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.
Extremes from Earth's viewpoint
Title | Planet | Star | Data | Notes |
---|---|---|---|---|
Most distant | SWEEPS-11 / SWEEPS-04 | – | 27,710 light years.[1] | An analysis of the lightcurve of the microlensing event PA-99-N2 suggests the presence of a planet orbiting a star in the Andromeda Galaxy (2.54 ± 0.11 Mly).[2] |
Least distant | Proxima Centauri b | Proxima Centauri | 4.22 light years | Also the closest rocky exoplanet, and closest potentially habitable exoplanet known. |
Star with the brightest apparent magnitude with a planet | Pollux b | Pollux[3] | Apparent magnitude is 1.14 | The evidence of planets around Vega with an apparent magnitude of 0.03 is strongly suggested by circumstellar disks surrounding it. As of 2013[update], no planets had yet been confirmed.[4] |
Largest angular distance separation from its host star | GU Piscium b | GU Piscium | 42 arc seconds[5] | WD 0806-661 b has an angular separation of 130.2 arc seconds from WD 0806-661. However, its planetary origin is unknown. |
Planetary characteristics
Title | Planet | Star | Data | Notes |
---|---|---|---|---|
Most massive | DENIS-P J082303.1-491201 b[6] | DENIS-P J082303.1-491201[7] | 28.5±1.9 Jupiter masses[8] | Most massive planet in the NASA Exoplanet Archive although, according to most definitions of planet, it may be too massive to be a planet, and may be a brown dwarf instead. It is part of an ultracool binary system.[6] |
Least massive | PSR B1257+12 A[9][10] | PSR B1257+12[9][10] | 0.02 MEarth[9][10] | Mass of PSR B1257+12 A is based on an assumption of coplanarity with the outer two planets. The least massive exoplanet for which a true mass is known is Gliese 581e with a mass of 2 MEarth.
Kepler-37b may be less massive (assuming Moon-like density), estimated mass >0.01 MEarth,[11] < 6 MEarth[12] |
Largest radius | HAT-P-32b[13] | HAT-P-32 | 2.04 Jupiter radii | CT Chamaeleontis b is slightly larger at 2.2 Jupiter radii, but may be a brown dwarf star. |
Smallest radius | Kepler-37b | Kepler-37 | 0.30 Earth radii | Slightly larger than the Moon. |
Most dense | PSR J1719-1438 b | PSR J1719-1438 | ≥23 g/cm3[14] | Pulsar planet; minimum density is inferred via Roche limit of the host star. |
Least dense | Kepler-453b[15] | Kepler-453 | 0–0.7 g/cm3[note 1] | The density of Kepler-453b has not been accurately measured, and it has a radius of 6.204 Re |
Hottest | Kepler-70b | Kepler-70 | 7143 K[17] | |
Coldest | OGLE-2005-BLG-390Lb | OGLE-2005-BLG-390L | 50 K | |
Highest albedo | Kepler-10b[citation needed] | Kepler-10 | 0.5–0.6 (geometric albedo) | |
Lowest albedo | TrES-2b | GSC 03549-02811 | Geometric albedo < 1%[18] | Best-fit model for albedo gives even 0.04% (0.0004)[18] |
Youngest | V830 Tau b | V830 Tau | 2 Myr | |
Oldest | PSR B1620-26 b | PSR B1620-26 | 13 Gyr | Orbits in a circumbinary orbit around two stellar remnants – a pulsar and a white dwarf |
Orbital characteristics
Title | Planet | Star | Data | Notes |
---|---|---|---|---|
Longest orbital period (Longest year) |
2MASS J2126-8140 | TYC 9486-927-1 | ~1,000,000 years | GU Piscium b previously held record at 163,000 years. |
Shortest orbital period (Shortest year) |
PSR J1719-1438 b[19] | PSR J1719-1438[20] | 0.092 days (2.2 hours)[19] | |
Most eccentric orbit | HD 20782 b[21] | HD 20782[21] | eccentricity of 0.97±0.01 | HD 80606 b has an orbital eccentricity of 0.9349,[22] previously held record |
Largest orbit around a single star[23][24] | HD 106906 b[23] | HD 106906[23] | ~650 AU[23] | |
Smallest orbit | PSR J1719-1438 b[25] | PSR J1719-1438 | 0.004 AU | |
Smallest orbit around binary star | Kepler-47b | Kepler-47AB | ≃0.3 AU | [26] |
Smallest ratio of semi-major axis of a planet orbit to binary star orbit | Kepler-16b | Kepler-16AB | 3.14 ± 0.01 | [27] |
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 | Fomalhaut b | Fomalhaut | 115 AU | The second stellar component of the system, TW Piscis Austrini, has a semi-major axis of 57,000 AU from Fomalhaut and the third stellar component, LP 876-10 orbits 158,000 AU away from Fomalhaut. |
Largest distance between binary stars with a circumbinary planet | FW Tauri AB b | FW Tau AB | ≈11 AU | [citation needed] |
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)[28] |
OGLE-2013-BLG-0341L b's semi-major axis is 0.7 AU.[29] |
Smallest semi-major axis difference between planets | Kepler-70b and Kepler-70c[30] | Kepler-70 | 0.0016 AU (about 240,000 km) | During closest approach, Kepler-70c would appear 5 times the size of the Moon in Kepler-70b's sky. |
Smallest semi-major axis ratio between 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 |
---|---|---|---|---|
Highest metallicity | HD 126614 Ab | HD 126614 A | +0.56 dex | Located in a triple star system. |
Lowest metallicity | Kepler-271b, c | Kepler-271 | −0.951 dex | BD+20°2457 may be the lowest metallicity planet host ([Fe/H]=−1.00), however the proposed planetary system is dynamically unstable. [2] The next lowest-metallicity system is Kepler-271. Planets were announced around even the extremely low metallicity stars HIP 13044 and HIP 11952, however these claims have since been disproven. [3] |
Highest stellar mass | HD 13189 b[31] | HD 13189[31] | 4.5±2.5 M☉[31] | Margin of error means the star Epsilon Tauri with a stellar mass of 2.723 M☉ is potentially the most massive known planet-harboring star.[32] |
Lowest stellar mass (main sequence) | TRAPPIST-1b, c, and d | TRAPPIST-1 | 0.08 M☉ | |
Lowest stellar mass (brown dwarf) | 2M J044144 b[33] | 2M J044144[33] | 0.02 M☉[33] | |
Largest stellar radius | HD 208527 b[34] | HD 208527 | 51.1 (± 8.3) R☉ | Star is a red giant. |
Smallest stellar radius (main sequence star) | Kepler-42 b[35] | Kepler-42 | 0.17 (± 0.05) R☉ | |
Smallest stellar radius (brown dwarf) | 2M 0746+20 b[36] | 2M 0746+20 | 0.089 (± 0.003) R☉ | Planet's mass is very uncertain at 30.0 (± 25.0) Mjup. |
Smallest stellar radius (pulsar) | PSR J1719-1438 b[37] | PSR J1719-1438 | 0.04 R☉ | |
Oldest star | HD 164922 b | HD 164922[38] | 13.4 billion years[38] | |
Hottest star with a planet | NY Virginis b | NY Virginis[39] | 33247 K | This star is a subdwarf B star and has a red dwarf companion of 0.14 solar masses with a semi-major axis of slightly under 4 million kilometers from the primary component. |
Hottest main-sequence star with a planet | Fomalhaut b | Fomalhaut[40] | 8590 K | HIP 78530 has a surface temperature of 10500K, but it is uncertain whether the orbiting companion is a brown dwarf or planet. |
System characteristics
Title | System | Planet(s) | Star(s) | Notes |
---|---|---|---|---|
System with most (confirmed) planets | HD 10180 | 9 | 1 | The planets are HD 10180b, c, ..., h. This system has 2 unconfirmed planets and more data is needed to confirm their existence.[41][42] |
System with most stars | Kepler 64 | PH1b (Kepler 64b) | 4 | PH1 has a circumbinary orbit. |
See also
- Extremes on Earth
- List of exoplanets
- List of stars with proplyds
- Methods of detecting exoplanets
- Terrestrial exoplanets
Notes
- ^ NASA does not give a direct density value, however both mass and radius values are given. Using the PHL density Calculator mass value of 0–30 Me and 6.204 Re were used and gave a result of 0–0.7 g/cm which may or may not be lower than Kepler-51d's density depending on the radius of Kepler-52d and the mass of Kepler-453b. The volume of Kepler-51d may be an order of magnitude smaller, or somewhat larger, than that of Jupiter, with possible densities between 10 and about 500 grams per liter.[16]
References
- ^ http://phl.upr.edu/projects/habitable-exoplanets-catalog/top10
- ^ Schneider, J. "Notes for star PA-99-N2". The Extrasolar Planets Encyclopaedia. Retrieved 6 August 2010.
- ^ Lee, T. A. (October 1970), "Photometry of high-luminosity M-type stars", Astrophysical Journal, 162: 217, Bibcode:1970ApJ...162..217L, doi:10.1086/150648
- ^ "NASA, ESA Telescopes Find Evidence for Asteroid Belt Around Vega" (Press release). Whitney Clavin, NASA. 8 January 2013. Retrieved 4 March 2013.
- ^ "GU Psc b". The Extrasolar Planet Encyclopaedia.
- ^ a b Sahlmann, J.; Lazorenko, P. F.; Ségransan, D.; Martín, E. L.; Queloz, D.; Mayor, M.; Udry, S. (August 2013). "Astrometric orbit of a low-mass companion to an ultracool dwarf". Astronomy & Astrophysics. arXiv:1306.3225. Bibcode:2013A&A...556A.133S. doi:10.1051/0004-6361/201321871.
- ^ Staff (8 March 2014). "DENIS-P J082303.1-491201". SIMBAD. Retrieved 8 March 2014.
- ^ Staff. "DENIS-P J082303.1-491201 b". Caltech. Retrieved 8 March 2014.
- ^ a b c New Scientist, "Smallest known exoplanet may actually be Earth-mass", Stephen Battersby, 19 January 2009 (accessed 5 August 2010)
- ^ a b c "Planets Around Pulsars", Alex Wolszczan (accessed 5 August 2010)
- ^ [NULL]. "Kepler: Discovery: Kepler-37b, a planet only slightly larger than the Moon". nasa.gov.
- ^ http://iopscience.iop.org/0067-0049/210/2/20/article; 2.78 ± 3.7 MEarth means 0 to 6 MEarth at 1 sigma
- ^ "HAT-P-32 b". The Extrasolar Planet Encyclopaedia.
- ^ Hirschler, Ben (25 August 2011). "Astronomers discover planet made of diamond". Reuters. Retrieved 12 January 2017.
- ^ "Kepler-453 b". caltech.edu.
- ^ HEC, Calculator (8 October 2015). "Exoplanet Calculator". PHL. Retrieved 8 October 2015.
- ^ "HEC Top 10 Lists of Exoplanets". Retrieved 11 November 2014.
- ^ a b David M. Kipping; et al. "Detection of visible light from the darkest world" (PDF). Monthly Notices of the Royal Astronomical Society. arXiv:1108.2297. Bibcode:2011MNRAS.417L..88K. doi:10.1111/j.1745-3933.2011.01127.x. Retrieved 12 August 2011.
- ^ a b http://mobile.reuters.com/article/idUSTRE77O69A20110825
- ^ koi-55-ex-pl-encyc>"Notes for star KOI-55". Extrasolar Planets Encyclopedia. Retrieved 1 January 2012.
- ^ a b [1], (accessed 29 May 2014)
- ^ ScienceDaily, "Students Find Jupiter-Sized Oddball Planet", 22 April 2009 (accessed 5 August 2010)
- ^ a b c d Chow, Denise (6 December 2013). "Giant Alien Planet Discovered in Most Distant Orbit Ever Seen". space.com. Retrieved 8 December 2013.
{{cite web}}
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(help) - ^ Bailey, Vanessa; et al. (January 2014). "HD 106906 b: A planetary-mass companion outside a massive debris disk". The Astrophysical Journal Letters. 780 (1). arXiv:1312.1265. Bibcode:2014ApJ...780L...4B. doi:10.1088/2041-8205/780/1/L4. L4.
- ^ Bailes, M.; Bates, S. D.; Bhalerao, V.; Bhat, N. D. R.; Burgay, M.; Burke-Spolaor, S.; d'Amico, N.; Johnston, S.; Keith, M. J.; et al. (2011). "Transformation of a Star into a Planet in a Millisecond Pulsar Binary" (PDF). Science. 333 (6050): 1717–20. arXiv:1108.5201. Bibcode:2011Sci...333.1717B. doi:10.1126/science.1208890. PMID 21868629.
- ^ OROSZ J.; WELSH W.; CARTER J.; FABRYCKY D.; COCHRAN W.; et al. (2012). "Kepler-47: A Transiting Circumbinary Multi-Planet System". Science. 337 (6101): 1511–4. arXiv:1208.5489. Bibcode:2012Sci...337.1511O. doi:10.1126/science.1228380. PMID 22933522.
- ^ Laurance R. Doyle; Joshua A. Carter; Daniel C. Fabrycky; Robert W. Slawson; Steve B. Howell; Joshua N. Winn; Jerome A. Orosz; Andrej Prsa; William F. Welsh; et al. (2011). "Kepler-16: A Transiting Circumbinary Planet". arXiv:1109.3432v1 [astro-ph.EP].
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(help) - ^ A. Gould; et al. "A Terrestrial Planet in a ~1 AU Orbit Around One Member of a ~15 AU Binary". arXiv:1407.1115.
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(help); "these projected separations are good proxies for the semi-major axis (afterupward adjustment by to correct for projection effects)" - ^ "A terrestrial planet in a ~1-AU orbit around one member of a ∼15-AU binary". Science. 345 (6192): 46–49. 4 July 2014. doi:10.1126/science.1251527.
{{cite journal}}
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(help) - ^ J. H. Telting, S. Charpinet. "A compact system of small planets around a former red-giant star". Nature. Retrieved 23 April 2013.
- ^ a b c "Notes for planet HD 13189 b". The Extrasolar Planets Encyclopaedia. Retrieved 15 September 2015.
- ^ "Notes for planet eps Tau b". The Extrasolar Planets Encyclopaedia. Retrieved 15 September 2015.
- ^ a b c Schneider, J. "Notes for planet 2M J044144 b". The Extrasolar Planets Encyclopaedia. Retrieved 28 November 2010.
- ^ "HD 208527 b". The Extrasolar Planet Encyclopaedia.
- ^ "Kepler-42 b". The Extrasolar Planet Encyclopaedia.
- ^ "The Extrasolar Planet Encyclopaedia — 2M 0746+20 b". exoplanet.eu.
- ^ "PSR J1719-1438 b". caltech.edu.
- ^ a b "HD 164922 b". The Extrasolar Planets Encyclopaedia. Retrieved 19 December 2012.
- ^ Joe Bauwens. "Sciency Thoughts: Planets in the NY Virginis system". sciencythoughts.blogspot.com.
- ^ "Fomalhaut b". The Extrasolar Planets Encyclopaedia. Retrieved 30 March 2013.
- ^ "HD 10180 i". The Extrasolar Planets Encyclopaedia. Retrieved 24 December 2012.
- ^ "HD 10180 j". The Extrasolar Planets Encyclopaedia. Retrieved 24 December 2012.
External links
- WiredScience, Top 5 Most Extreme Exoplanets, Clara Moskowitz, 21 January 2009