List of exoplanet extremes

Short description: none

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.

## Contents

* 1 Extremes from Earth's viewpoint
* 2 Planetary characteristics
* 3 Orbital characteristics
* 4 Stellar characteristics
* 5 System characteristics
* 6 See also
* 7 References
* 8 External links

## Extremes from Earth's viewpoint

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.

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

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[4] | The disputed planet candidate CVSO 30 c may be more distant, at 1,200 light-years.
Closest directly visible  | COCONUTS-2b | COCONUTS-2  | 35.5 light-years[4] | WISE 1217+1626 B is closer, but is generally considered a brown dwarf. Proxima Centauri c (confirmed in 2020 using archival Hubble data from 1995+) may have been directly imaged.[5]
Star with the brightest apparent magnitude with a planet  | Pollux b | Pollux[6] | Apparent magnitude is 1.14  | Aldebaran (apparent magnitude 0.75–0.95) has a disputed 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), a candidate planet around Vega has been detected.[8]
Star with the faintest apparent magnitude with a planet  | MOA-bin-29Lb  | MOA-bin-29L  | Apparent magnitude is 44.61[4] |
Largest angular distance separation from its host star  | COCONUTS-2b | COCONUTS-2  | 594 arcseconds[9] |

## Planetary characteristics

Title  | Planet  | Star  | Data  | Notes

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Least massive  | PSR B1257+12 b | PSR B1257+12 | 0.020±0.002 M⊕[4] | The extrasolar planetesimal WD 1145+017 b is less massive, at 0.00067 M⊕.[9]
Most massive | The candidate for the most massive planet is contentious, as it is difficult to distinguish between a highly massive planet and a brown dwarf (the border between them approximately from 13 to 80 MJ). So it is estimated the largest planets are approximately a dozen Jupiter masses.
Largest radius | TYC 8998-760-1 b | TYC 8998-760-1 | 3.0 [[Astronomy:Jupiter radius | J}}}}}}]][9]
Smallest radius | Kepler-37b | Kepler-37 | 0.296±0.037 R⊕[4] | The extrasolar planetesimals SDSS J1228+1040 b[10] and WD 1145+017 b are smaller.
Most dense  | Kepler-131c  | Kepler-131  | 77.7+55
−55 g/cm3[11] | Highly uncertain
Least dense  | Kepler-51c, b and/or possibly d[12] | Kepler-51[12] | ~ 0.03 g/cm3[12] | The 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.[12]
Hottest  | KELT-9b | KELT-9  | 4,050±180 K[4] | The disputed planet candidate Kepler-70b may be hotter, at >7,000 K.[13]
Coldest  |  OGLE-2016-BLG-1195Lb |  OGLE-2016-BLG-1195L  | 31 K |
Highest albedo | Kepler-1658b | Kepler-1658  | 0.758[14] (geometric albedo)  |
Lowest albedo  | TrES-2b | GSC 03549-02811 | Geometric albedo < 1%[15] | Best-fit model for albedo gives 0.04% (0.0004).[13]
Youngest  | Proplyd 133-353  | Proplyd 133-353  | The upper mass limit (13 Jupiter masses) may make this a brown dwarf.
Oldest  | WASP-183b  | WASP-183  | 14.9±1.7 Gyr[4] | The estimated age of the universe is 13.8 billion years, within the margin of error. The disputed Kapteyn b is the oldest potentially habitable exoplanet at 11 Gyr.[16]

## Orbital characteristics

Title  | Planet  | Star  | Data  | Notes

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Longest orbital period
(Longest year) | COCONUTS-2b | COCONUTS-2  | 1.1 million years[17] | 2MASS J2126–8140 previously held this record at ~900,000 years.
Shortest orbital period
(Shortest year) | SWIFT J1756.9-2508 b | SWIFT J1756.9-2508 | 48 minutes, 56.5 seconds[18] | K2-137b has the shortest orbit around a main-sequence star (an M dwarf) at 4.31 hours.[19]
Most eccentric orbit | HD 20782 b[20] | HD 20782 | 0.956±0.004 | [21] Record among confirmed planets. The disproven planet candidate at VB 10 was thought to have a higher eccentricity of 0.98.[22]
Largest orbit around a single star  | COCONUTS-2b | COCONUTS-2  | 7,506+5,205
−2,060 astronomical unit|AU[4] | Projected separation of 6,471 AU.[17] Next largest are 2MASS J2126–8140 with 6,900 AU and HD 106906 b[23] with ~738 AU.
Smallest orbit  | WD 1202-024 B | WD 1202-024 | 0.0021 AU
Smallest orbit around binary star  | Kepler-47b | Kepler-47AB | 0.2877+0.0014
−0.0011 astronomical unit|AU[4] | [24]
Smallest ratio of semi-major axis of a planet orbit to binary star orbit  | Kepler-16b | Kepler-16AB | 3.14 ± 0.01  | [25]
Largest orbit around binary star  | DT Virginis c | DT Virginis | 1,168 AU  | Star system is also known as Ross 458 AB. The planet was eventually confirmed to be below deuterium burning limit but its formation origin is unknown.
Largest orbit around a single star in a multiple star system  | ROXs 12 b | ROXs 12 | 210±20 astronomical unit|AU[4] |
Largest distance between binary stars with a circumbinary planet  | FW Tauri b  | FW Tauri AB  | ≈11 AU  | FW Tauri AB b orbits at a distance of 150–300 AU.[26]
Closest orbit between stars with a planet orbiting one of the stars  | OGLE-2013-BLG-0341LBb | OGLE-2013-BLG-0341LB | ~12–17 AU
(10 or 14 AU projected distance)[27] | OGLE-2013-BLG-0341L b's semi-major axis is 0.7 AU.[27]
Smallest semi-major-axis difference between consecutive planets  | Kepler-70b and Kepler-70c[13] | Kepler-70 | 0.0016 AU (240,000 km)  | During closest approach, Kepler-70c would appear 5 times the size of the Moon in Kepler-70b's sky.[needs update]
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

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[4] | BD+20°2457 may be the lowest-metallicity planet host ([Fe/H]=−1.00); however, the proposed planetary system is dynamically unstable.[28] Kapteyn's Star may also be the lowest-metallicity planet host ([Fe/H]=−0.99±0.04), but its planets are most likely artifacts of stellar activity and rotation.[29]

Planets were announced around even the extremely low-metallicity stars HIP 13044 and HIP 11952; however, these claims have since been disproven.[30]

Highest stellar mass  | Mu2 Scorpii b | Mu2 Scorpii | 9.1±0.3 M☉[31] | M51-ULS-1b, listed as a candidate planet with 4 sigma confidence, may be the planet with the highest-mass host star. The host is a massive O-class supergiant and a black hole orbiting each other at 0.8 AU, with a combined system mass of >60 solar masses. The planet is a Saturn-sized (0.72 Jupiter radii) object orbiting the black-hole/supergiant binary at 10 AU. The host stars giving off a combined 1 million solar luminosities, the planet receives the equivalent irradiation of 51 Pegasi b, which orbits its star at 0.045 AU. M51-ULS-1b would also be one of the youngest planets ever discovered, with a system age of <10 million years according to evolutionary models.[32]

Because M51-ULS-1b requires further confirmation, the object V921 Sco b, a 60-Jupiter-mass object orbiting a 20-solar-mass 30,000 K Herbig Haro B0IV-class subgiant at 835 AU, may actually be the record holder. Despite the large distance, V921 Sco b receives a comparable amount of irradiation as Mars, owing to the large mass and luminosity of the host star. At 20 solar masses, V921 Sco is the most massive object to host a substellar object. Normally, V921 Sco b would be considered a brown dwarf, but given the high mass of the host star, and the growing studies that confirm the correlation of more massive planets around more massive stars, this object could be considered a planet. Hatzes and Rauer quote an upper limit of 60 Jupiter masses for a core-accretion formation of high-mass gas giants, which is how heavy this object is. Furthermore, the Extrasolar Planets Encyclopedia lists objects up to 60 Jupiter masses as planets if they orbit stars.[33]

b Centauri has a mass of 6 solar masses.

The stars R126 and R66 in the Large Magellanic Cloud have masses of 70 and 30 solar masses and have dust discs but no planets have been detected yet.

Lowest stellar mass (main sequence)  | OGLE-2016-BLG-1195Lb | OGLE-2016-BLG-1195L  | 0.078+0.016
−0.012 M☉[4] | Could also be OGLE-2015-BLG-1771L, at 0.077+0.119
−0.044 M☉.[4]
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 Jupiter masses each.[34]
Largest stellar radius  | HD 240237 b | HD 240237 | 71.23±17.07 R☉[4] | HD 81817 is larger, at 83.8±7.8 R☉,[4] but its substellar companion is most likely a brown dwarf or red dwarf. R Leonis (299 or 320-350 R☉)[35][36] has a candidate planet. It is a Mira variable.
Smallest stellar radius (main sequence star)  | Teegarden's Star b and c | Teegarden's Star | 0.107±0.004 R☉[4] | VB 10 (0.102 R☉)[37] has a disproven planet candidate.
Smallest stellar radius (brown dwarf)  | 2M 0746+20 b[38] | 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[39][40][41] | PSR B0943+10 | 0.000003737 R☉[42] |
Oldest star  | WASP-183b  | WASP-183  | 14.9±1.7 Gyr[4] | The estimated age of the universe is 13.8 billion years, within the margin of error.
Hottest star with a planet  | NN Serpentis planets  | NN Serpentis | 57,000 K[4] |
Hottest main-sequence star with a planet  | b Centauri b | b Centauri | 18,310±320 K[43] | V921 Scorpii b orbits a hotter star, at 30,000 K. Its host star is a 20-solar-mass B0IV-class subgiant.[33] 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, but as the star is a supergiant, does not count as on the main sequence.

Coolest star with a planet  | TRAPPIST-1b, c, d, e, f, g and h | 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

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

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System with most planets  | Kepler-90 | 8  | 1
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.[44]
System with most stars  | Kepler-64 | PH1b (Kepler-64b)  | 4  | PH1b has a circumbinary orbit.
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 only 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.[4]
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 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.

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.[4] 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.[4] 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.[4] 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

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

## References

1. ↑ "HEC: Top 10 Exoplanets". University of Puerto Rico at Arecibo. 5 December 2015. http://phl.upr.edu/projects/habitable-exoplanets-catalog/top10.
2. ↑ "Exoplanet-catalog-Exoplanet exploration-Kepler-1606b". https://exoplanets.nasa.gov/exoplanet-catalog/2252/kepler-1606-b/.
3. ↑ Specht, D. (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. doi:10.1093/mnras/stad212.
4. ↑ 4.00 4.01 4.02 4.03 4.04 4.05 4.06 4.07 4.08 4.09 4.10 4.11 4.12 4.13 4.14 4.15 4.16 4.17 4.18 4.19 4.20 4.21 "Planetary Systems Composite Data". https://exoplanetarchive.ipac.caltech.edu/cgi-bin/TblView/nph-tblView?app=ExoTbls&config=PSCompPars.
5. ↑ Gratton, R. (June 2020). "Searching for the near-infrared counterpart of Proxima c using multi-epoch high-contrast SPHERE data at VLT". Astronomy & Astrophysics 638: A120. doi:10.1051/0004-6361/202037594. Bibcode: 2020A&A...638A.120G.
6. ↑ Lee, T. A. (October 1970), "Photometry of high-luminosity M-type stars", The Astrophysical Journal 162: 217, doi:10.1086/150648, Bibcode: 1970ApJ...162..217L
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 et al. (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. doi:10.3847/1538-3881/abdec8. Bibcode: 2021AJ....161..157H.
9. ↑ 9.0 9.1 9.2 "The Extrasolar Planet Encyclopaedia — Catalog Listing". http://exoplanet.eu/catalog/.
10. ↑ "Planet SDSS J1228+1040 b". http://exoplanet.eu/catalog/sdss_j1228+1040_b/.
11. ↑ Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew W.; Rowe, Jason F.; Jenkins, Jon M.; Bryson, Stephen T.; Latham, David W.; Howell, Steve B. et al. (2014-01-13). "Masses, Radii, and Orbits of Small Kepler Planets: The Transition from Gaseous to Rocky Planets". The Astrophysical Journal Supplement Series 210 (2): 20. doi:10.1088/0067-0049/210/2/20. ISSN 0067-0049. Bibcode: 2014ApJS..210...20M.
12. ↑ 12.0 12.1 12.2 12.3 Very Low-Density Planets around Kepler-51 Revealed with Transit Timing Variations and an Anomaly Similar to a Planet-Planet Eclipse Event: Kento Masuda
13. ↑ 13.0 13.1 13.2 Charpinet, S. et al. (21 December 2011). "A compact system of small planets around a former red-giant star". Nature 480 (7378): 496–499. doi:10.1038/nature10631. ISSN 1476-4687. PMID 22193103. Bibcode: 2011Natur.480..496C.
14. ↑ "The Extrasolar Planet Encyclopaedia — Kepler-1658 b". http://exoplanet.eu/catalog/kepler-1658_b/.
15. ↑ David M. Kipping (2011). "Detection of visible light from the darkest world". Monthly Notices of the Royal Astronomical Society 417 (1): L88–L92. doi:10.1111/j.1745-3933.2011.01127.x. Bibcode: 2011MNRAS.417L..88K. http://www.astro.princeton.edu/~dsp/PrincetonSite/Home_files/darkest_world.pdf. Retrieved 2011-08-12.
16. ↑ "Introducing Earth's bigger, older brother: planet Kapteyn b". 14 June 2014. https://phys.org/news/2014-06-earth-bigger-older-brother-planet.html.
17. ↑ 17.0 17.1 Zhang, Zhoujian; Liu, Michael C.; Claytor, Zachary R.; Best, William M. J.; Dupuy, Trent J.; Siverd, Robert J. (2021). "The Second Discovery from the COCONUTS Program: A Cold Wide-orbit Exoplanet around a Young Field M Dwarf at 10.9 pc". The Astrophysical Journal Letters 916 (2): L11. doi:10.3847/2041-8213/ac1123. Bibcode: 2021ApJ...916L..11Z.
18. ↑ "The Extrasolar Planet Encyclopaedia — SWIFT J1756-2508". http://exoplanet.eu/catalog/swift_j1756-2508/.
19. ↑ "The Extrasolar Planet Encyclopaedia — K2-137 b.". 2018. http://exoplanet.eu/catalog/k2-137_b/.
20. ↑ "HD 20781 b". http://www.openexoplanetcatalogue.com/system.html?id=HD+20781+b.
21. ↑ "The Extrasolar Planet Encyclopaedia — HD 20782 b". http://exoplanet.eu/catalog/hd_20782_b/.
22. ↑ "The Extrasolar Planet Encyclopaedia — VB 10 b". http://exoplanet.eu/catalog/vb_10_b/.
23. ↑ De Rosa, Robert J.; Kalas, Paul (February 2019). "A Near-coplanar Stellar Flyby of the Planet Host Star HD 106906". The Astronomical Journal 157 (3): 125. doi:10.3847/1538-3881/ab0109. Bibcode: 2019AJ....157..125D.
24. ↑ Orosz, J. et al. (2012). "Kepler-47: A Transiting Circumbinary Multi-Planet System". Science 337 (6101): 1511–4. doi:10.1126/science.1228380. PMID 22933522. Bibcode: 2012Sci...337.1511O.
25. ↑ Laurance R. Doyle et al. (2011). "Kepler-16: A Transiting Circumbinary Planet". Science 333 (6049): 1602–1606. doi:10.1126/science.1210923. PMID 21921192. Bibcode: 2011Sci...333.1602D.
26. ↑ Kraus, Adam; J. Ireland, Michael; A. Cieza, Lucas; Hinkley, Sasha; J. Dupuy, Trent; P. Bowler, Brendan; C. Liu, Michael (2 January 2014). "Three Wide Planetary-Mass Companions to FW Tau, ROXs 12, and ROXs 42B". The Astrophysical Journal 781 (1): 1311. doi:10.1088/0004-637X/781/1/20. Bibcode: 2014ApJ...781...20K.
27. ↑ 27.0 27.1 Gould, A. et al. (3 July 2014). "A terrestrial planet in a ~1-AU orbit around one member of a 15-AU binary". Science 345 (6192): 46–49. doi:10.1126/science.1251527. ISSN 0036-8075. PMID 24994642. Bibcode: 2014Sci...345...46G. "these projected separations are good proxies for the semi-major axis (afterupward adjustment by [math]\displaystyle{ \sqrt{3/2} }[/math] to correct for projection effects)".
28. ↑ Horner, J.; Wittenmyer, R. A.; Hinse, T. C.; Marshall, J. P. (2014). "A dynamical investigation of the proposed BD +20 2457 system". Monthly Notices of the Royal Astronomical Society 439 (1): 1176. doi:10.1093/mnras/stu081. Bibcode: 2014MNRAS.439.1176H.
29. ↑ Bortle, Anna et al. (2021). "A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star". The Astronomical Journal 161 (5): 230. doi:10.3847/1538-3881/abec89. Bibcode: 2021AJ....161..230B.
30. ↑ Jones, M. I.; Jenkins, J. S. (2014). "No evidence of the planet orbiting the extremely metal-poor extragalactic star HIP 13044". Astronomy and Astrophysics 562: A129. doi:10.1051/0004-6361/201322132. Bibcode: 2014A&A...562A.129J.
31. ↑ "Notes for mu2 scorpii". The Extrasolar Planets Encyclopaedia. http://exoplanet.eu/catalog/mu2_sco_b/. Retrieved 2022-05-06.
32. ↑ "Notes for planet M51-ULS-1b". The Extrasolar Planets Encyclopaedia. http://exoplanet.eu/catalog/m51-uls-1_b/. Retrieved 2021-07-18.
33. ↑ 33.0 33.1 "V921Sco b". The Extrasolar Planets Encyclopaedia. http://exoplanet.eu/catalog/v_921_sco_b/. Retrieved 2021-07-18.
34. ↑ "Notes for planet 2MASSS J1119-1137 AB". The Extrasolar Planets Encyclopaedia. http://exoplanet.eu/catalog/2mass_j11193254_ab/. Retrieved 2017-08-29.
35. ↑ De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics 523: A18. doi:10.1051/0004-6361/200913771. Bibcode: 2010A&A...523A..18D.
36. ↑ Fedele (2005). "The K -Band Intensity Profile of R Leonis Probed by VLTI/VINCI". Astronomy & Astrophysics 431 (3): 1019–1026. doi:10.1051/0004-6361:20042013. Bibcode: 2005A&A...431.1019F.
37. ↑ Linsky, Jeffrey L.; Wood, Brian E.; Brown, Alexander; Giampapa, Mark S.; Ambruster, Carol (December 1995). "Stellar Activity at the End of the Main Sequence: GHRS Observations of the M8 Ve Star VB 10". The Astrophysical Journal 455: 670. doi:10.1086/176614. ISSN 0004-637X. Bibcode: 1995ApJ...455..670L.
38. ↑ "The Extrasolar Planet Encyclopaedia — 2M 0746+20 b". exoplanet.eu. http://exoplanet.eu/catalog/2m_0746+20_b/.
39. ↑ Suleymanova, S. A.; Rodin, A. E. (2014-11-01). "Detection of regular variations in the intensity and pulse time of arrival of the anomalous pulsar PSR B0943+10" (in en). Astronomy Reports 58 (11): 796–807. doi:10.1134/S1063772914110067. ISSN 1562-6881. Bibcode: 2014ARep...58..796S. https://doi.org/10.1134/S1063772914110067.
40. ↑ "The Extrasolar Planet Encyclopaedia — PSR B0943+10 c". http://exoplanet.eu/catalog/psr_b0943+10_c/.
41. ↑ "The Extrasolar Planet Encyclopaedia — PSR B0943+10 b". http://exoplanet.eu/catalog/psr_b0943+10_b/.
42. ↑ Yue, Y. L.; Cui, X. H.; Xu, R. X. (2006-10-01). "Is PSR B0943+10 a low-mass quark star?". The Astrophysical Journal 649 (2): L95–L98. doi:10.1086/508421. ISSN 0004-637X. Bibcode: 2006ApJ...649L..95Y.
43. ↑ Janson, Markus; Gratton, Raffaele; Rodet, Laetitia; Vigan, Arthur; Bonnefoy, Mickaël; Delorme, Philippe; Mamajek, Eric E.; Reffert, Sabine et al. (2021). "A wide-orbit giant planet in the high-mass b Centauri binary system". Nature 600 (7888): 231–234. doi:10.1038/s41586-021-04124-8. PMID 34880428. Bibcode: 2021Natur.600..231J.
44. ↑ "NASA telescope reveals largest batch of Earth-size, habitable-zone planets around single star". Exoplanet Exploration: Planets Beyond our Solar System. nasa.gov. 21 February 2017. https://exoplanets.nasa.gov/news/1419/nasa-telescope-reveals-largest-batch-of-earth-size-habitable-zone-planets-around-single-star/.

## External links

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

* v
* t
* e

Exoplanetology

* Planet
* Definition
* IAU
* Planetary science

Main topics|

* Exoplanet
* Methods of detecting exoplanets
* Planetary system

Sizes
and types|

| Terrestrial|

* Carbon planet
* Coreless planet
* Desert planet
* Dwarf planet
* Ice planet
* Iron planet
* Lava planet
* Mega-Earth
* Ocean planet
* Sub-Earth
* Super-Earth

|

Gaseous|

* Eccentric Jupiter
* Gas dwarf
* Helium planet
* Hot Jupiter
* Hot Neptune
* Ice giant
* Mini-Neptune
* Super-Neptune
* Super-Jupiter

Other types|

* Brown dwarf
* Chthonian planet
* Circumbinary planet
* Disrupted planet
* Double planet
* Eyeball planet
* Mesoplanet
* Planemo
* Planet/Brown dwarf boundary
* Planetesimal
* Protoplanet
* Pulsar planet
* Sub-brown dwarf
* Ultra-cool dwarf
* Ultra-short period planets (USP)

Formation
and evolution|

* Accretion
* Accretion disk
* Asteroid belt
* Circumplanetary disk
* Circumstellar disc
* Circumstellar envelope
* Cosmic dust
* Debris disk
* Detached object
* Disrupted planet
* Excretion disk
* Exoplanetary Circumstellar Environments and Disk Explorer
* Exozodiacal dust
* Extraterrestrial materials
* Extraterrestrial sample curation
* Giant-impact hypothesis
* Gravitational collapse
* Hills cloud
* Interplanetary dust cloud
* Interplanetary medium
* Interplanetary space
* Interstellar cloud
* Interstellar dust
* Interstellar medium
* Interstellar space
* Kuiper belt
* List of interstellar and circumstellar molecules
* Merging stars
* Molecular cloud
* Nebular hypothesis
* Oort cloud
* Outer space
* Planetary migration
* Planetary system
* Planetesimal
* Planet formation
* Protoplanetary disk
* Ring system
* Rubble pile
* Sample-return mission
* Scattered disc
* Star formation

Systems|

* Exocomet
* Exomoon
* Interstellar comet
* Mean-motion resonances
* Retrograde planet
* Rogue planet
* Tidally detached exomoon
* Titius–Bode laws
* Trojan planet

Host stars|

* A
* B
* Binary star
* Brown dwarfs
* Extragalactic planet
* F/Yellow-white dwarfs
* G/Yellow dwarfs
* Herbig Ae/Be
* K/Orange dwarfs
* M/Red dwarfs
* Planets in globular clusters
* Pulsar
* Red giant
* Subdwarf B
* Subgiant
* T Tauri
* White dwarfs
* Yellow giants

Detection|

* Astrometry
* Direct imaging
* list
* Microlensing
* list
* Polarimetry
* Pulsar timing
* list
* Radial velocity
* list
* Transit method
* list
* Transit-timing variation

Habitability|

* Astrobiology
* Circumstellar habitable zone
* Earth analog
* Extraterrestrial liquid water
* Habitability of natural satellites
* Superhabitable planet

Catalogues|

* Catalog of Nearby Habitable Systems
* Exoplanet Data Explorer
* Extrasolar Planets Encyclopaedia
* NASA Exoplanet Archive
* NASA Star and Exoplanet Database

Lists|

* Exoplanetary systems
* Host stars
* Multiplanetary systems
* Stars with proplyds
* Exoplanets
* Lists of exoplanets
* Discoveries
* Extremes
* Firsts
* Nearest
* Largest
* Most massive
* Terrestrial candidates
* Kepler
* Potentially habitable
* Discovered exoplanets by year
* before 2000
* 2000–2009
* 2010
* 2011
* 2012
* 2013
* 2014
* 2015
* 2016
* 2017
* 2018
* 2019

Other|

* Carl Sagan Institute
* Exoplanet phase curves
* Nexus for Exoplanet System Science
* Planets in science fiction
* Sudarsky's gas giant classification

* Discoveries of exoplanets
* Search projects

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