List of exoplanet extremes

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

[edit]

Title  | Planet  | Star  | Data  | Notes

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Most distant discovered  | SWEEPS-11 / SWEEPS-04 | SWEEPS J175902.67−291153.5 / SWEEPS J175853.92−291120.6  | 27,710 light-years[1] | Several candidate extragalactic planets have 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]

The most distant potentially habitable planet confirmed is Kepler-1606b, at 2,870 light-years distant,[3] 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 17,000 light-years away.[4]

Least distant | Proxima Centauri b, c and d | Proxima Centauri | 4.25 light-years  | Proxima Centauri b and d are the closest rocky exoplanets, b is the closest potentially habitable exoplanet known, and c is the closest mini-Neptune 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 visible  | CT Chamaeleontis b | CT Chamaeleontis | 622 light-years[5] | The disputed planet candidate CVSO 30 c may be more distant, at 1,200 light-years.
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.[5]

Proxima Centauri c (confirmed in 2020 using archival Hubble data from 1995+) may have been directly imaged.[6]

Star with the brightest apparent magnitude with a planet  | Alpha Arietis b  | Hamal[5][a] | Apparent magnitude is 2.005  | Alpha Centauri A (apparent magnitude 0.01) has an planet candidate. The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it.[7] As of 2021[update], a candidate planet around Vega has been detected.[8]

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.[9] Pollux (apparent magnitude 1.14[10]) has a reported planet (Thestias), but the existence of this planet has been questioned.[11][12] Mirfak (α Per, apparent magnitude 1.806) was claimed to have an orbiting planet, whose existence has likewise been disputed.[13]

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.[14]

Star with the faintest apparent magnitude with a planet  | MOA-bin-29Lb | MOA-bin-29L | Apparent magnitude is 44.61[5] |
Largest angular distance separation from its host star  | COCONUTS-2b | COCONUTS-2 | 594 arcseconds[15] |

## Planetary characteristics

[edit]

Title  | Planet  | Star  | Data  | Notes

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Least massive  | PSR B1257+12 b (Draugr)  | PSR B1257+12 (Lich)  | 0.020±0.002 M🜨[5] | The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 ME.[15]
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[16][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.[17][18]: 62 A candidate for the most massive object that formed in a protoplanetary disk is HD 206893 b, at about 28 MJ. Both this object and its 13 MJ sibling HD 206893 c fuse deuterium.[19][20]
Largest radius | DH Tauri b  | DH Tauri | 2.6±0.7 – 2.7±0.8 RJ[21] | Next largest is PDS 70 b with 2.09+0.23
−0.31 - 2.72+0.15
−0.17 RJ.[22]

Proplyd 133-353 is larger at 7.4±0.3 – 8.0±1.1 RJ.[23][c] It might be considered as a sub-brown dwarf or a rogue planet, with a photoevaporating disk.

HAT-P-67b has the largest accurately measured radius, at 2.085+0.096
−0.071 RJ.[24][25]

Smallest radius | Kepler-37b | Kepler-37 | 0.296±0.037 R🜨[5] | The extrasolar planetesimals SDSS J1228+1040 b[26] and WD 1145+017 b are smaller.
Most dense  | TOI-4603b | HD 245134 | 14.1+1.7
−1.6 g/cm3 [27] | TOI-4603b has a mass of 12.89+0.58
−0.57 MJ and a radius of 1.042+0.038
−0.035 RJ.[28]

KELT-1b is denser, with 22.1+5.62
−9.16 g/cm3.[29] But, with a mass of 27.23 MJ, it is likely a brown dwarf. Kepler-131c might be more dense at 77.7+55
−55 g/cm3,[30] but the value is highly uncertain.

Least dense  | Kepler-51c, b and/or possibly d[31] | Kepler-51[31] | ~ 0.03 g/cm3[31] | The bulk densities of Kepler-51 b and c have been constrained to be below 0.05 g/cm3 (expected value 0.03 g/cm3 for each). The density of Kepler-51d is determined to be 0.046 ± 0.009 g/cm3[31]. Next least dense is super-Neptune planet WASP-193b, with 0.059 ± 0.014 g/cm3.[32]
Hottest (irradiated hot Jupiter)  | KELT-9b | KELT-9 | 4,050±180 K[5](3777 °C)  | The unconfirmed planets Kepler-70b and Kepler-70c may be hotter, both at >6,800 K (assuming an albedo of 0.1 for both).[33]
Hottest (self-luminous)  | GQ Lupi b | GQ Lupi | 2,650±100 K[34](2377 °C)  | Depending on its mass value, GQ Lupi b may be either a massive planet or a brown dwarf.[35]
Coldest |  OGLE-2005-BLG-390Lb |  OGLE-2005-BLG-390L | 50 K (−223.2 °C)[36][d] | The disputed planet Proxima Centauri c may be cooler, at 39 K (−234.2 °C).[37]
Highest albedo | LTT 9779 b | LTT 9779 | 0.8[38] | For comparison, Earth is 0.3 and Venus is 0.76.
Lowest albedo  | TrES-2b | GSC 03549-02811 | Geometric albedo < 1%[39] | Best-fit model for albedo gives 0.04% (0.0004).[33]
Youngest  | CHXR 73 b  | CHXR 73 | 2 Myr[5] | The free-floating planet or sub-brown dwarf Proplyd 133-353 is younger, at 0.5 Myr.[40][41] However, as a free-floating planet, it does not meet the IAU's working definition of a planet.[42]

2MASS J04414489+2301513 b is listed as the youngest planet in the NASA Exoplanet Archive, at an age of 1 Myr,[5] but fails the mass ratio criterion of the IAU working definition of an exoplanet; the mass ratio with the primary is smaller than ~1/25[42] and 'more likely to have been produced by cloud core fragmentation' (like a star).[43]

K2-33b is the youngest transiting planet, at an age of 9.3 Myr.[44]

Oldest  | PSR B1620-26 b | PSR B1620-26 | 11.2–12.7 Gyr[45] | The currently accepted age of the universe is around 13.8 billion years.

## Orbital characteristics

[edit]

Title  | Planet  | Star  | Data  | Notes

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Longest orbital period
(Longest year) | Gliese 900 b (CW2335+0142)  | Gliese 900 | 1.4 million years[46] | COCONUTS-2b previously held this record at 1,100,000 years.
Shortest orbital period
(Shortest year) | PSR J1719-1438 b | PSR J1719-1438 | 2.17695 h (131 minutes)[47] | A substellar object announced around the pulsar SWIFT J1756.9−2508 may have a shorter orbital period of under an hour, around 54 minutes.[48] M62H b has an orbit almost exactly 1 hour longer.[49] A planetary-mass object orbiting the white dwarf GP Comae Berenices has an even shorter orbital period of 46 minutes and is sometimes listed as an exoplanet.[50] However, it is more likely the remaining core of a former white dwarf being highly disrupted.[51]

K2-137b has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.[52]

Largest orbital separation  | Gliese 900 b (CW2335+0142)  | Gliese 900 | 12,000 AU[53][5] |
Smallest orbital separation  | PSR J1719-1438 b | PSR J1719−1438 | 0.0044 AU (658,230 km)  | [54]
Most eccentric orbit | HD 20782 b[55] | HD 20782 | 0.956±0.004 | [56] Record among confirmed planets. The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.[57] HD 80606 b previously held this record at 0.93226+0.00064
−0.00069.
Highest orbital inclination | HD 204313 e | HD 204313 | 176.092°+0.963°
−2.122° | [58][59]
Lowest orbital inclination  | HD 331093 b | HD 331093 | >0.3704° | [60][59] HD 43197 c has the lowest orbital inclination that is not a lower limit, of 11.42°+5.388°
−3.07°.[59]
Largest orbit around a single star  | COCONUTS-2b | L 34-26 | 7,506 AU  | Next largest are 2MASS J2126–8140 with 6,900 AU and HD 106906 b[61] with ~738 AU.

UCAC4 328-061594 b has an even longer orbital separation (19,000 AU), although its mass (21 MJ)[5][53] is higher than the deuterium burning limit (13 MJ).

Smallest orbit around binary star  | Kepler-47b | Kepler-47AB | 0.2877+0.0014
−0.0011 AU[5] | [62]
Smallest ratio of semi-major axis of a planet orbit to binary star orbit  | Kepler-16b | Kepler-16AB | 3.14 ± 0.01  | [63]
Largest orbit around binary star  | SR 12 (AB) c | SR 12 AB | ≈1100 AU[64] | SR 12 (AB) c has a mass of 0.013±0.007 M☉.[64]

ROXs 42B (AB) b is lower in mass at 9.0+6
−3 MJ, however also in projected separation of ≈150 AU.[65]

DT Virginis c, 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 27±4 MJ.[66]

Largest orbit around a single star in a multiple star system  | ROXs 12 b | ROXs 12 | 210±20 AU[5] |
Largest separation between binary stars with a circumbinary planet  | SR 12 (AB) c | SR 12 AB | ≈26 AU[64] | SR 12 (AB) c has a mass of 0.013±0.007 M☉ at a projected separation of ≈1100 AU.[64]

FW Tauri b orbits at a projected separation of 330±30 AU around a ≈11 AU separated binary.[67] It was shown to be more likely a 0.1 M☉ star surrounded by a protoplanetary disk than a planetary-mass companion.[68]

Largest orbit around three stars  | Gliese 900 b (CW2335+0142)  | Gliese 900 | 12,000 AU[53][5] |
Closest orbit between stars with a planet orbiting one of the stars  | Nu Octantis Ab | Nu Octantis | 2.629 AU[69] | Nu Octantis Ab's semi-major axis is 1.276 AU.
Smallest semi-major axis ratio between consecutive planets  | Kepler-36b and Kepler-36c | Kepler-36 | 11%  | Kepler-36b and c have semi-major axes of 0.1153 AU and 0.1283 AU, respectively, c is 11% further from star than b.

## Stellar characteristics

[edit]

Title  | Planet  | Star  | Data  | Notes

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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[5] | BD+20°2457 may be the lowest-metallicity planet host ([Fe/H]=−1.00); however, the proposed planetary system is dynamically unstable.[70]

Planets were announced around even the extremely low-metallicity stars HIP 13044 and HIP 11952; however, these claims have since been disproven.[71]

A brown dwarf or massive planetary companion was announced around the population II star HE 1523-0901, whose metallicity is −2.65±0.22 dex.[72] 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.[73]

Highest stellar mass  | Mu2 Scorpii b | Pipirima | 9.1±0.3 M☉[74] | M51-ULS-1b, listed as a candidate planet with 4 sigma confidence, may be the planet with the highest-mass host star.[75] 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[76] 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☉[59] | The mass of this star is near to the hydrogen burning limit.

KMT-2016-BLG-2142L have a lower mass, of 0.073+0.117
−0.04 M☉, but the value is highly uncertain.[59]

Lowest stellar mass (brown dwarf)  | 2MASS J1119-1137 B  | 2MASS J1119–1137 A  | 0.0033 M☉ | The system 2MASS J1119-1137 AB is a pair of binary rogue planets approximately 3.7 MJup each.[77]
Largest stellar radius  | HD 208527 b | HD 208527 | 51.1±8.3 R☉[5] | Other stars, such as HD 18438, Mirach and Delta Virginis are larger, but their substellar companions are more massive than the deuterium burning limit (13 MJ), and thus might be brown dwarfs rather than exoplanets.[5]

R Leonis (320-350 R☉)[78] has a candidate planet. It is a Mira variable. R Fornacis (585 R☉),[e] another Mira variable, also has a candidate planet.[79][80]

The stars R126 and R66 in the Large Magellanic Cloud have radius of 78 R☉ and 131 R☉[81] and have dust discs but no planets have been detected yet.

Smallest stellar radius (main sequence star)  | TRAPPIST-1 planets  | TRAPPIST-1 | 0.1192±0.0013 R☉[82] | VB 10 (0.102 R☉)[83] has a disproven planet candidate.
Smallest stellar radius (brown dwarf)  | 2M 0746+20 b[84] | 2M 0746+20 | 0.089 (± 0.003) R☉ | Planet's mass is very uncertain at 30.0 (± 25.0) MJup.
Smallest stellar radius (stellar remnant)  | PSR B0943+10 b and c; Draugr, Poltergeist and Phobetor | PSR B0943+10 and Lich | 0.000007187 R☉ (5 km)[85][86][f] | Both stars (PSR B0943+10 and PSR B1257+12) have almost the same size.

PSR B0943+10 may be a quark star. If so, its radius is predicted to be 2.6 km.[85]

Highest stellar luminosity | Beta Cancri b | Beta Cancri | 794 L☉[59] | This is the most luminous star to host a planet that is not a potential brown dwarf.[59]

The star Mirfak, whose luminosity is 3780 L☉,[87] 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.[13] R Leonis (at 3537 L☉)[78] has a candidate planet. R Fornacis (at 5800 L☉)[79] also has a candidate planet. The stars R126 and R66 in the Large Magellanic Cloud have luminosity of 1400000 L☉ and 320000 L☉[81] 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☉ | [88][59]
Hottest star with a planet  | NSVS 14256825 b | NSVS 14256825 | 40,000 K[89] | NN Serpentis is hotter, with a temperature of 57,000 K,[5] but the existence of its planets is disputed.[90]
Hottest normal star with a planet[g] | b Centauri b | b Centauri | 18,310±320 K[91] | V921 Scorpii b orbits a hotter star, at 30,000 K. Its host star is a 20-solar-mass B0IV-class subgiant.[92] 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 | 2,511 K  | Technically Oph 162225-240515, CFBDSIR 1458+10 and WISE 1217+1626 are cooler, but are classified as brown dwarfs.

## System characteristics

[edit]

Title  | System(s)  | Planet(s)  | Star(s)  | Notes

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System with most planets  | Kepler-90 | 8  | 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.[93] The four planets Tau Ceti e, f, g and h are considered as strong candidates.[94]

HD 10180 has six confirmed planets and potentially three more planets.[95]

System with most planets in habitable zone  | TRAPPIST-1 | 7  | 1  | Four planets in this system (d, e, f and g) orbit within the habitable zone.[96]
System with most stars  | Kepler-64 | PH1b (Kepler-64b)  | 4  | PH1b 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.[97] The quintuple star system GG Tauri has several protoplanetary disks but no planets have been detected yet.[98]

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)  | TYC 8998-760-1 | b, c | 1  | TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.[5]
Multiplanetary system with smallest range of semi-major axis (smallest difference between the star's nearest planet and its farthest planet)  | Kepler-429 | b, c, d | 1  | Kepler-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 8998-760-1 | b, c | 1  | TYC 8998-760-1 b and c have a semi-major axis of 162 and 320 AU, respectively.[5] The separation between closest and furthest is 158 AU.
System with smallest total planetary mass  | Kepler-444 | b, c, d, e, f  | 3  | The 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 mass  | Nu Ophiuchi | b, c  | 1  | Nu Ophiuchi b and c have masses of 22.206 and 24.662 Jupiter masses, respectively.[5] They may be brown dwarfs.
Multiplanetary system with smallest mean planetary mass  | Kepler-444 | b, c, d, e, f  | 3  | The 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 largest mean planetary mass  | Nu Ophiuchi | b, c  | 1  | Nu Ophiuchi b and c have masses of 22.206 and 24.662 Jupiter masses, respectively.[5] They may be brown dwarfs.
Exo-multiplanetary system with smallest range in planetary mass, log scale (smallest proportional difference between the most and least massive planets)  | Teegarden's Star | b, c  | 1  | Teegarden 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-37 | b, d | 1  | Mercury and Jupiter have a mass ratio of 5,750 to 1. Kepler-37 d and b may have a mass ratio between 500 and 1,000, and Gliese 676 c and d have a mass ratio of 491.

## See also

[edit]

* Extremes on Earth
* Lists of exoplanets
* List of exoplanet firsts
* List of stars with proplyds
* Methods of detecting exoplanets
* List of potentially habitable exoplanets

## Notes and references

[edit]

1. ^ "HEC: Top 10 Exoplanets". University of Puerto Rico at Arecibo. 5 December 2015. Archived from the original on 17 December 2013. Retrieved 1 August 2017.
2. ^ Gui, Yuqian; Zang, Weicheng; Zhai, Ruocheng; Ryu, Yoon-Hyun; Udalski, Andrzej; Yang, Hongjing; Han, Cheongho; Mao, Shude; Authors), (Leading; Albrow, Michael D.; Chung, Sun-Ju; Gould, Andrew; Hwang, Kyu-Ha; Jung, Youn Kil; Shin, In-Gu (July 2024). "Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets". The Astronomical Journal. 168 (2): 49. Bibcode:2024AJ....168...49G. doi:10.3847/1538-3881/ad4ce5. ISSN 1538-3881.
3. ^ "Exoplanet-catalog-Exoplanet exploration-Kepler-1606b".
4. ^ Specht, D.; et al. (2023). "Kepler K2Campaign 9 – II. First space-based discovery of an exoplanet using microlensing". Monthly Notices of the Royal Astronomical Society. 520 (4): 6350–6366. arXiv:2203.16959. doi:10.1093/mnras/stad212.
5. ^ a b c d e f g h i j k l m n o p q r s t u v "Planetary Systems Composite Data". NASA Exoplanet Archive. Retrieved 12 December 2021.
6. ^ Gratton, R.; et al. (June 2020). "Searching for the near-infrared counterpart of Proxima c using multi-epoch high-contrast SPHERE data at VLT". Astronomy & Astrophysics. 638: A120. arXiv:2004.06685. Bibcode:2020A&A...638A.120G. doi:10.1051/0004-6361/202037594. S2CID 215754278.
7. ^ "NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega" (Press release). Whitney Clavin, NASA. 8 January 2013. Retrieved 4 March 2013.
8. ^ Hurt, Spencer A.; Quinn, Samuel N.; Latham, David W.; Vanderburg, Andrew; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry; Angus, Ruth; Latham, Christian A.; Zhou, George (21 January 2021). "A Decade of Radial-velocity Monitoring of Vega and New Limits on the Presence of Planets". The Astronomical Journal. 161 (4): 157. arXiv:2101.08801. Bibcode:2021AJ....161..157H. doi:10.3847/1538-3881/abdec8. S2CID 231693198.
9. ^ Reichert, Katja (25 March 2019). "Precise radial velocities of giant stars XII. Evidence against the proposed planet Aldebaran b". Astronomy & Astrophysics. A22: 625. arXiv:1903.09157. Bibcode:2019A&A...625A..22R. doi:10.1051/0004-6361/201834028. S2CID 85459692.
10. ^ Ducati, J. R. (2002), "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system", CDS/ADC Collection of Electronic Catalogues, 2237: 0, Bibcode:2002yCat.2237....0D, doi:10.26093/cds/vizier, VizieR Cat. II/237/colors.
11. ^ Aurière, Michel; Konstantinova-Antova, Renada; et al. (August 2014). "Pollux: a stable weak dipolar magnetic field but no planet?". Proceedings of the International Astronomical Union. Magnetic Fields throughout Stellar Evolution. Vol. 302\. pp. 359–362. arXiv:1310.6907. Bibcode:2014IAUS..302..359A. doi:10.1017/S1743921314002476.
12. ^ Aurière, M.; Petit, P.; et al. (February 2021). "Pollux: A weak dynamo-driven dipolar magnetic field and implications for its probable planet". Astronomy & Astrophysics. 646: A130. arXiv:2101.02016. Bibcode:2021A&A...646A.130A. doi:10.1051/0004-6361/202039573.
13. ^ a b Lee, B. -C; Han, I.; Park, M. -G.; Kim, K. -M.; Mkrtichian, D. E. (2012). "Detection of the 128-day radial velocity variations in the supergiant α Persei. Rotational modulations, pulsations, or a planet?". Astronomy and Astrophysics. 543: A37. arXiv:1205.3840. Bibcode:2012A&A...543A..37L. doi:10.1051/0004-6361/201118539. S2CID 118482287.
14. ^ Ygouf, Marie; Beichman, Charles; et al. (October 2023). "Searching for Planets Orbiting Fomalhaut with JWST/NIRCam". The Astronomical Journal. 167 (1): 26. arXiv:2310.15028. Bibcode:2024AJ....167...26Y. doi:10.3847/1538-3881/ad08c8.
15. ^ a b "The Extrasolar Planet Encyclopaedia — Catalog Listing". Extrasolar Planets Encyclopaedia. 11 January 1995. Retrieved 4 May 2019.
16. ^ Khandelwal, Akanksha; Sharma, Rishikesh; Chakraborty, Abhijit; Chaturvedi, Priyanka; Ulmer-Moll, Solène; Ciardi, David R.; Boyle, Andrew W.; Baliwal, Sanjay; Bieryla, Allyson; Latham, David W.; Prasad, Neelam J. S. S. V.; Nayak, Ashirbad; Lendl, Monika; Mordasini, Christoph (1 April 2023). "Discovery of a massive giant planet with extreme density around the sub-giant star TOI-4603". Astronomy & Astrophysics. 672: L7. arXiv:2303.11841. Bibcode:2023A&A...672L...7K. doi:10.1051/0004-6361/202245608. ISSN 0004-6361.
17. ^ Lecavelier des Etangs, A.; Lissauer, Jack J. (June 2022). "The IAU working definition of an exoplanet". New Astronomy Reviews. 94: 101641. arXiv:2203.09520. Bibcode:2022NewAR..9401641L. doi:10.1016/j.newar.2022.101641. IAU website link
18. ^ Kirkpatrick, J. Davy; Marocco, Federico; et al. (April 2024). "The Initial Mass Function Based on the Full-sky 20 pc Census of ∼3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series. 271 (2): 55. arXiv:2312.03639. Bibcode:2024ApJS..271...55K. doi:10.3847/1538-4365/ad24e2.
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1. ^ Gamma Leonis is mentioned to have a slightly higher magnitude (1.99), but it is the combined magnitude of the system and not of the planet-hosting star. The true apparent magnitude is 2.37.
2. ^ The deuterium burning limit also depends on the metallicity and abundance of helium. Metal-rich planets, for example, need a lower mass to fuse deuterium.
3. ^ Based on the estimated temperature and luminosity.
4. ^ This is the calculated equilibrium temperature, assuming an albedo of 0.3
5. ^ Determined using angular diameter and distance.
0.008 milliarcseconds * 680 pc = diameter of 5.44 au.
6. ^ This is the radius
7. ^ A normal star is a star that is past its protostar period, in its main fusion period, before becoming a degenerate star, black hole, or post-stellar nebula, and is not a brown dwarf

## External links

[edit]

* WiredScience, Top 5 Most Extreme Exoplanets, Clara Moskowitz, 21 January 2009

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Exoplanets

* Planet
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Main topics|

* Exoplanet
* Exoplanet orbital and physical parameters
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Sizes
and
types|

| Terrestrial|

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Gaseous|

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Other types|

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Other|

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Portals:

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