Kepler-62f

Kepler-62f
Exoplanet List of exoplanets

Artist's impression of the Kepler-62 system (sizes to scale) compared to the planets of the inner Solar System with their respective habitable zones.
Parent star
Star Kepler-62 (KOI-701)
Constellation Lyra
Right ascension (α) 18h 52m 51.06019s
Declination (δ) +45° 20′ 59.507″
Apparent magnitude (mV) 13.654[1]
Distance~1200 ly
(368[2] pc)
Spectral type K2V[2]
Mass (m) 0.69 (± 0.02)[2] M☉
Radius (r) 0.64 (± 0.02)[2] R☉
Temperature (T) 4925 (± 70)[2] K
Metallicity [Fe/H] −0.37 (± 0.04)[2]
Age 7 (± 4)[2] Gyr
Physical characteristics
Mass(m)2.8+7.4
−1.6[3] M⊕
Radius(r)1.41 (± 0.07)[2] R⊕
Stellar flux(F⊙)0.41 (± 0.05)[2] ⊕
Temperature (T) 208 K (−65 °C; −85 °F)
Orbital elements
Semi-major axis(a) 0.718 (± 0.007)[2] AU
Eccentricity (e) ~0[2]
Orbital period(P) 267.291 (± 0.005)[2] d
Inclination (i) 89.90 (± 0.03)[2]°
Discovery information
Discovery date 18 April 2013[2][4]
Discoverer(s) Kepler spacecraft
Discovery method Transit[2]
Discovery status Published article
Other designations
KOI-701.04; K00701.04; KOI-701 f; 2MASS J18525105+4520595 f; KIC 9002278 f; WISE J185251.03+452059.0 f
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

Kepler-62f[2][4][5] (also known by its Kepler Object of Interest designation KOI-701.04) is a super-Earth exoplanet orbiting within the habitable zone of the star Kepler-62, the outermost of five such planets discovered by NASA's Kepler spacecraft. It is located about 1,200 light-years (370 parsecs, or nearly 1.135×1016 km) from Earth in the constellation of Lyra.[6] The exoplanet was found by using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. Kepler-62f may be a terrestrial or ocean-covered planet; it lies within the outer part of its host star's habitable zone.[2][7]

Characteristics

Mass, radius and temperature

Kepler-62f is a super-Earth, an exoplanet with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. It has an equilibrium temperature of 208 K (−65 °C; −85 °F), close to that of Mars.[8] It has a radius of 1.4 R⊕,[2] placing it below the radius of ≥1.6 R⊕ where it would otherwise be a mini-Neptune with a volatile composition, with no solid surface.[9] Due to its radius, it is likely a rocky planet. However, the mass isn't constrained yet, estimates place an upper limit of <35 M⊕, the real mass is expected to be significantly lower than this.[2] The true value is likely around 2.8 M⊕, assuming a rocky composition.[3]

Host star

The planet orbits a (K-type) star named Kepler-62, orbited by a total of five planets.[2] The star has a mass of 0.69 M☉ and a radius of 0.64 R☉. It has a temperature of 4925 K and is 7 billion years old.[2] In comparison, the Sun is 4.6 billion years old[10] and has a temperature of 5778 K.[11] The star is somewhat metal-poor, with a metallicity ([Fe/H]) of −0.37, or 42% of the solar amount.[2] Its luminosity (L☉) is 21% that of the Sun.[2]

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.65. Therefore, it is too dim to be seen with the naked eye.

Orbit

Kepler-62f orbits its host star with an orbital period of 267.29 days at a distance of about 0.718 AU (nearly the same distance as Venus from the Sun, which is 0.723 AU). It receives 41% of the amount of sunlight that Earth does from the Sun.[2]

Habitability

Artist's conception of a rocky Earth-size planet orbiting within the habitable zone of its parent star.

Given the planet's age (7 ± 4 billion years), irradiance (0.41 ± 0.05 times Earth's) and radius (1.41 ± 0.07 times Earth's), a rocky (silicate-iron) composition with the addition of a possibly substantial amount of water is considered plausible.[2] A modeling study indicates it is likely that a great majority of planets in its size range are completely covered by ocean.[12][13] If its density is the same as Earth's, its mass would be 1.413 or 2.80 times Earth's. The planet has the potential for hosting a moon according to a study of tidal effects on potentially habitable planets.[14] The planet may be the only habitable-zone candidate which would avoid desiccation by irradiation from the host star at its current location.[15]

Although Kepler-62f may be an ocean-covered planet possessing rock and water at the surface, it is the farthest out from its star, so without a supplementary amount of carbon dioxide (CO
2), it may be a planet covered entirely in ice.[16] In order for Kepler-62f to sustain an Earth-like climate (with an average temperature of around 284–290 K (11–17 °C; 52–62 °F), at least 5 bars (4.9 atm) of carbon dioxide would have to be present in the planet's atmosphere.[17]

Because it is the outermost planet, the effects of tidal evolution from the inner planets and the host star on Kepler-62f are not likely to have had significant outcomes over its lifetime. The axial tilt is likely to have been unchanged, and thus, the planet may have an axial tilt (anywhere from 14°–30°) and rotational period somewhat similar to Earth.[18] This can further make the planet more sustainable for habitability, as it would be able to transfer heat to the night side, instead of it being a planet with its surface being half water and half ice. K-type stars like Kepler-62 can live for approximately 20–40 billion years, 2 to 4 times longer than the estimated lifetime of our Sun.[19] The low stellar activity of orange dwarfs like Kepler-62, creates a relatively benign radiation environment for planets orbiting in their habitable zones, increasing their potential habitability.[20]

One review assay in 2015 concluded that Kepler-62f, along with the exoplanets Kepler-186f and Kepler-442b, were likely the best candidates for being potentially habitable planets.[21]

On 13 May 2016, researchers at University of California, Los Angeles (UCLA) announced that they had found various scenarios that allow the exoplanet to be habitable. They tested several simulations based on Kepler-62f having an atmosphere that ranges in thickness from the same as Earth’s all the way up to 12 times thicker than our planet’s, various concentrations of carbon dioxide in its atmosphere, ranging from the same amount as is in the Earth’s atmosphere up to 2,500 times that level and several different possible configurations for its orbital path.[22]

Discovery, follow-up studies & SETI target

Confirmed small exoplanets in habitable zones (artist's impressions).
(Kepler-62e, 62f, 186f, 296e, 296f, 438b, 440b, 442b)[23]

NASA's Kepler spacecraft observed 150000 stars in the Kepler Input Catalog, including Kepler-62, between 13 May 2009 and 17 March 2012. The software pipeline that searched for periodic dip in the stellar brightness, the sign of a planetary transit of the star, initially found three planets around Kepler-62, including Kepler-62e. Due to a bug in the software pipeline, the planet 62f was missed. A Kepler team member discovered three additional transits that had been missed by the pipeline,[4] which occurred every 267 days, and with a more detailed analysis the Kepler team concluded that a fourth planetary body, 62f, was responsible for the periodic 267-day transits. The discovery, along with the planetary system of the star Kepler-69 were announced on April 18, 2013.[2]

On 9 May 2013, a congressional hearing by two U.S. House of Representatives subcommittees discussed "Exoplanet Discoveries: Have We Found Other Earths?," prompted by the discovery of exoplanet Kepler-62f, along with Kepler-62e and Kepler-69c. A related special issue of the journal Science, published earlier, described the discovery of the exoplanets.[24]

Kepler-62f and the other Kepler-62 exoplanets are being specially targeted as part of the SETI search programs.[25] They will scan the areas for any signals that may represent technological life in the system. Given the interstellar distance of 1,200 light-years (370 pc), the signals would have left the planet that many years ago. As of 2016, no such signals have been found.

At nearly 1,200 light-years (370 pc) distant, Kepler-62f is too remote and its star too far for current telescopes or the next generation of planned telescopes to determine its mass or whether it has an atmosphere. The Kepler spacecraft focused on a single small region of the sky but next-generation planet-hunting space telescopes, such as TESS and CHEOPS, will examine nearby stars throughout the sky.

Nearby stars with planets can then be studied by the upcoming James Webb Space Telescope and future large ground-based telescopes to analyze atmospheres, determine masses and infer compositions. Additionally the Square Kilometer Array would significantly improve radio observations over the Arecibo Observatory and Green Bank Telescope.[26]

See also

References

  1. ↑ "Kepler Input Catalog search result". Space Telescope Science Institute. Retrieved 18 April 2013.
  2. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 Borucki, William J.; et al. (18 April 2013). "Kepler-62: A Five-Planet System with Planets of 1.4 and 1.6 Earth Radii in the Habitable Zone". Science Express. 340 (6132): 587–590. arXiv:1304.7387Freely accessible. Bibcode:2013Sci...340..587B. doi:10.1126/science.1234702. PMID 23599262.
  3. 1 2 "PHL's Exoplanets Catalog - Planetary Habitability Laboratory @ UPR Arecibo".
  4. 1 2 3 Johnson, Michele; Harrington, J.D. (18 April 2013). "NASA's Kepler Discovers Its Smallest 'Habitable Zone' Planets to Date". NASA. Retrieved 18 April 2013.
  5. ↑ Overbye, Dennis (18 April 2013). "2 Good Places to Live, 1,200 Light-Years Away". New York Times. Retrieved 18 April 2013.
  6. ↑ "Kepler-62f: A Possible Water World".
  7. ↑ "3 Potentially Habitable Super-Earth Planets Explained (Infographic)".
  8. ↑ "Kepler-62 f". NASA Exoplanet Archive. Retrieved 23 July 2016.
  9. ↑ "Most 1.6 Earth-radius planets are not rocky". 31 July 2014.
  10. ↑ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
  11. ↑ Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
  12. ↑ "Water worlds surface: Planets covered by global ocean with no land in sight". Harvard Gazette. 18 April 2013. Retrieved 19 April 2013.
  13. ↑ Kaltenegger, L.; Sasselov, D.; Rugheimer, S. (18 April 2013). "Water Planets in the Habitable Zone: Atmospheric Chemistry, Observable Features, and the case of Kepler-62e and -62f". The Astrophysical Journal. 775 (2): L47. arXiv:1304.5058Freely accessible. Bibcode:2013ApJ...775L..47K. doi:10.1088/2041-8205/775/2/L47.
  14. ↑ Sasaki, Takashi; Barnes, Jason W. (30 June 2014). "Longevity of moons around habitable planets". International Journal of Astrobiology. 13 (4): 324–336. Bibcode:2014IJAsB..13..324S. doi:10.1017/S1473550414000184.
  15. ↑ Luger, Rodrigo; Barnes, Rory (2015). "Extreme Water Loss and Abiotic O2 Buildup On Planets Throughout the Habitable Zones of M Dwarfs". Astrobiology. 15 (2): 119–143. arXiv:1411.7412Freely accessible. Bibcode:2015AsBio..15..119L. doi:10.1089/ast.2014.1231. PMC 4323125Freely accessible. PMID 25629240.
  16. ↑ "Water Planets in the Habitable Zone: A Closer Look at Kepler 62e and 62f". Harvard-Smithsonian Center for Astrophysics. Sci Tech Daily. April 22, 2013. Retrieved 2016-05-10.
  17. ↑ Shields, Aomawa L.; et al. (2016). "The Effect of Orbital Configuration on the Possible Climates and Habitability of Kepler-62f". Astrobiology. 16 (6): 443–64. arXiv:1603.01272Freely accessible. Bibcode:2016AsBio..16..443S. doi:10.1089/ast.2015.1353. PMC 4900229Freely accessible. PMID 27176715.
  18. ↑ Adam Hanhazy (2015-02-19). "Planets Can Alter Each Other's Climates over Eons". Astrobiology. Retrieved 2016-06-22.
  19. ↑ Paul Glister (August 12, 2009). "In Praise of K-class Stars". Centauri Dreams. Retrieved July 2, 2016.
  20. ↑ "Life Could Easily Develop Around Orange Dwarfs". Softpedia. Retrieved May 17, 2016.
  21. ↑ Paul Gilster, Andrew LePage (2015-01-30). "A Review of the Best Habitable Planet Candidates". Centauri Dreams, Tau Zero Foundation. Retrieved 2015-07-24.
  22. ↑ http://online.liebertpub.com/doi/abs/10.1089/ast.2015.1353 The Effect of Orbital Configuration on the Possible Climates and Habitability of Kepler-62f
  23. ↑ Clavin, Whitney; Chou, Felicia; Johnson, Michele (6 January 2015). "NASA's Kepler Marks 1,000th Exoplanet Discovery, Uncovers More Small Worlds in Habitable Zones". NASA. Retrieved 6 January 2015.
  24. ↑ Staff (3 May 2013). "Special Issue: Exoplanets". Science. Retrieved 18 May 2013.
  25. ↑ "Has Kepler Found Ideal SETI-target Planets?". SETI Institute. 19 April 2013. Retrieved 17 September 2013.
  26. ↑ Siemion, Andrew P.V.; Demorest, Paul; Korpela, Eric; Maddalena, Ron J.; Werthimer, Dan; Cobb, Jeff; Langston, Glen; Lebofsky, Matt; Marcy, Geoffrey W.; Tarter, Jill (3 February 2013). "A 1.1 to 1.9 GHz SETI Survey of the Kepler Field: I. A Search for Narrow-band Emission from Select Targets". Astrophysical Journal. 767: 94. arXiv:1302.0845Freely accessible. Bibcode:2013ApJ...767...94S. doi:10.1088/0004-637X/767/1/94.

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Coordinates: 18h 52m 51.06019s, +45° 20′ 59.507″

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