List of exoplanet extremes
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The following are lists of extremes among the known exoplanets. The properties listed here are those for which values are known reliably. The study of exoplanets is one of the most dynamic emerging fields of science, thus these values may change as new discoveries are made.
Extremes from Earth's viewpoint
| Title | Planet(s) | Star | Data | Notes |
|---|---|---|---|---|
| Most distant discovered | SWEEPS-11 / SWEEPS-04 | SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6 | 27,700 light-years[1] | Assuming the largest distance from the microlensing light-curve, the planet OGLE-2017-BLG-0364Lb might be more distant, at around 32,600 light-years (10,000 pc).[2]
PSR J0738-4042 at 37,000 light-years was shown to be affected by a disk of asteroids, but no planets have been detected yet.[3] The most distant potentially habitable planet confirmed is Kepler-1606b, at 2,870 light-years distant,[4] although the unconfirmed planet KOI-5889.01 is over 5,000 light-years distant. On 31 March 2022, K2-2016-BLG-0005Lb was reported to be the most distant exoplanet discovered by the Kepler telescope, at 16,960 light-years away.[5] Among rogue planets, the furthest are very likely extragalactic planets within the lensing system SDSS J1004+4112 at 6.3 billion light-years.[6] |
| Least distant | Proxima Centauri b Proxima Centauri d |
Proxima Centauri | 4.25 light-years | Proxima Centauri b is the closest potentially habitable exoplanet known. As Proxima Centauri is the closest star to the Sun (and will stay so for the next 25,000 years), this is an absolute record, unless a closer brown dwarf/compact object with a planet is discovered.
In about 25,000 years Alpha Centauri AB will be closer to the Sun than its companion Proxima Centauri. If no companion is confirmed around these two stars, no closer brown dwarf/compact object with a planet is found and no planet is found around either Ross 248 or Gliese 445, the least distant record will change in a bit earlier than 80,000 years from now, making Ross 128 b, a "temperate exoplanet in the inner edge of the habitable zone"[7] the least distant one. |
| Most distant directly visible | CT Chamaeleontis b | CT Chamaeleontis | 622 light-years[1] | The resolved likely close to equal mass binary brown dwarf NIRISS-NGC1333-10 AB, the mass of NIRISS-NGC1333-10 B is slightly higher than the deuterium burning limit, is more distant at 978 light-years.[8]
The disputed planet CVSO 30 c may be more distant, at 1,165 light-years away.[9] The candidate planet AT Pyxidis b may also be more distant, at ~1,207 light-years away.[10] Among rogue planets, o005 s41280 is the most distant at 17,300 light-years; followed by A2744-BD-1 and o006 s00089, at 15,520 and 6,520 light-years away, respectively.[11][12] As free-floating objects, all of them might not be considered as planets, although their masses might be below 13 MJ.[13] |
| Closest directly visible | Epsilon Indi Ab | Epsilon Indi | 12.05 light-years | COCONUTS-2b at 35.5 light-years is the next closest directly visible.[1]
WISE 0855-0714 is closer, at about 7.4 light-years away. As a free-floating object, it might not be considered as planet, although its mass is below 13 MJ.[13] The planet Alpha Centauri Ab is also closer (4.34 light-years) and might have been directly imaged.[14] |
| Closest Hot Jupiter type exoplanet to Earth | Upsilon Andromedae b | Upsilon Andromedae A | 44.0±0.1 ly | |
| Closest Super Jupiter type exoplanet to Earth | Epsilon Indi Ab | Epsilon Indi | 11.867±0.004 ly | |
| Closest Super Earth type exoplanet to Earth | Proxima Centauri b | Proxima Centauri | 4.2465±0.0003 ly | |
| Star with the brightest apparent magnitude (in visible) with a planet | Alpha Arietis b | Hamal[1][a] | Apparent magnitude is 2.005 | Alpha Centauri A (apparent magnitude 0.01) has a directly imaged candidate planet.[14] The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.[15] As of 2021[update], a candidate planet around Vega has been detected.[16]
Aldebaran (apparent magnitude varies between 0.75 and 0.95) was thought to have a candidate planet; however, later studies found the existence of the planet dubious.[17][18] Similarly, Pollux (apparent magnitude = 1.14) and Mirfak (apparent magnitude = 1.806) were claimed to have orbiting planets, all of which have been either questioned or disproved.[19][20][21][22][23] An Earth-mass planet claimed to orbit Alpha Centauri B (apparent magnitude = 1.33) was subsequently refuted.[24] A 2023 study detected 10 luminous point sources around the primary star of Fomalhaut system (apparent magnitude = 1.16), of which the last source may or may not be a planetary-mass companion.[25] This star was previously thought to harbour a directly imaged planet named Fomalhaut b, before the realization of object as an expanding debris cloud from a planetesimal collision.[26] |
| Star with the faintest apparent magnitude (in visible) with a planet | MOA-bin-29Lb | MOA-bin-29L | Apparent magnitude is 44.61[1] | |
| Closest planet to the celestial north pole (i.e. highest declination) | TOI-1691 b | TOI-1691 | Declination of +86° 51′ 37.23″[1] | |
| Closest planet to the celestial south pole (i.e. lowest declination) | HD 110082 b | HD 110082 | Declination of −88° 07′ 16″[1] | |
| Star with the highest apparent motion (i.e. proper motion) with a planet | Barnard planets[27] | Barnard's Star | 10.358 arcsec/yr[28] |
As Barnard's Star has the highest apparent motion in the sky,[28] this is currently an absolute record. |
| Largest angular distance separation from its host star | COCONUTS-2b | COCONUTS-2 | 594 arcseconds[29] | A candidate planet or brown dwarf around BD+29 5007 has an even larger angular separation of about 935 arcseconds.[30] |
| Smallest resolved angular distance separation from its parent star | Beta Pictoris c | Beta Pictoris | 0.138 arcseconds | Derived from its separation of ~2.68 AU[31] and its distance of 63.4 light-years (19.4 parsecs). |
| Smallest angular distance separation from its parent star | NGC 6440 X-2 b | NGC 6440 X-2 | 0.31 microarcseconds | Derived from its separation of 0.00255 AU and its distance of ~27,070 light-years (8,300 parsecs).[32] |
| Star with the largest apparent size (angular diameter) | Alpha Arietis b | Hamal | 7.006±0.027 mas | Accounted for the limb darkening effect.[33]
Several stars have a larger angular diameter and were claimed to have candidate planets: Aldebaran (20.58±0.03 mas),[17][34] L2 Puppis (17.9±1.6 mas)[35][36] and Alpha Centauri A (8.314±0.016 mas).[14][37] |
Planetary characteristics
| Title | Planet | Star | Data | Notes |
|---|---|---|---|---|
| Most massive | The most massive planet is difficult to define due to the blurry line between planets and brown dwarfs. If the borderline is defined as the deuterium fusion threshold (roughly 13 MJ at solar metallicity[38][b]), the most massive planets are those with true mass closest to that cutoff; if planets and brown dwarfs are differentiated based on formation, their mass ranges overlap.[39][40]: 62 A candidate for the most massive object that formed in a protoplanetary disk is CWW 89Ab, at about 36 MJ. This object is massive enough to have fused deuterium early in its life, but its atmosphere indicates it may have formed via the very high-mass end of the planet formation process.[41] | |||
| Most massive in proportion to the mass of the star(s) it revolves around | Delorme 1 b | Delorme 1 | Mass ratio is ~0.034 | 2M1207 b has a larger ratio to 2M1207 of ~0.2, but the host is a brown dwarf. 2M1207 b may be a sub-brown dwarf instead of a planetary-mass companion.[42]
The planet candidate NSV 1440 b has a higher mass ratio at 0.045 ± 0.002 to its host star, which is a white dwarf. However, with a mass near 30 MJ, it is likely a companion star that was stripped down to a substellar-mass object.[43] |
| Most massive in proportion to the mass of the host object it revolves around | CFHTWIR-Oph 98 b | CFHTWIR-Oph 98 A | Mass ratio is ~0.51[c] | Both, this object[44] and (DRS2009) 1996[45] with a mass ratio of ~0.35[d] may be sub-brown dwarfs instead of a planetary companion. |
| Least massive | PSR J0337+1715 (AB) b | PSR J0337+1715 | 0.0041±0.003 M🜨[46] | A 2025 study cast doubt on the existence of the planet, instead attributing it to "red noise", variability within the pulsar itself, which can appear as a planet.[47]
The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 M🜨.[29] As a reference, the mass of Earth's moon is 0.012 M🜨.[48] |
| Largest radius | DH Tauri b | DH Tauri | 2.7±0.8 RJ[49] | Proplyd 133-353 is larger at up to 7.4±0.3 – 8.0±1.1 RJ.[50][e] It might be considered as a sub-brown dwarf or a rogue planet, with a photoevaporating disk.
The largest transiting planet known is HAT-P-67 b at 2.140±0.025 RJ.[51] |
| Smallest radius | Kepler-37b | Kepler-37 | 0.296±0.037 R🜨[1] | The extrasolar planetesimal WD 1145+017 b is smaller. |
| Smallest radius with a confirmed atmosphere | TOI-561 b | TOI-561 | 1.39 R🜨[1] | [52] The planet LHS 1478 b is smaller (at 1.17 R🜨) and might have an atmosphere.[53] |
| Most dense | GP Comae Berenices b | GP Comae Berenices | ≥185 g/cm3[54] | According to the IAU working definition of exoplanets GP Comae Berenices b, being 10 times more massive than Jupiter, is a planet, despite that it might have formed as a white dwarf that was stripped down to a planetary-mass object. For reference, it is a lot denser than osmium at 293 K, the densest naturally occurring stable element on Earth. It is suspected that GP Comae Berenices b might be composed of strange matter based on its density.[54]
TOI-4603 b is the densest planet which orbits a normal star and is not a potential brown dwarf, with 14.1+1.7 |
| Least dense | Kepler-51d | Kepler-51[56] | 0.0381±0.0085 g/cm3[57] | Next least dense are the super-Neptune planet WASP-193b with 0.059±0.014 g/cm3[58] and the hot Jupiter HAT-P-67b with 0.060+0.020 −0.021 g/cm3,[59] tied with Kepler-51 b with 0.060±0.037 g/cm3.[57] A predicted highly evaporating planet was proposed to orbit the star FU Orionis with a density of about 0.0042 g/cm3.[f] |
| Highest planetary rotation rate | Beta Pictoris b | Beta Pictoris | 19.9±1.0 km/s | Value measured at the planetary equator.[61] |
| Hottest (irradiated planet) | KELT-9b | KELT-9 | 4,050±180 K[1] (3,777 °C) | The candidate planets OGLE-TR-1001b and KOI-2093.03 are hotter, at 4,200 K and 6,285 K, respectively.[62][63]
A candidate planet was suggested to orbit WD 2226-210, the central star of the Helix Nebula, with an equilibrium temperature of 4,970 K.[64] Kepler-70b and Kepler-70c are often described as the hottest known exoplanets, both at >6,800 K (assuming an albedo of 0.1 for both),[65] but their existences are highly doubtful.[66][67] |
| Hottest (self-luminous) | GQ Lupi b | GQ Lupi | 2,650±100 K[68] (2,377 °C) |
GQ Lupi b may be either a massive planet or a brown dwarf.[68] |
| Coldest | OGLE-2005-BLG-390Lb | OGLE-2005-BLG-390L | 50 K (−223.2 °C)[69][g] | The disputed planet Proxima Centauri c may be cooler, at 39 K (−234.2 °C).[70] |
| Fastest jetstream wind | WASP-127b | WASP-127 | 33,000 km/h (9,200 m/s)[71] |
|
| Strongest magnetic field | Tau Boötis b | Tau Boötis | 117±38 G[h] | For comparison, the field strength of Jupiter is 4.17 G.[73]
The magnetic field of SIMP J013656.5+093347 is stronger at ~3,200 G.[74] As a free-floating object, it might not be considered a planet.[13] |
| Highest albedo | LTT 9779 b | LTT 9779 | 0.79±0.15[75] | This is value for the western dayside region, with the overall albedo of dayside being 0.50±0.07.[75]
For comparison, the albedo values of Earth and Venus are 0.3 and 0.76, respectively. |
| Lowest albedo | TrES-2b | GSC 03549-02811 | Geometric albedo < 1%[76] | Best-fit model for albedo gives 0.04% (0.0004).[65] |
| Youngest | DH Tauri b | DH Tauri | 0.7+0.3 −0.2 Myr[77] |
The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.[50][78] However, as a free-floating planet, it does not meet the IAU's working definition of a planet.[79]
2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr,[1] but fails the mass ratio criterion of the IAU working definition of an exoplanet; the mass ratio with the primary is larger than the L4/L5 limit of stability ≈ 1/25[79] and the companion is 'more likely to have been produced by cloud core fragmentation' (which is similar to a star).[80] Two planetary candidates proposed to orbit IRS 63 might be younger at ≲0.5 Myr.[81] IRAS 04125+2902 b is the youngest transiting planet at an age of ~3 Myr.[82] HD 114082b is the youngest radial velocity planet at an age of 15±6 Myr.[83][84] CI Tauri c would be the youngest radial velocity planet at an age of 2–3 Myr, if confirmed.[85][i] |
| Oldest | TOI-157 b | TOI-157 | 12.82+0.73 −1.40 Gyr[88] |
The currently accepted age of the universe is around 13.8 billion years. Could alternatively be PSR B1620-26 b with 11.2–12.7 Gyr.[89]
Two disproven planets had been thought to orbit the star HIP 11952,[90] whose age is 12.8±2.6 Gyr.[91] The star HE 1523-0901 might be older at 13.2 Gyr[92] and has a candidate planet or brown dwarf.[93] |
Orbital characteristics
| Title | Planet | Star | Data | Notes |
|---|---|---|---|---|
| Longest orbital period (Longest year) |
Gliese 900 b (CW2335+0142) | Gliese 900 | 1.27 million years[94][1][j] | COCONUTS-2b previously held this record at 1.1 million years.[j] |
| Shortest orbital period (Shortest year) |
GALEX 0718+3731 b | GALEX 0718+3731 | 0.187 h (11.2 minutes)[1] | KOI 1843.03 has the shortest orbit around a main-sequence star (an M dwarf) at 4.25 hours.[95] |
| Largest orbital separation | Gliese 900 b (CW2335+0142) | Gliese 900 | 12,000 AU[96][1] | UCAC4 328-061594 b has an even larger orbital separation (19,000 AU), although its mass (21 MJ)[1][96] is higher than the deuterium burning limit (13 MJ).
Another candidate around BD+29 5007 has an even larger orbit of about 22,100 AU. There is no consensus about its age and the resulting mass, and it could be a field brown dwarf. The companion of ASASSN-21js has an orbit of about 13,000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass.[97] |
| Smallest orbital separation (smallest semi-major axis) | GALEX 0718+3731 b | GALEX 0718+3731 | 0.000834 AU[1] | TOI-6324 b has the smallest orbital separation from a main-sequence star (an M dwarf) at ~0.0043 AU.[98] |
| Most eccentric orbit | HD 20782 b | HD 20782 | 0.950[1] | Could alternatively be HD 28254 b with an eccentricity at 0.95+0.03 −0.04.[1] The possible planets HD 205577 b, SGR 1935+2154 b and SGR 1806-20 b have even higher eccentricities at 0.972+0.08 The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.[101] |
| Highest orbital inclination | HD 204313 e | HD 204313 | 176.092°+0.963° −2.122°[1] |
[102][103] |
| Lowest orbital inclination | HD 331093 b | HD 331093 | >0.3704°[103][1] | [104] HD 43197 c has the lowest orbital inclination that is not a lower limit, of 11.42°+5.388° −3.07°.[103] |
| Largest semi-amplitude | WASP-18b | WASP-18 | 1,814+23 −24 m/s |
[105] The planetary-mass objects CoRoT-3b, GPX-1 b and KELT-1Ab have larger semi-amplitudes at 2,173±25 m/s,[106] 2,310±180 m/s[107] and 4,239±52 m/s,[108] respectively; however, they are likely brown dwarfs rather than planets.[109] |
| Smallest semi-amplitude | Barnard's Star e | Barnard's Star | 0.221±0.038 m/s | [27] |
| Largest orbit around a single star | COCONUTS-2b | L 34-26 | 7506 AU[1] | Next largest are 2MASS J2126–8140 with 6,900 AU and WD 0806-661 b[110] with ~2500 AU.
UCAC4 328-061594 b has a significantly larger orbital separation (about 19,000 AU), although its mass (21 MJ)[1][96] is higher than the deuterium burning limit (13 MJ). |
| Smallest orbit around binary star | Kepler-47b | Kepler-47 | 0.2877+0.0014 −0.0011 AU[1] |
[111]
Kepler-1521 b has a smaller orbit with semi-major axis at 0.2347±0.0011 AU.[1] The planet might be circumbinary, as the binarity of host star is suggested but not confirmed.[112] |
| Smallest ratio of semi-major axis of binary star orbit to a planet orbiting one of the stars (S-type planet) | Nu Octantis Ab | Nu Octantis | 2.06 | [113] |
| Largest orbit around binary star | SR 12 c | SR 12 | ≈1100 AU[114] | SR 12 c has a mass of 0.013±0.007 M☉.[114]
DT Virginis c, also known as Ross 458 c, at a projected separation of ≈1200 AU, with several mass estimates below the deuterium burning limit, has a latest mass determination of 27±4 MJ.[115] The binary 2MASS J0249-0557 AB has a planetary-mass companion less massive than 13 MJ at a larger separation of 1,950±200 AU, although this companion might have formed as a brown dwarf based on the mass ratio to the host stars.[116] |
| Largest orbit around a single star in a multiple star system | DH Tauri b | DH Tauri | ≈330 AU[117] | |
| Largest separation between binary stars with a circumbinary planet | SR 12 c | SR 12 | ≈26 AU[114] | SR 12 c has a mass of 0.013±0.007 M☉ at a projected separation of ≈1,100 AU.[114] FW Tauri b orbits at a projected separation of 330±30 AU around a ≈11 AU separated binary.[118] It was shown to be likely a 0.1 M☉ star surrounded by a protoplanetary disk rather than a planetary-mass companion.[119] |
| Largest orbit around three stars | Gliese 900 b (CW2335+0142) | Gliese 900 | 12,000 AU[96][1] | |
| Closest orbit between stars with a planet orbiting one of the stars (S-type planet) | DMPP-3 Ab | HD 42936 | 1.139 AU[120][121] | DMPP-3 Ab's semi-major axis is around 0.067 AU. |
| Closest orbit between stars with planets orbiting both the stars | Struve 2398 Ab and Struve 2398 Bc | Struve 2398 A and Struve 2398 B | 63±1 AU | The only known planet of Struve 2398 A has a semi-major axis of 0.068 AU while the confirmed planet of Struve 2398 B has a semi-major axis of 0.139 AU.[122][123] |
| Smallest semi-major axis ratio between consecutive planets | Kepler-36b and Kepler-36c | Kepler-36 | 1.11 | Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively; hence the planet c is 1.11 times further from star than b.
2MASS J1657-5343 b and 2MASS J1657-5343 c have semi-major axes of 165 AU and 180 AU, resulting in the planet c being ~1.09 times further from star than b.[124][125] Despite being listed in Extrasolar Planets Encyclopaedia as planets, these companions are most likely brown dwarfs based on the mass. There have been unconfirmed detections of co-orbital pairs of exoplanet, each of which has a semi-major axis ratio of almost 1. |
| Largest semi-major axis ratio between consecutive planets | WASP-4b and WASP-4c | WASP-4 | 347.1 | WASP-4b and c have semi-major axes of 0.0229 AU and ≈7.95 AU,[126] respectively; hence the planet c is about 347.1 times further from star than b.
The disputed planets CVSO 30 b and CVSO 30 c[127] have semi-major axes of 0.0084 AU and 662±96 AU,[128] respectively. This might result in a larger ratio at 67380:1 – 90240:1. |
Stellar characteristics
| Title | Planet | Star | Data | Notes |
|---|---|---|---|---|
| Highest metallicity | HD 126614 Ab | HD 126614 A | +0.56 dex | Located in a triple star system. |
| Lowest metallicity | K2-344b | K2-344 | −0.95±0.02 dex[1] | BD+20 2457 may be the lowest-metallicity planet host ([Fe/H]=-1.00); however, the proposed planetary system is dynamically unstable.[129][k]
Planets were announced around even the extremely low-metallicity stars HIP 13044 and HIP 11952; however, these claims have since been disproven.[90] A brown dwarf or planetary-mass companion was announced around the population II star HE 1523-0901, whose metallicity is −2.65±0.22 dex.[131] While the inclination of the companion is not known, if its orbit is nearly face-on, it would be sufficiently massive to be a red dwarf instead.[93] A disputed substellar companion, possibly a Jovian planet, was announced to orbit[132] the B-type subdwarf star HD 149382 with a metallicity of -1.30 dex.[133] |
| Lowest color index | b Centauri b | b Centauri | −0.157±0.002[134] | The subgiant star Pipirima has a lower B-V color index at -0.219;[135] however, its planetary-mass companions Mu2 Scorpii b and (the candidate) Mu2 Scorpii c might be either brown dwarfs or planets.[136] |
| Highest color index | GJ 3512 b and GJ 3512 c | GJ 3512 | +1.904±0.046[137] | For reference, the Sun with its eight confirmed planets has a B-V color index of +0.656.[138]
A candidate planet was reported around the carbon star V Hydrae,[139] whose B-V color index is higher at +5.43.[140] |
| Highest stellar mass | b Centauri b | b Centauri | 5–6 M☉ | The subgiant star Pipirima has a higher mass of 9.1±0.3 M☉,[141] but its planetary-mass companions Mu2 Scorpii b and (the candidate) c might be either brown dwarfs or planets.[136]
The candidate planemo IGR J12580+0134 b might be a blanet, whose host has a mass of 300,000 to 18 million M☉.[142] The candidate exoplanet M51-ULS-1 b orbits two objects, a B-type supergiant with a mass of 20 M☉,[143] and a neutron star or black hole with a mass of 1.4 to 10 M☉.[144][l] The star Mirfak (at 7.3±0.3 M☉)[145] has disproved orbiting planets.[23] The stars R126 (HD 37974), R66 (HD 268835) and HH 1177 in the Large Magellanic Cloud have masses of 70, 30 and 12 M☉ and have dust discs[146] but no planets have been detected yet. |
| Lowest stellar mass (Main-sequence) | KMT-2021-BLG-1554Lb | KMT-2021-BLG-1554L | 0.08+0.013 −0.014 M☉[103] |
The mass of this star is near the hydrogen burning limit.
KMT-2016-BLG-2142L has a lower mass of 0.073+0.117 |
| Largest stellar radius | HD 220074 b | HD 220074 | 59.60+5.85 −6.31 R☉[147] |
Other stars, such as HD 18438, Mirach and Delta Virginis are larger, but their substellar companions are more massive than the deuterium burning limit at about 13 MJ, and thus might be brown dwarfs rather than exoplanets.[1]
Candidate planets were reported around the red giants V Camelopardalis (716±185 R☉),[148][149] R Fornacis (585 R☉[m]),[150][151] V Hydrae (430 R☉),[139] R Leonis (320−350 R☉)[148][152] and L2 Puppis (123±14 R☉).[36] The stars R126 and R66 in the Large Magellanic Cloud have radii of 78 R☉ and 131 R☉[153] and have dust discs but no planets have been detected yet. |
| Smallest stellar radius | PSR J1211-0633 b | PSR J1211-0633 | 0.0000143 R☉ (9.9 km)[154] |
A hypothetical planet was proposed to orbit SGR 1935+2154, whose radius is smaller at 4.35 km (6.25×10−6 R☉).[155][156] |
| Smallest stellar radius (brown dwarf) | TVLM 513-46546b | TVLM 513-46546 | 0.097–0.109 R☉[157] | Lower than that of any brown dwarf in the NASA Exoplanet Archive.[103] |
| Smallest stellar radius (main-sequence star) | TRAPPIST-1 planets | TRAPPIST-1 | 0.1192±0.0013 R☉[158] | VB 10 (at 0.102 R☉)[159] has a disproven planet candidate. |
| Highest stellar luminosity | HD 158996 b | HD 158996 | 849.2 L☉[147][n] | This is the most luminous star to host a confirmed planet that is not a potential brown dwarf.[103]
The star Mirfak, whose luminosity is 3780 L☉,[160] was claimed to have an orbiting planet with a minimum mass of 6.6±0.2 MJ. However, the existence of the planet is doubtful.[22] Candidate planets were reported around the red giants V Hydrae (at 18,000 L☉),[139][161] U Equulei (at ~6,000 L☉),[162][163] R Fornacis (at 5,800 L☉),[150] R Leonis (at 3,537 L☉),[152] L2 Puppis (at 1,490±150 L☉)[36][164] and BD+20 2457 (at 1,479 L☉).[165][166] The host star system of the unconfirmed planet M51-ULS-1 b has a luminosity of ≈260,000 L☉.[144][o] The stars R126, R66 and HH 1177 in the Large Magellanic Cloud have luminosities of 1.4 million L☉, 320,000 L☉ and 19,000 L☉[146][153] and have dust discs but no planets have been detected yet. |
| Lowest stellar luminosity (main-sequence star) | TRAPPIST-1 planets | TRAPPIST-1 | 0.0005495 L☉ | [167][103] |
| Highest stellar rotational velocity | Kappa Andromedae b | Kappa Andromedae | ~176 km/s [168] | The star HIP 64892 rotates slightly faster at projective velocity 178 km/s; however, its orbiting companion, which weighs at ~29–37 MJ and is listed as a planet by EPE,[169] might be most likely a brown dwarf.[170]
The stars 51 Ophiuchi, HD 38056 and Phi Leonis rotate at 267±5 km/s,[171] ~195 km/s[172] and ~254 km/s,[173] respectively, and have dust discs but no planets have been detected yet. |
| Hottest star with a planet | SWIFT J1756.9−2508 b | SWIFT J1756.9−2508 | 4.64 million K | [p] |
| Hottest non-compact star with a planet | NSVS 14256825 planets | NSVS 14256825 | 40,000 K (primary)[175] | NN Serpentis is hotter, with a temperature of 57,000 K for the primary star,[1] but the existence of its planets is disputed.[176]
A candidate planet was found orbiting the O-type subdwarf TOI-709, whose effective temperature is higher at 50,000 K.[177] |
| Hottest main-sequence star with a planet | b Centauri b | b Centauri | 18,310±320 K[178] | |
| Coolest star with a planet | TRAPPIST-1 planets | TRAPPIST-1 | 2,511 K | Technically the primary components of Oph 162225-240515, CFBDSIR 1458+10, WISE J0336−0143 and WISE 1217+1626 are cooler, but are classified as brown dwarfs.
The cooler stars R Fornacis at 2,100 K[179] and V Camelopardalis at 2,414±86 K[149] were both claimed to have a planet candidate.[148][151] A gas giant planet was found orbiting TVLM 513-46546,[180] which is an ultracool star (2,242 K) located close to the brown dwarf/red dwarf mass boundary.[181] |
System characteristics
| Title | System(s) | Planet(s) (in order from star) | Star(s) | Notes |
|---|---|---|---|---|
| System with most planets | Kepler-90 | 8 (b, c, i, d, e, f, g, h) |
1 | Tau Ceti currently has no confirmed planetary companion, although it has been proposed that the number of orbiting planets may be 8, 9 or even 10.[182] The four planets Tau Ceti e, f, g and h are considered as strong candidates.[183]
HD 10180 has six confirmed planets and potentially three more planets.[184] As a reference, the Solar System has eight verified major planets, alongside multiple dwarf planets (the existence of Planet Nine and Planet Ten is yet unconfirmed).[185][q][189] |
| System with most planets in habitable zone | TRAPPIST-1 | 4 (b, c, d, e, f, g, h) |
1 | Four planets in this system (d, e, f and g) orbit within the circumstellar habitable zone.[190] |
| System with most planets in exact orbital resonance | HD 110067 | 6 (b, c, d, e, f, g) |
3 | Each consecutive pair of the planets b, c, d, e, f and g is locked in the resonance of 3:2, 3:2, 3:2, 4:3 and 4:3, respectively.[191] |
| System with most stars | Kepler-64 | b | 4 | PH1b (Kepler-64b) has a circumbinary orbit.
30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system before later studies revealing a true mass well above the red dwarf-mass limit of 80 MJ.[192] The planetary mass-companion HIP 81208 Cb will be potentially located in a quadruple star system, if the star Gaia DR3 6020420074469092608 is confirmed to be gravitationally bound to the system.[193] The quintuple and quadruple star systems GG Tauri and HD 98800 both have several protoplanetary disks but no planets have been detected yet.[194][195] Similarly, the star β3 Tucanae A, located in a sextuple star system, was suggested to have a debris disk with no planets having been found.[196] |
| System with most stellar-like objects | Kepler-64 | b | 4 | PH1b (Kepler-64b) has a circumbinary orbit.
The polar circumbinary planet 2M1510 b is located in either a tertiary or a quadruple system of brown dwarfs.[197] The planetary-mass object 2MASS J04414489+2301513 b is within a quadruple system with one star and two brown dwarfs. |
| Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star) | Kepler-42 | b, c, d | 1 | Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively.
Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. |
| Multiplanetary system with largest mean semi-major axis (planets are farthest from their star) | YSES 1 | b, c | 1 | YSES 1 b and c have a semi-major axis of ~162 and ~320 AU, respectively.[1] |
| Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet) | Kepler-42 | b, c, d | 1 | Kepler-42 b, c and d have a semi-major axis of 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is therefore 0.0094 AU.
Kepler-70 b, c and d (all unconfirmed and disputed) have a semi-major axis of only 0.006, 0.0076 and ~0.0065 AU, respectively. The separation between closest and furthest is therefore shorter at 0.0016 AU (240,000 km). |
| Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet) | AB Pictoris | c, b | 1 | AB Pictoris b and c have semi-major axes of ~190 and ~4 AU,[198] respectively. The separation between closest and furthest is thus around 186 AU.
Two planetary-mass objects with masses slightly above the deuterium limit Mu2 Scorpii b and c (the later is unconfirmed) have semi-major axes of ~19 and ~242 AU, respectively; hence the range of semi-major axis is about 223 AU.[136] |
| System with smallest total planetary mass | Barnard's Star | d, b, c, e | 1 | The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively.[27]
For comparison, Mars has a mass of 0.105 Earth masses. |
| System with largest total planetary mass | HR 8799 | e, d, c, b | 1 | Four planets each having masses within the range 6.0 – 9.6 MJ. The total mass might be larger as there might be an additional planet orbiting HR 8799 with a mass of 4 – 7 MJ.[199] Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively.[1] They are likely brown dwarfs. HD 81817 b and c have masses of 24.1 and ≥22.6 Jupiter masses, respectively.[31] These companions are also likely brown dwarfs. |
| Multiplanetary system with smallest mean planetary mass | Barnard's Star | d, b, c, e | 1 | The planets d, b, c and e have minimum masses of 0.263, 0.299, 0.335 and 0.193 Earth masses, respectively.[27]
For comparison, Mars has a mass of 0.105 Earth masses. |
| Multiplanetary system with largest mean planetary mass | Titawin | b, c, d | 2 | The three planets b, c and d have masses of 1.70+0.33 −0.24, 14.0+2.3 −5.3 and 10.2+0.7 −3.3 Jupiter masses, respectively. This results in a mean planetary mass of 5.7 – 9.7 MJ.[200][201] Could alternatively be the system of HR 8799, in which four planets each have masses within the range 5.7 – 9.1 MJ. Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively.[1] They are likely brown dwarfs. HD 81817 b and c have masses of 24.1 and ≥22.6 Jupiter masses, respectively.[31] These companions are also likely brown dwarfs. |
| Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets) | HD 37124 | b, c, d | 1 | HD 37124 c and d are estimated to have masses of 0.652 and 0.69 Jupiter masses, respectively (hence a ratio of about 1.058 to 1).[202] |
| Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets) | Gliese 676A | d, e, b, c | 2 | Gliese 676A c and d have a mass ratio of about 975 to 1.[r] For comparison, Mercury and Jupiter have a mass ratio of 5,780 to 1.
The planet KMT-2020-BLG-0414Lc and the super-Earth KMT-2020-BLG-0414Lb have a mass ratio of about 4,590 to 1,[s] although at 27.0+4.0 |
