List of exoplanets discovered in 2024

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 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

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2MASS J05581644-4501559 b  | 6–12  |  |  | 1043  |  | imaging  | 94.5  | 0.259±0.02[1] | 3218±158[1] | [2]
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[3]
BD-14 3065 b  | 12.11+0.95
−0.91 | 1.926±0.094  | 4.3  | 0.0646±0.0026  | 1957±28  | transit  | 1847.4[4][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[5]
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.[6][7]
Gaia20eae b | 6  |  |  | 0.062  |  | disc thermal instability  | 9226+3130
−2021[8] | 1.15  | 4330±300[8] | First object detected by this method[9]
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 |  | [10]
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  | [11]
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[12]
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[13]
Gliese 900 b | 10.5  |  | 500,000,000[14] | 12,000  |  | imaging  | 68[14] | 1.08 (combined)  | 3976[15] | Located in a three-star system.[16] It has the longest orbital time of any exoplanet so far at 1.4 million years.[17]
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  | [18]
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[19]
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  | [20]
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  | [21]
HD 48948 c | 0.0229±0.00220  |  | 37.920+0.026
−0.024 | 0.1951±0.0016  | 413±6  | radial vel.  | [21]
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.[21]
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[22]
HD 73344 b  | 0.00939+0.00787
−0.00599 | 0.2573+0.0073
−0.0064 | 15.6  | 0.131  | 911±7  | transit  | 114.7  | 1.2±0.02  | 6220±64  | The dayside temperature can be as high as 1,066 K if the planet is tidally locked. Another planet in the system (HD 73344 c) is suspected. The later has a minimum mass of 116.3 ME and an orbital period of 66 days.[23]
HD 75898 c | 8.49±0.65  |  | 6717±40  | 7.39±0.05  |  | astrometry and radial vel.  | 263  | 1.28±0.13  | 6021±50  | [24]
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[25]
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  | [26]
HD 118203 c | 11.1+1.3
−1 |  | 5070  | 6.2±0.2  | 146±3  | radial vel.  | 300±0.5  | 1.353±0.006  | 5872±20  | [27]
HD 128717 b  | 12.8  |  | 1089.2  | 2.18  |  | astrometry  | 240±0.5  | 1.17+0.6
−0.16 | 6158±115  | [28]
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 | [29]
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 | [29]
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.[30] 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[31]
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.[32]
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  | [33]
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  | [34]
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[35] | May be a brown dwarf. Estimates of the mass vary from 13.8 MJ to 30+31
−12 MJ.[36]
HIP 67522 c |  | 0.731+0.055
−0.057 | 14.335  | 0.1235  | 915+22
−19 | transit  | 414[37] | 1.2±0.05[37] | 5675±75[37] | [38]
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  | [39]
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  | [40]
KMT-2016-BLG-2321Lb  | 3.58±1.22  |  |  | 3.58±0.81  |  | microlensing  | 11,670±3980  | 0.73±0.28  |  | [41]
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 |  | [42]
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 |  | [42]
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 |  | [42]
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 |  | [43]
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 |  | [44]
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 |  | [44]
KMT-2022-BLG-0732Lb  | 1.12±0.65  |  |  | 4.11+0.74
−1.14 |  | microlensing  | 21,712+3879
−6000 | 0.54±0.31  |  | [43]
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 |  | [43]
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 |  | [43]
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.[45]
KMT-2023-BLG-0469Lb  | 0.124+0.092
−0.067 |  |  | 2.37±0.9  |  | microlensing  | 23,050+3260
−3910 | 0.47±0.36  |  | [46]
KMT-2023-BLG-0735Lb  | 0.12±0.07  |  |  | 2.75±1  |  | microlensing  | 20,830+3910
−3260 | 0.61±0.34  |  | [46]
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 |  | [47]
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[45]
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 |  | [45]
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.[48]
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.[49]
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  | [50]
M62H b | 2.83  | <0.683 [d][e] | 0.133  | 0.004908  |  | timing  | 21,500[51] | 1.4  |  | Pulsar planet located in the globular cluster Messier 62.[52] Second shortest orbit of any confirmed exoplanet after PSR J1719-1438 b.[53]
MOA-2016-BLG-526Lb  | 6.93±0.75  |  |  | 2.07±0.35  |  | microlensing  | 22,490  | 0.4  |  | [41]
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 |  | [46]
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)[54]
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  | [54]
NGTS-29 b  | 0.393  | 0.857  | 69.33  | 0.347  | 414  | transit  | 487±1  | 1.034±0.032  | 5730±80  | [55]
NGTS-30 b | 0.96  | 0.93  | 98.3  | 0.408  | 390  | transit  | 762.5  | 0.94  | 5455  | Also known as TOI-4862 b[56]
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 |  | [57]
OGLE-2016-BLG-1598Lb | 5.91±1.74  |  |  | 2.5±0.88  |  | microlensing  | 19,270±5670  | 0.55±0.32  |  | [41]
OGLE-2016-BLG-1800Lb  | 2.59±1.46  |  |  | 1.88±0.51  |  | microlensing  | 21,100±3360  | 0.41±0.22  |  | [41]
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 |  | [58]
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 |  | [42] Assuming the largest distance, it would be the most distant confirmed exoplanet, surpassing SWEEPS-04/11.[53]
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 |  | [58]
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.[58]
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.[59]
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.[60]
SPECULOOS-3 b |  | 0.08716  | 0.719  | 0.00733  | 553  | transit  | 57.9  | 0.1  | 2800  | Ultra-short period planet[61]
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.[62]
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[63][a] | 1.01±0.03  | 5757+72
−65 | [64]
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  | [65]
TIC 139270665 b  | 0.463  | 0.645  | 23.624  | 0.163  | 700  | transit  | 618  | 1.035+0.052
−0.062 | 5844+84
−82 | [66][67]
TIC 139270665 c  | 4.89+0.66
−0.37 |  | 1010+780
−220 | 2+0.93
−0.31 | 200+18
−35 | radial vel.  | [67]
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.[68]
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)[69]
Also known as TOI-6883 b[70]
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.[71]
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  | [72]
TOI-201 b  | 0.42+0.05
−0.03 | 1.008+0.012
−0.015 | 52.978  | 0.3+0.02
−0.03 | 759+37
−26 | transit  | 373  | 1.316±0.027  | 6394±75  | [73]
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  | [74]
TOI-261 b  |  | 0.271  | 3.36  | 0.035  | 1722  | transit  |  | 0.50  | 5890  | [72]
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][3]
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  | [3]
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☉)[75]
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  | [76]
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  | [76]
TOI-480 b  | 0.0654  |  | 6.866  |  |  | transit  | 177.8  | 1.2  | 6,212  | [77]
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  | [78]
TOI-654 b  |  | 0.211  | 1.53  | 0.021  | 749  | transit  |  | 0.53  | 3433  | [72]
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  | [79]
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  | [80]
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.[65]
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 | [81]
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[82]
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  | [72]
TOI-907 b  |  | 0.858  | 4.58  | 0.055  | 1847  | transit  |  | 1.07  | 6272  | [72]
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  | [83]
TOI-1173 Ab | 0.08213±0.00598  | 0.723±0.015  | 7.064  | 0.0702±0.0012  | 863.9±9.8  | transit  | 430.85[84][a] | 0.911+0.028
−0.03 | 5350±340  | Low-density planet located in a wide binary system.[85]
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  | [32]
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  | [86]
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.[87]
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  | [32]
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  | [86]
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  | [32]
TOI-1294 b  | 0.1957±0.016  | 0.8199±0.0277  | 3.915  | 0.0489  |  | transit  | 1052±7  | 1.02±0.13  | 5714±126  | [88]
TOI-1294 c  | 0.467±0.053  |  | 160.1±2.5  | 0.581  |  | radial vel.  | 1052±7  | 1.02±0.13  | 5714±126  | [89]
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[90]
TOI-1347 c | 0.0088±0.0072  | 0.143±0.009  | 4.842  |  | 1000±25  | transit  | [90]
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 | [91]
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 | [91]
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  | [92]
TOI-1410 b  |  | 0.262  | 1.22  | 0.020  | 1396  | transit  |  | 0.72  | 4635  | [72]
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  | [93]
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 | [81]
TOI-1450 Ab  | 0.00396±0.0004  | 0.1±0.004  | 2.04  |  | 722±35  | transit  | 73.2±0.1  | 0.48±0.24  | 3437±86  | Located in a binary star system. It is the second-lowest mass transiting planet with a high-precision mass measurement.[94]
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.[94]
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  | [32]
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 | [32]
TOI-1683 b  |  | 0.236  | 3.06  | 0.037  | 929  | transit  |  | 0.69  | 4402  | [72]
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).[95]
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  | [32]
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  | [32]
TOI-1798 b  |  | 0.126  | 0.44  | 0.011  | 2122  | transit  | 369.147+1.008
−1.005 | 0.86  | 5165  | [72]
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  | 369.147+1.008
−1.005 | 0.86  | 5165  | [32]
TOI-1806 b  |  | 0.304  | 15.15  | 0.088  | 337  | transit  |  | 0.39  | 3272  | [72]
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  | [32]
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.[96]
TOI-1828 b  | 0.1841±0.012  | 0.769±0.017  | 9.09  | 0.0859  |  | transit  | 1208±8  | 1.04±0.13  | 5809±127  | [97]
TOI-1855 b  | 1.133±0.096  | 1.65+0.37
−0.62 | 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 | [98]
TOI-1885 b  | 1.624±0.103  | 1.219±0.037  | 6.544060±0.000006  |  |  | transit  | 1826.773+21.464
−20.982 |  | 6527±98  | [93]
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 | [99]
TOI-2019 b  | 0.109±0.0132  | 0.505±0.0250  | 15.3444±0.0055  |  |  | transit  | 645.812+2.684
−2.665 |  | 5590  | [93]
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 | [98]
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  | [81]
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 | [100]
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  | [101]
TOI-2368 b  | 0.65±0.18  | 0.967+0.06
−0.03 | 5.175  | 0.05649±0.001  | 1000+44
−30 | transit  | 685±3.9  | 0.897+0.048
−0.049 | 5360+230
−170 | [98]
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  | [102]
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  | [103]
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  | [102]
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  |  | [104]
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  |  | [104]
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  | [102]
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 | [64]
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  | [105]
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  | [105]
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  | [103]
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[106]
TOI-3321 b  | 0.554±0.076  | 1.39+0.07
−0.06 | 3.652  | 0.047±0.001  | 1616±30  | transit  | 928+10.8
−10.4 | 1.041+0.084
−0.068 | 5850±140  | [98]
TOI-3353 b  |  | 0.238  | 4.67  | 0.060  | 1264  | transit  |  | 1.33  | 6365  | [72]
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  | [107]
TOI-3894 b  | 0.85±0.15  | 1.36±0.05  | 4.335  | 0.0543±0.0014  | 1519±22  | transit  | 1343+12.7
−12.4 | 1.138+0.089
−0.075 | 6000±110  | [98]
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  | [98]
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 | [98]
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.[108]
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  | [109]
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  | [110]
TOI-4443 b  |  | 0.153  | 1.85  | 0.030  | 1639  | transit  |  | 1.05  | 5834  | [72]
TOI-4495 b  |  | 0.324  | 5.18  | 0.062  | 1383  | transit  |  | 1.17  | 6156  | [72]
TOI-4562 c | 5.77+0.37
−0.56 |  | 3990+201
−192 | 5.219±0.002  |  | timing  | 1131±12[111] | 1.218+0.054
−0.048[111] | 6096±32[111] | [112]
TOI-4527 b  |  | 0.0812  | 0.40  | 0.008  | 1363  | transit  |  | 0.48  | 3702  | [72]
TOI-4602 b  |  | 0.227  | 3.98  | 0.051  | 1380  | transit  |  | 1.12  | 6012  | [72]
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.[113]
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  | [105]
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  | [114]
TOI-5082 b  |  | 0.227  | 4.24  | 0.051  | 1165  | transit  |  | 1.00  | 5670  | [72]
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  | [40]
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 | [98]
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  | [98]
TOI-5388 b  |  | 0.169  | 2.59  | 0.024  | 601  | transit  |  | 0.29  | 3495  | [72]
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  | [40]
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  | [40]
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  | [115]
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  | [116]
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  | [117]
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 | [116]
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[117]
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  | [109]
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  | [40]
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  | [117]
V808 Aurigae b [ru] | 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.[118]
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[119]
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[120]

## Specific exoplanet lists

[edit]

Lists of exoplanets

* 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 (150)
* List of exoplanets discovered in 2016 (1497)
* List of exoplanets discovered in 2017 (158)
* List of exoplanets discovered in 2018 (304)
* 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 (312)
* List of exoplanets discovered in 2023 (304)
* List of exoplanets discovered in 2024 (189)

## Notes

[edit]

1. ^ a b c d e f g Distance calculated from parallax
2. ^ The radius is the same as that of the Earth, with an uncertainty of 10%
3. ^ Calculated using a/R⋆ (ratio between Semi-major axis and host star radius)
4. ^ 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
5. ^ Since the density is only a lower limit, the radius is an upper limit.
6. ^ 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.
7. ^ 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.
8. ^ a b c Assuming albedos of 0.3 and 0 respectively.
9. ^ a b It is not known which of the stars the planet orbits.

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69. ^ Sgro, Lauren A.; Dalba, Paul A.; Esposito, Thomas M.; Marchis, Franck; Dragomir, Diana; Villanueva Jr., Steven; Fulton, Benjamin; Billiani, Mario; Loose, Margaret (23 May 2024), "Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists", The Astronomical Journal, 168 (1): 26, arXiv:2405.15021, Bibcode:2024AJ....168...26S, doi:10.3847/1538-3881/ad5096
70. ^ Conzo, G.; Moriconi, M. (26 February 2024). "TOI-6883.01: A Single-transit Planet Candidate Detected from TESS". Research Notes of the AAS. 8 (2): 53. Bibcode:2024RNAAS...8...53C. doi:10.3847/2515-5172/ad2c85. ISSN 2515-5172.
71. ^ Vach, Sydney; Zhou, George; Huang, Chelsea X.; Mann, Andrew W.; Barber, Madyson G.; Bieryla, Allyson; Latham, David W.; Collins, Karen A.; Rogers, James G. (28 July 2024). "A transiting multi-planet system in the 61 million year old association Theia 116". arXiv:2407.19680 [astro-ph.EP].
72. ^ a b c d e f g h i j k l m n o p Hord, Benjamin J.; et al. (147) (23 April 2024). "Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST". The Astronomical Journal. 167 (5): 233. arXiv:2308.09617. Bibcode:2024AJ....167..233H. doi:10.3847/1538-3881/ad3068.
73. ^ Hobson, Melissa J.; et al. (2021). "A Transiting Warm Giant Planet around the Young Active Star TOI-201". The Astronomical Journal. 161 (5): 235. arXiv:2103.02685. Bibcode:2021AJ....161..235H. doi:10.3847/1538-3881/abeaa1.
74. ^ Mascareño, A. Suárez; Passegger, V. M.; Hernández, J. I. González; Armstrong, D. J.; Nielsen, L. D.; Lovis, C.; Lavie, B.; Sousa, S. G.; Silva, A. M. (6 February 2024). "TESS and ESPRESSO discover a super-Earth and a mini-Neptune orbiting the K-dwarf TOI-238". Astronomy and Astrophysics. 685: A56. arXiv:2402.04113. Bibcode:2024A&A...685A..56S. doi:10.1051/0004-6361/202348958.
75. ^ "The Extrasolar Planet Encyclopaedia — TOI-329 b". Extrasolar Planets Encyclopaedia. Paris Observatory.
76. ^ a b Lacedelli, G.; et al. (2024). "Characterisation of TOI-406 as showcase of the THIRSTEE program: A 2-planet system straddling the M-dwarf density gap". arXiv:2409.11083 [astro-ph.EP].
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79. ^ Cointepas, M.; et al. (56) (30 April 2024). "TOI-663: A newly discovered multi-planet system with three transiting mini-Neptunes orbiting an early M star". Astronomy and Astrophysics. 685: A19. Bibcode:2024A&A...685A..19C. doi:10.1051/0004-6361/202346899. hdl:20.500.11850/673980. Retrieved 29 June 2024.
80. ^ Alqasim, A.; Grieves, N.; Rosário, N. M.; Gandolfi, D.; Livingston, J. H.; Sousa, S.; Collins, K. A.; Teske, J. K.; Fridlund, M. (29 July 2024). "TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit". Monthly Notices of the Royal Astronomical Society. 533 (1): 1–26. arXiv:2407.20525. Bibcode:2024MNRAS.533....1A. doi:10.1093/mnras/stae1767.
81. ^ a b c Hori, Y.; Fukui, A.; Hirano, T.; Narita, N.; de Leon, J. P.; Ishikawa, H. T.; Hartman, J. D.; Morello, G.; García, N. Abreu (21 May 2024), "The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M dwarfs", The Astronomical Journal, 167 (6): 289, arXiv:2405.12637, Bibcode:2024AJ....167..289H, doi:10.3847/1538-3881/ad4115
82. ^ Psaridi, Angelica; Osborn, Hugh; Bouchy, François; Lendl, Monika; Parc, Léna; Billot, Nicolas; Broeg, Christopher; Sousa, Sérgio G.; Adibekyan, Vardan (30 January 2024). "Discovery of two warm mini-Neptunes with contrasting densities orbiting the young K3V star TOI-815". Astronomy and Astrophysics. 685: A5. arXiv:2401.15709. Bibcode:2024A&A...685A...5P. doi:10.1051/0004-6361/202348678.
83. ^ Mallorquín, M.; Lodieu, N.; Béjar, V. J. S.; Osorio, M. R. Zapatero; Sanz-Forcada, J.; Alarcon, M. R.; Tabernero, H. M.; Nagel, E.; Collins, K. A. (27 February 2024). "TOI-1135 b: A young hot Saturn-size planet orbiting a solar-type star". Astronomy and Astrophysics. 685: A90. arXiv:2402.17448. Bibcode:2024A&A...685A..90M. doi:10.1051/0004-6361/202349016.
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85. ^ Jhon Yana Galarza; Ferreira, Thiago; Lorenzo-Oliveira, Diego; Simon, Joshua D.; Reggiani, Henrique; Piro, Anthony L.; McWilliam, Andrew; Netto, Yuri; Valio, Adriana; Ciardi, David R. (2024). "TOI-1173 A $b$: The First Inflated Super-Neptune in a Wide Binary System". arXiv:2403.06240v1 [astro-ph.EP].
86. ^ a b Bell, J. Serrano; Díaz, R. F.; Hébrard, G.; Martioli, E.; Heidari, N.; Sousa, S.; Boisse, I.; Almenara, J. M.; Alonso-Santiago, J. (12 February 2024). "TOI-1199 b and TOI-1273 b: Two new transiting hot Saturns detected and characterized with SOPHIE and TESS". Astronomy & Astrophysics. 684: A6. arXiv:2402.07861. Bibcode:2024A&A...684A...6S. doi:10.1051/0004-6361/202348288.
87. ^ Thao, Pa Chia; Mann, Andrew W.; Barber, Madyson G.; Kraus, Adam L.; Tofflemire, Benjamin M.; Bush, Jonathan L.; Wood, Mackenna L.; Collins, Karen A.; Vanderburg, Andrew (7 June 2024). "TESS Hunt for Young and Maturing Exoplanets (THYME) X: a two-planet system in the 210 Myr MELANGE-5 Association". The Astronomical Journal. 168 (1): 41. arXiv:2406.05234. Bibcode:2024AJ....168...41T. doi:10.3847/1538-3881/ad4993.
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90. ^ a b Rubenzahl, Ryan A.; Dai, Fei; Howard, Andrew W.; Lissauer, Jack J.; Van Zandt, Judah; Beard, Corey; Giacalone, Steven; Murphy, Joseph M. Akana; Chontos, Ashley (12 February 2024). "The TESS-Keck Survey. XII. A Dense 1.8 R🜨 Ultra-Short-Period Planet Possibly Clinging to a High-Mean-Molecular-Weight Atmosphere After the First Gyr". arXiv:2402.07451 [astro-ph.EP].
91. ^ a b Hill, Michelle L.; Kane, Stephen R.; Dalba, Paul A.; MacDougall, Mason; Fetherolf, Tara; Li, Zhexing; Pidhorodetska, Daria; Batalha, Natalie M.; Crossfield, Ian J. M. (5 February 2024), "The TESS–Keck Survey. XIX. A Warm Transiting Sub-Saturn-mass Planet and a Nontransiting Saturn-mass Planet Orbiting a Solar Analog", The Astronomical Journal, 167 (4): 151, arXiv:2402.03498, Bibcode:2024AJ....167..151H, doi:10.3847/1538-3881/ad2765
92. ^ 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.
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94. ^ 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
95. ^ Desai, Anmol; Turtelboom, Emma V.; Harada, Caleb K.; Dressing, Courtney D.; Rice, David R.; Murphy, Joseph M. Akana; Brinkman, Casey L.; Chontos, Ashley; Crossfield, Ian J. M. (11 February 2024). "The TESS-Keck Survey. XVIII. A sub-Neptune and spurious long-period signal in the TOI-1751 system". The Astronomical Journal. 167 (5): 194. arXiv:2402.07110. Bibcode:2024AJ....167..194D. doi:10.3847/1538-3881/ad29ee.
96. ^ Lange, Sarah; Murphy, Joseph M. Akana; Batalha, Natalie M.; Crossfield, Ian J. M.; Dressing, Courtney D.; Fulton, Benjamin; Howard, Andrew W.; Huber, Daniel; Isaacson, Howard; Kane, Stephen R.; Petigura, Erik A.; Robertson, Paul; Weiss, Lauren M.; Behmard, Aida; Beard, Corey (23 May 2024). "The TESS-Keck Survey. VII. A Superdense Sub-Neptune Orbiting TOI-1824*". The Astronomical Journal. 167 (6): 282. Bibcode:2024AJ....167..282L. doi:10.3847/1538-3881/ad34d9. ISSN 1538-3881.
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98. ^ a b c d e f g h i Schulte, Jack; Rodriguez, Joseph E.; Bieryla, Allyson; Quinn, Samuel N.; Collins, Karen A.; Yee, Samuel W.; Nine, Andrew C.; Soares-Furtado, Melinda; Latham, David W. (11 January 2024), "Migration and Evolution of giant ExoPlanets (MEEP) I: Nine Newly Confirmed Hot Jupiters from the TESS Mission", The Astronomical Journal, 168 (1): 32, arXiv:2401.05923, Bibcode:2024AJ....168...32S, doi:10.3847/1538-3881/ad4a57
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101. ^ Parviainen, Hannu; Murgas, Felipe; Esparza-Borges, Emma; Peláez-Torres, A.; Palle, Enric; Luque, Rafael; Zapatero-Osorio, M. R.; Korth, Judith; Fukui, Akihiko (22 January 2024). "TOI-2266 b: a keystone super-Earth at the edge of the M dwarf radius valley". Astronomy and Astrophysics. 683: A170. arXiv:2401.11879. Bibcode:2024A&A...683A.170P. doi:10.1051/0004-6361/202347431.
102. ^ a b c Eberhardt, Jan; Hobson, Melissa J.; Henning, Thomas; Trifonov, Trifon; Brahm, Rafael; Espinoza, Nestor; Jordán, Andrés; Thorngren, Daniel; Burn, Remo; Rojas, Felipe I.; Sarkis, Paula; Schlecker, Martin; Pinto, Marcelo Tala; Barkaoui, Khalid; Schwarz, Richard P. (27 February 2024). "Three Warm Jupiters around Solar-analog stars detected with TESS". The Astronomical Journal. 166 (6): 271. arXiv:2402.17592. doi:10.3847/1538-3881/ad06bc. ISSN 0004-6256.
103. ^ 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.
104. ^ 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". arXiv:2408.05612 [astro-ph.EP].
105. ^ 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". arXiv:2409.07520 [astro-ph.EP].
106. ^ 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].
107. ^ 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". arXiv:2409.03704 [astro-ph.EP].
108. ^ 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
109. ^ 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.
110. ^ Martin, Pierre-Yves (2024). "Planet TOI-4438 b". exoplanet.eu. Retrieved 6 March 2024.
111. ^ 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.
112. ^ 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". arXiv:2409.06924 [astro-ph.EP].
113. ^ 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.
114. ^ 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.
115. ^ 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].
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