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 |
---|---|---|---|---|---|---|---|---|---|---|
2MASS J05581644-4501559 b | 6–12 | 1043 | imaging | 94.5 | 0.259±0.02 [1] | 3218±158 [1] | [2] | |||
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 [3] [lower-alpha 1] | 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. [4] Also known as TOI-4987 b |
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 | [5] Highly eccentric orbit (e = 0.58). Cited as confirmed by NASA Exoplanet Archive and exoplanet.eu. [6] [5] | ||
Gliese 341 b | 0.00227±0.00044 | 0.0821±0.045 | 7.577 | 540 | transit | 33.9 | 0.506 | 3745 | [7] Also known as TOI-741 b | |
HD 63433 d | 0.09573±0.0141 | 4.21 | 0.0503±0.0027 | 1040±40 | transit | 71.7 | 0.99±0.03 | 5688±28 | [8] Hot Earth-sized exoplanet | |
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 | [9] Also known as TOI-1778 b |
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 | [10] | ||
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 | [11] | ||
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 | [11] | ||
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 [12] | [13] May be a brown dwarf. Estimated of the mass vary from 13.8 MJ to 30+31 −12 MJ. | |
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 | [14] | ||
KMT-2016-BLG-2321Lb | 3.58±1.22 | 3.58±0.81 | microlensing | 11,670±3980 | 0.73±0.28 | [15] | ||||
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 | [16] The mass of the planet can be as low as 0.042+0.021 −0.022 MJ | ||||
KMT-2023-BLG-0469Lb | 0.124+0.092 −0.067 | 2.37±0.9 | microlensing | 23,050+3260 −3910 | 0.47±0.36 | [17] | ||||
KMT-2023-BLG-0735Lb | 0.12±0.07 | 2.75±1 | microlensing | 20,830+3910 −3260 | 0.61±0.34 | [17] | ||||
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 | [16] Estimates of the planet's mass varies between 0.3+0.34 −0.16 MJ and 0.77+0.87 −0.42 MJ | ||||
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 | [16] | ||||
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 | [18] | |
M62H b | 2.83 | 0.133 | 0.004908 | timing | 21,500 [19] | 1.4 | Pulsar planet located in the globular cluster Messier 62. [20] | |||
MOA-2016-BLG-526Lb | 6.93±0.75 | 2.07±0.35 | microlensing | 22,490 | 0.4 | [15] | ||||
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 | [17] | ||||
OGLE-2016-BLG-1598Lb | 5.91±1.74 | 2.5±0.88 | microlensing | 19,270±5670 | 0.55±0.32 | [15] | ||||
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) [21] |
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 | [21] |
NGTS-30 b | 0.96 | 0.93 | 98.3 | 0.408 | 390 | transit | 762.5 | 0.94 | 5455 | [22] Also known as TOI-4862 b |
OGLE-2016-BLG-1800Lb | 2.59±1.46 | 1.88±0.51 | microlensing | 21,100±3360 | 0.41±0.22 | [15] | ||||
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 | [23] | ||||
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 | [23] | ||||
OGLE-2017-BLG-1275Lb | 5.9±2.2 | 1.19±0.36 | microlensing | 25,070±2930 | 0.63±0.23 | [23] Another solution suggests a larger semi-major axis, of 2.09±0.63 AU | ||||
OGLE-2023-BLG-0836Lb | 4.36+2.35 −2.2 | 3.7+1 −1.2 | microlensing | 16,690+4430 −5250 | [lower-alpha 2] | [24] The planet is located in a binary star system, and is likely to be orbiting both stars in the system. | ||||
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 | [25] Located in the open cluster Messier 67 | |
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. [26] | |
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 | 1.01±0.03 | 5757+72 −65 | [27] | |
TIC 139270665 b | 0.463 | 0.645 | 23.624 | 0.163 | 700 | transit | 618 | 1.035+0.052 −0.062 | 5844+84 −82 | [28] [29] |
TIC 139270665 c | 4.89+0.66 −0.37 | 1010+780 −220 | 2+0.93 −0.31 | 200+18 −35 | radial vel. | 618 | 1.035+0.052 −0.062 | 5844+84 −82 | [29] | |
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 | [30] |
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 | [31] The host star is part of a binary star system with a red dwarf companion |
TOI-815 c | 0.0739±0.00755 | 0.2337+0.0089 −0.008 | 34.976 | 0.193±0.004 | 469±9 | transit | 193.76±0.15 | 0.776±0.036 | 4869±77 | [31] The host star is part of a binary star system with a red dwarf companion |
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 | [32] |
TOI-1173 Ab | 0.08213±0.00598 | 0.723±0.015 | 7.064 | 0.0702±0.0012 | 863.9±9.8 | transit | 0.911+0.028 −0.03 | 5350±340 | [33] Low-density planet located in a wide binary system | |
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 | [34] |
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 | [34] |
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 | [35] Ultra-short period planet | |
TOI-1347 c | 0.0088±0.0072 | 0.143±0.009 | 4.842 | 1000±25 | transit | 480.8±2 | 0.913±0.033 | 5464±100 | [35] | |
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 | [36] |
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 | [36] | |
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 | [37] The host star is metal-poor ([Fe/H] = –0.40 dex) |
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 | [38] |
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 | [38] |
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 | [39] | |
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 | [38] |
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 | [40] |
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 | [40] |
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 | [40] |
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 | [27] |
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 | [38] |
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 | [38] |
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 | [38] |
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 | [38] |
TOI-4436 b | 0.1891 | 16.337 | 0.0872+0.0013 −0.0014 | 308±9 | transit | 73.15 | 0.331±0.015 | 3298+75 −73 | [41] Located in a triple hierarchical stellar system | |
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 | [42] |
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 [lower-alpha 3] | 5600±50 or 5800±50 [lower-alpha 3] | Habitable-zone planet located in a binary star system. The temperature reaches 420 K when the stars are at periastron. [43] |
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 | [38] |
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 | [38] |
V808 Aurigae b | 6.8±0.7 | 4109±362 | timing | 698±13 | 0.9±0.1 | [44] The planet's host star is a polar. The mass value for the planet is only a minimum mass. | ||||
VHS J183135.58-551355.9 | 7±1 | 1.42+0.04 −0.03 | 1085±60 | imaging | 180.6±17.9 | Free-floating planet [45] | ||||
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 | [46] Ultra-short period planet |
OGLE-2005-BLG-071L is a distant, magnitude 19.5 galactic bulge star located in the constellation Scorpius, approximately 11,000 light years away from the Solar System. The star is probably a red dwarf with a mass 43% of that of the Sun.
Planet Hunters is a citizen science project to find exoplanets using human eyes. It does this by having users analyze data from the NASA Kepler space telescope and the NASA Transiting Exoplanet Survey Satellite. It was launched by a team led by Debra Fischer at Yale University, as part of the Zooniverse project.
TOI-700 is a red dwarf 101.4 light-years away from Earth located in the Dorado constellation that hosts TOI-700 d, the first Earth-sized exoplanet in the habitable zone discovered by the Transiting Exoplanet Survey Satellite (TESS).
TOI-700 d is a near-Earth-sized exoplanet, likely rocky, orbiting within the habitable zone of the red dwarf TOI-700, the outermost planet within the system. It is located roughly 101.4 light-years (31.1 pc) away from Earth in the constellation of Dorado. The exoplanet is the first Earth-sized exoplanet in the habitable zone discovered by the Transiting Exoplanet Survey Satellite (TESS).
LTT 3780, also known as TOI-732 or LP 729-54, is the brighter component of a wide visual binary star system in the constellation Hydra. This star is host to a pair of orbiting exoplanets. Based on parallax measurements, it is located at a distance of 72 light years from the Sun. LTT 3780 has an apparent visual magnitude of 13.07, requiring a telescope to view.
L 98-59 is a bright M dwarf star, located in the constellation of Volans, at a distance of 10.608 parsecs, as measured by Gaia.
TESS Hunt for Young and Maturing Exoplanets (THYME) is an exoplanet search project. The researchers of the THYME collaboration are mainly from the United States and search for young exoplanets using data from the Transiting Exoplanet Survey Satellite (TESS). The new discoveries should help to understand the early evolution of exoplanets. As of March 2023 the collaboration produced 9 papers announcing the discovery of exoplanets.
The TESS-Keck Survey or TKS is an exoplanet search project that uses the Keck I and the Automated Planet Finder (APF) to conduct ground-based follow-up of planet candidates discovered by the Transiting Exoplanet Survey Satellite. The TKS aims to measure the mass for about 100 exoplanets and has been awarded some of the largest time allocations in the histories of Keck I and APF. The program has four main science themes:
TOI-2180 b is a giant exoplanet orbiting the G-type star TOI-2180, also known as HD 238894. It was discovered with the help of the Transiting Exoplanet Survey Satellite and is currently the exoplanet with the longest orbital period TESS was able to uncover. TOI-2180 b orbits its host star every 260.16 days.
HD 63433 c is a mini-Neptune exoplanet orbiting the Sun-like star HD 63433. It is the outermost planet in its planetary system, being located 0.1448 astronomical units (21,660,000 km) from its star, and completing one orbit every 21 days. Despite being the outermost planet in the system, it is still located close to its star, meaning that its temperature is hot, being estimated between 267 and 406 °C. HD 63433 c is about 2.7 times larger than Earth and 15.5 times more massive, but still smaller and less massive than Neptune. In 2022, a study showed that its atmosphere, made up of hydrogen, is being evaporated by the strong radiation from its star, causing it to slowly turn into a super-Earth planet.