List of exoplanet extremes explained

The following are lists of extremes among the known exoplanets. The properties listed here are those for which values are known reliably. It is important to note that the study of exoplanets is one of the most dynamic emerging fields of science, and these values may change wildly as new discoveries are made.

Extremes from Earth's viewpoint

TitlePlanetStarDataNotes
Most distant discoveredSWEEPS-11 / SWEEPS-04SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.627 710 light-years[1] been detected.

Assuming the largest distance value 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] SGR 1935+2154 b could also be the most distant exoplanet, with distance estimates ranging from 21,500[3] to 28,400 ly.[4]

The most distant potentially habitable planet confirmed is Kepler-1606b, at 2870 light-years distant,[5] although the unconfirmed planet KOI-5889.01 is over 5000 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 17 000 light-years away.[6]

Least distant (c and d)4.25 light-yearsProxima Centauri b and (the candidate planet) d are the closest potentially rocky exoplanets,[7] b is the closest potentially habitable exoplanet known, and (the disputed planet) c is the closest mini-Neptune/Super-Earth and potentially ringed planet. 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.
Most distant directly visibleCT Chamaeleontis bCT Chamaeleontis622 light-years[8] The disputed planet candidate CVSO 30 c may be more distant, at 1,200 light-years.
Closest directly visibleEpsilon Indi AbEpsilon Indi12.05 light-yearsCOCONUTS-2b at 35.5 light-years is the next closest directly visible.Proxima Centauri c (confirmed in 2020 using archival Hubble data from 1995+) may have been directly imaged.[9]
Star with the brightest apparent magnitude with a planetAlpha Arietis bHamalApparent magnitude is 2.005Alpha Centauri A (apparent magnitude 0.01) has a planet candidate. The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.[10], a candidate planet around Vega has been detected.[11] Aldebaran (apparent magnitude varies between 0.75 and 0.95) was suspected to have a candidate planet, however later studies found the existence of the planet inconclusive.[12] Pollux (apparent magnitude 1.14) has a reported planet (Thestias), but the existence of this planet has been questioned.[13] [14] Mirfak (α Per, apparent magnitude 1.806) was claimed to have an orbiting planet, whose existence has likewise been disputed.[15]

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 be either an unrelated background object or a planetary-mass companion.[16]

Star with the faintest apparent magnitude with a planetMOA-bin-29LbMOA-bin-29LApparent magnitude is 44.61
Star with the highest apparent motion (i.e, proper motion) with a planetBarnard's Star b[17] Barnard's Star10.358
arcsec/yr[18] 		As Barnard's Star has the highest apparent motion in the sky, this is currently an absolute record.
Largest angular distance separation from its host starCOCONUTS-2bCOCONUTS-2594 arcsecondsA candidate planet or brown dwarf around BD+29 5007 might have an even larger angular separation of about 935 arcseconds.[19]
Smallest angular distance separation from its parent starSWIFT J1756.9−25080.34 microarcsecondsDerived from its separation of 0.00269 AU and its distance of ~26 000 light-years (8000 pc).[20]

Planetary characteristics

TitlePlanetStar DataNotes
Most massiveThe 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 at solar metallicity[21]), 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.[22] [23] A candidate for the most massive object that formed in a protoplanetary disk is HD 206893 b, at about . Both this object and its sibling HD 206893 c fuse deuterium.[24] [25] <---Most massive in proportion to the mass of the star(s) it revolves around
Least massivePSR B1257+12 b (Draugr)PSR B1257+12 (Lich)The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 .[26]

A candidate planet at PSR J0337+1715 is even lighter, with half of the Moon's mass or .[27]

-Least massive in proportion to the mass of the star(s) it revolves around-->
Largest radiusDH Tauri bDH Tauri [28] Next largest is PDS 70 b with 2.092.72 .[29] Proplyd 133-353 is larger at up to 7.4 – 8.0 .[30] It might be considered as a sub-brown dwarf or a rogue planet, with a photoevaporating disk.

HAT-P-67b has the largest accurately and precisely measured radius, at .[31]

Smallest radiusKepler-37bKepler-37The extrasolar planetesimals SDSS J1228+1040 b[32] and WD 1145+017 b are smaller.
Most densePSR J1719−1438 bPSR J1719−1438≥23 g/cm3 [33] According to the IAU working definition of exoplanets PSR J1719−1438 b, being slightly more massive than Jupiter, is a planet, despite it possibly formed like a white dwarf from a yellow dwarf star and suffered from the influence of the host star to become a carbon-rich diamond-like object. For reference, it is about as dense or denser than Osmium at 293 K, the densest naturally occurring element on Earth. The planetary-mass object GP Comae Berenices b might also be the remaining core of a companion star, whose density is believed to be higher than 185 g/cm3 suggesting the object is a "strange quark-planet".

TOI-4603b is the next densest with 14.1 g/cm3,[34] a mass of 12.89 MJ and a radius of 1.042 RJ.[35]

KELT-1b is similarly dense with 22.1 g/cm3.[36] But, with a mass of 27.23 MJ, it is likely a brown dwarf. Kepler-131c might be more dense at g/cm3,[37] but the value is highly uncertain.

Least denseKepler-51c and/or possibly dKepler-51[38] g/cm3 [39] The bulk density of Kepler-51 d has been constrained to be 0.038 ± 0.006 g/cm3. Next least dense are the Hot Saturn HAT-P-67 with about 0.044 g/cm3 and the super-Neptune planet WASP-193b, with 0.059 ± 0.014 g/cm3.[40]
Largest ratio of rotation rate to breakup velocityKappa Andromedae~
Hottest (irradiated hot Jupiter)KELT-9bKELT-94050 ± 180 KThe unconfirmed planets Kepler-70b and Kepler-70c may be hotter, both at >6800 K (assuming an albedo of 0.1 for both).[41]
Hottest (self-luminous)GQ Lupi bGQ Lupi2650 ± 100 K[42] Depending on its mass value, GQ Lupi b may be either a massive planet or a brown dwarf.[43]
Coldest50K[44] may be cooler, at 39K.[45]
Highest albedoLTT 9779 bLTT 97790.8[46] For comparison, Earth is 0.3 and Venus is 0.76.
Lowest albedoGeometric albedo [47] Best-fit model for albedo gives 0.04% (0.0004).
YoungestDH Tauri bDH Tauri Myr[48] The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.[49] [50] However, as a free-floating planet, it does not meet the IAU's working definition of a planet.2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr, 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[51] and 'more likely to have been produced by cloud core fragmentation' (like a star).[52]

IRAS 04125+2902 b is the youngest transiting planet at an age of 3 Myr.[53]

CI Tauri c would be the youngest radial velocity planet at an age of 2–3 Myr, if confirmed.[54]

OldestTOI-157 bTOI-157 Gyr[55] 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.[56]

Orbital characteristics

TitlePlanetStarDataNotes
Longest orbital period
(Longest year)		Gliese 900 b (CW2335+0142)Gliese 9001.27 million years[57] COCONUTS-2b previously held this record at 1,100,000 years.
Shortest orbital period
(Shortest year)		 (35 minutes)[58] K2-137b has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.[59]
Largest orbital separationGliese 900 b (CW2335+0142)Gliese 90012 000 AUUCAC4 328-061594 b has an even longer orbital separation (19 000 AU), although its mass (21 MJ) 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 resulting mass, and it could be a field brown dwarf.

The companion of ASASSN-21js has an orbit of 13 000 AU, but it is unknown if it is a brown dwarf or a planet due to its unknown mass.[60]

Smallest orbital separation0.00139 AU
Most eccentric orbitSGR 1935+21540.992 or 0.994
Highest orbital inclinationHD 204313 eHD 204313[61]
Lowest orbital inclinationHD 331093 bHD 331093[62] HD 43197 c has the lowest orbital inclination that is not a lower limit, of .[63]
Most inclined retrograde orbit//planet name here////star name here////orbital inclination here////notes here//-->
Most inclined prograde orbit//planet name here////star name here////orbital inclination here////notes here//-->
Least inclined retrograde orbit//planet name here////star name here////orbital inclination here////notes here//-->
Least inclined prograde orbit//planet name here////star name here////orbital inclination here////notes here//-->
Largest orbit around a single starCOCONUTS-2bL 34-267506 AUNext largest are 2MASS J2126–8140 with 6900 AU and HD 106906 b[64] with ~738 AU.UCAC4 328-061594 b has an even longer orbital separation (19,000 AU), although its mass [65] is higher than the deuterium burning limit .
Smallest orbit around binary star[66]
Smallest ratio of semi-major axis of a planet orbit to binary star orbit3.14 ± 0.01[67]
Largest orbit around binary starSR 12 (AB) cSR 12 AB≈1100 AU[68] SR 12 (AB) c has a mass of .ROXs 42B (AB) b is lower in mass at 9.0, however also in projected separation of ≈150 AU.[69]

, also known as Ross 458 (AB) c, at a projected separation of ≈1200 AU, with several mass estimates below the deuterium burning limit, has a latest mass determination of .[70]

Largest orbit around a single star in a multiple star systemDH Tauri bDH Tauri330 AU[71]
Largest separation between binary stars with a circumbinary planetSR 12 (AB) cSR 12 AB≈26 AUSR 12 (AB) c has a mass of at a projected separation of ≈1100 AU.FW Tauri b orbits at a projected separation of around a ≈11 AU separated binary.[72] It was shown to be more likely a star surrounded by a protoplanetary disk than a planetary-mass companion.[73]
Largest orbit around three starsGliese 900 b (CW2335+0142)Gliese 90012 000 AU
Closest orbit between stars with a planet orbiting one of the stars (S-type planet)HD 429361.139 AU[74] [75] DMPP-3 Ab's semi-major axis is around 0.067 AU. The next closest orbit between stars with an S-type planet occurs in Nu Octantis system, of which the separation between the stellar components is 2.629 AU.[76]
Smallest semi-major axis ratio between consecutive planetsKepler-36b and Kepler-36cKepler-361.11Kepler-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.-Largest semi-major-axis difference between consecutive planets
Largest semi-major axis ratio between consecutive planetsHD 83443 b and HD 83443 cHD 83443205.1 HD 83443 b and c have semi-major axes of 0.039 AU and 8.0 AU, respectively; hence the planet c is 205.1 times further from star than b.

Stellar characteristics

TitlePlanetStarData Notes
Highest metallicity+0.56 dex
Lowest metallicityK2-344bK2-344BD+20°2457 may be the lowest-metallicity planet host ([Fe/H]=−1.00); however, the proposed planetary system is dynamically unstable.[77] Planets were announced around even the extremely low-metallicity stars HIP 13044 and HIP 11952; however, these claims have since been disproven.[78]

A brown dwarf or massive planetary companion was announced around the population II star HE 1523-0901, whose metallicity is dex.[79] While the inclination of the companion is not known, if its orbit is nearly face-on, it would be sufficiently massive to become a red dwarf instead.|-| Highest stellar mass| b Centauri (AB)b| b Centauri AB| 5 - 6 M☉| Pipirima has a higher mass of,[80] but its planet candidate Mu2 Scorpii b is most likely a brown dwarf having 14.4 ± 0.8 MJ. The candidate planet M51-ULS-1b and the candidate planemo IGR J12580+0134 b might be the blanets, whose hosts have masses of ≫10 and 9 150 000 Solar masses, respectively.[81] [82]

The stars R126 (HD 37974), R66 (HD 268835) and HH 1177 in the Large Magellanic Cloud have masses of 70, 30 and 15 solar masses and have dust discs[83] but no planets have been detected yet.|-| Lowest stellar mass (main sequence)| KMT-2021-BLG-1554Lb| KMT-2021-BLG-1554L| | The mass of this star is near the hydrogen burning limit. has a lower mass of, but the value is highly uncertain.|-| Largest stellar radius| HD 208527 b| HD 208527| [84] | Other stars, such as HD 18438, Mirach and Delta Virginis are larger, but their substellar companions are more massive than the deuterium burning limit, and thus might be brown dwarfs rather than exoplanets.R Leonis [85] has a candidate planet. R Fornacis at also has a planet candidate.[86] [87]

The stars R126 and R66 in the Large Magellanic Cloud have radius of and [88] and have dust discs but no planets have been detected yet.|-| Smallest stellar radius (main sequence star)| TRAPPIST-1 planets| TRAPPIST-1| | VB 10 [89] has a disproven planet candidate.|-| Smallest stellar radius (stellar remnant)| SGR 1935+2154 b | SGR 1935+2154| |PSR B0943+10 may be a quark star. If so, its radius is predicted to be 2.6km. If a normal neutron star, its radius is 10 km.[90] |-|Highest stellar luminosity||Beta Cancri||This is the most luminous star to host a planet that is not a potential brown dwarf.The star Mirfak, whose luminosity is,[91] was claimed to have an orbiting planet with a minimum mass of 6.6 ± 0.2 Jupiter masses. However, the existence of the planet is doubtful. R Leonis (at) has a candidate planet. R Fornacis (at) also has a candidate planet. The bright giant BD+20°2457 (at [92]) was believed to have two planetary-mass companions orbiting although the claimed system configuration is dynamically unstable.

The stars R126 and R66 in the Large Magellanic Cloud have luminosities of and [93] and have dust discs but no planets have been detected yet.|-|Lowest stellar luminosity (main sequence star)|TRAPPIST-1 planets|TRAPPIST-1||[94] |-| Hottest star with a planet| PSR B0943+10 b and c| PSR B0943+10| 3 100 000 K[95] | Blackbody temperature of a small emitting area at the poles. Suggested to actually be a low-mass quark star. |-| Hottest non-degenerate star with a planet| NSVS 14256825 (AB)b| NSVS 14256825 AB| 40 000 K (primary)[96] | NN Serpentis is hotter, with a temperature of 57 000 K for the primary star, but the existence of its planets is disputed.[97] |-| Hottest normal star with a planet| b Centauri (AB)b| b Centauri AB| 18 310 ± 320 K[98] | V921 Scorpii b orbits a hotter star, at 30,000 K. Its host star is a 20-solar-mass B0IV-class subgiant.[99] However, at 60 Jupiter masses, it is not considered a planet under most definitions.The candidate planet M51-ULS-1b's supergiant primary is an O5-class supergiant with an estimated surface temperature of 40,000 K.|-| Coolest star with a planet| TRAPPIST-1 planets| TRAPPIST-1 | 2511 K| Technically Oph 162225-240515, CFBDSIR 1458+10 and WISE 1217+1626 are cooler, but are classified as brown dwarfs.The Mira-variable R Fornacis at 2100 K[100] has a planet candidate.A gas giant planet was found orbiting TVLM 513-46546[101], which is an ultracool star (2242 K) located very close to the brown dwarf/star mass boundary.[102] |}

System characteristics

TitleSystem(s)Planet(s)Star(s)Notes
System with most planetsKepler-9081Tau 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.[103] The four planets Tau Ceti e, f, g and h are considered as strong candidates.[104] HD 10180 has six confirmed planets and potentially three more planets.[105]
System with most planets in habitable zoneTRAPPIST-171Four planets in this system (d, e, f and g) orbit within the habitable zone.[106]
System with most starsKepler-64PH1b (Kepler-64b)4PH1b has a circumbinary orbit. 30 Arietis Bb was believed to be either brown dwarf or a massive gas giant in a quadruple star system until later studies revealed a true mass well above 80 MJup.[107] The quintuple star system GG Tauri has several protoplanetary disks but no planets have been detected yet.[108]
Multiplanetary system with smallest mean semi-major axis (planets are nearest to their star)Kepler-42b, c, d1Kepler-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)TYC 8998-760-1b, c1TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.
Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet)Kepler-429b, c, d1Kepler-429 b, c and d have a semi-major axis of only 0.0116, 0.006 and 0.0154 AU, respectively. The separation between closest and furthest is only 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 only 0.0016 AU (239,356 km).
Multiplanetary system with largest range of semi-major axis (largest difference between the star's nearest planet and its farthest planet)TYC 8998-760-1b, c1TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively. The separation between closest and furthest is 158 AU.-Multiplanetary system with smallest mean difference in semi-major axis between neighboring planets (orbits are most closely spaced to each other)
Multiplanetary system with largest mean semi-major axis between neighboring planets (orbits are most spread out with respect to each other)-->
System with smallest total planetary massKepler-444b, c, d, e, f3The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.
System with largest total planetary massHR 8799b, c, d, e1Four planets having > 5 Jupiter masses each.
Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively. They are likely brown dwarfs.		-System with smallest ratio of total planetary mass to stellar mass
System with largest ratio of total planetary mass to stellar mass-->
Multiplanetary system with smallest mean planetary massKepler-444b, c, d, e, f3The planets in the Kepler-444 system have radii of 0.4, 0.497, 0.53, 0.546 and 0.741 Earth radii, respectively. Due to their size and proximity to Kepler-444, these must be rocky planets, with masses close to that of Mars. For comparison, Mars has a mass of 0.105 Earth masses and a radius of 0.53 Earth radii.-Multiplanetary system with smallest ratio of mean planetary mass to stellar mass -->
Multiplanetary system with largest mean planetary massHR 8799b, c, d, e1Four planets having > 5 Jupiter masses each.
Nu Ophiuchi b and c have minimum masses of 22.206 and 24.662 Jupiter masses, respectively. They are likely brown dwarfs.		-Multiplanetary system with largest ratio of mean planetary mass to stellar mass -->
Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets)b, c1Teegarden b and c are estimated to have masses of 1.05 and 1.11 Earth masses, respectively.
Exo-multiplanetary system with largest range in planetary mass, log scale (largest proportional difference between the most and least massive planets)Kepler-37b, d1Mercury and Jupiter have a mass ratio of 5750 to 1. Kepler-37 d and b may have a mass ratio between 500 and 1000, and Gliese 676 c and d have a mass ratio of 491.

See also

External links

Notes and References

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