body in the system". Astronomy and Astrophysics. 690: L7. arXiv:2409.06924. Bibcode:2024A&A...690L...7F. doi:10.1051/0004-6361/202451935.
- ^ Eisner, Nora L.; Grunblatt, Samuel K.; Barragán, Oscar; Faridani, Thea H.; Lintott, Chris; Aigrain, Suzanne; Johnston, Cole; Mason, Ian R.; Stassun, Keivan G.; Bedell, Megan; Boyle, Andrew W.; Ciardi, David R.; Clark, Catherine A.; Hebrard, Guillaume; Hogg, David W. (1 May 2024). "Planet Hunters TESS V: a planetary system around a binary star, including a mini-Neptune in the habitable zone". The Astronomical Journal. 167 (5): 241. arXiv:2404.18997. Bibcode:2024AJ....167..241E. doi:10.3847/1538-3881/ad1d5c. ISSN 0004-6256.
- ^ Castro-González, A.; Lillo-Box, J.; Armstrong, D. J.; Acuña, L.; Aguichine, A.; Bourrier, V.; Gandhi, S.; Sousa, S. G.; Delgado-Mena, E. (26 September 2024), "TOI-5005 b: A super-Neptune in the savanna near the ridge", Astronomy & Astrophysics, 691: A233, arXiv:2409.18129, doi:10.1051/0004-6361/202451656
- ^ Montalto, M.; et al. (39) (29 May 2024). "The GAPS programme at TNG. LVII. TOI-5076b: A warm sub-Neptune planet orbiting a thin-to-thick-disk transition star in a wide binary system". Astronomy and Astrophysics. 687. arXiv:2405.18950. Bibcode:2024A&A...687A.226M. doi:10.1051/0004-6361/202349082.
- ^ "TOI-5319 Overview". NASA Exoplanet Archive.
- ^ Reji, Varghese; Kanodia, Shubham; Ninan, Joe; Cañas, Caleb I.; Libby-Roberts, Jessica; Lin, Andrea S. J.; Gupta, Arvind F.; Sewaby, Tera N.; Larsen, Alexander (4 September 2024). "Searching for GEMS: TOI-5688 A b, a low-density giant orbiting a high-metallicity early M-dwarf". arXiv:2409.01371 [astro-ph.EP].
- ^ a b Ghachoui, M.; Rackham, B. V.; Dévora-Pajares, M.; Chouqar, J.; Timmermans, M.; Kaltenegger, L.; Sebastian, D.; Pozuelos, F. J.; Eastman, J. D. (1 August 2024). "TESS discovery of two super-Earths orbiting the M-dwarf stars TOI-6002 and TOI-5713 near the radius valley". Astronomy & Astrophysics. 690: A263. arXiv:2408.00709. Bibcode:2024A&A...690A.263G. doi:10.1051/0004-6361/202451120.
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- ^ Bernabò, Lia Marta; Kanodia, Shubham; Canas, Caleb I.; Cochran, William D.; Csizmadia, Szilárd; Mahadevan, Suvrath; Stefánsson, Gudhmundur; Gupta, Arvind F.; Monson, Andrew (25 September 2024). "Searching for GEMS: TOI-6383Ab, a giant planet transiting an M3-dwarf star in a binary system". arXiv:2409.16889 [astro-ph.EP].
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- ^ Saunders, Nicholas; Grunblatt, Samuel K.; Huber, Daniel; Ong, J. M. Joel; Schlaufman, Kevin C.; Hey, Daniel; Li, Yaguang; Butler, R. P.; Crane, Jeffrey D. (14 October 2024). "TESS Giants Transiting Giants. VII. A Hot Saturn Orbiting an Oscillating Red Giant Star". arXiv:2410.11037 [astro-ph.EP].
- ^ Leichty, McKenna; Garnavich, Peter; Littlefield, Colin; Schwope, Axel D.; Kurpas, Jan; Mason, Paul A.; Beuermann, Klaus (26 February 2024). "An Eccentric Planet Orbiting the Polar V808 Aurigae". The Astrophysical Journal. 967 (2): 81. arXiv:2402.16959. Bibcode:2024ApJ...967...81L. doi:10.3847/1538-4357/ad3bac.
- ^ Bickle, Thomas P.; Schneider, Adam C.; Gagné, Jonathan; Faherty, Jacqueline K.; Rothermich, Austin; Vos, Johanna M.; Suárez, Genaro; Kirkpatrick, J. Davy; Meisner, Aaron M. (6 May 2024), "Discovery of the Remarkably Red L/T Transition Object VHS J183135.58-551355.9", The Astronomical Journal, 168 (2): 66, arXiv:2405.03849, Bibcode:2024AJ....168...66B, doi:10.3847/1538-3881/ad4b16
- ^ Grieves, N.; Bouchy, F.; Armstrong, D. J.; Akinsanmi, B.; Psaridi, A.; Ulmer-Moll, S.; Frensch, Y. G. C.; Helled, R.; Muller, S. (22 June 2024), Refining the WASP-132 multi-planetary system: discovery of a cold giant planet and mass measurement of a hot super-Earth, arXiv:2406.15986v1
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2024 in space | |||
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Space probe launches  |
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