Kepler-438b

Kepler-438b[1][2][3]
Exoplanet List of exoplanets

Approximate size comparison of Kepler-438b (right) with Earth
Parent star
Star Kepler-438
Constellation Lyra[2]
Right ascension (α) 18h 46m 35.000s
Declination (δ) +41° 57′ 3.93″
Apparent magnitude (mV) 14.467
Distance470[2] ly
(145 pc)
Spectral type M?V
Mass (m) 0.544+0.06
−0.04 M☉
Radius (r) 0.52+0.06
−0.04 R☉
Temperature (T) 3748 (± 112) K
Metallicity [Fe/H] 0.16 (± 0.14)
Age 4.4+0.8
−0.7[3] Gyr
Physical characteristics
Radius(r)1.12 (± 0.16) R⊕
Stellar flux(F⊙)1.40+0.67
−0.77 ⊕
Temperature (T) 276 K (3 °C; 37 °F)
Orbital elements
Semi-major axis(a) 0.16600 AU
Eccentricity (e) 0.03+0.01
−0.03[3]
Orbital period(P) 35.23319 d
Inclination (i) 89.860°
Discovery information
Discovery date 2015[4]
Discoverer(s) Kepler spacecraft
Discovery method Transit
Discovery status Published refereed article
Other designations
KOI-3284.01; Kepler-438 b; KOI-3284 b; K03284.01; WISE J184634.98+415704.0 b; KIC 6497146 b; 2MASS J18463499+4157039 b
Database references
Extrasolar Planets
Encyclopaedia		data
SIMBADdata
Exoplanet Archivedata
Open Exoplanet Cataloguedata

Kepler-438b (also known by its Kepler Object of Interest designation KOI-3284.01) is a confirmed near-Earth-sized exoplanet, likely rocky, orbiting on the inner edge of the habitable zone of the red dwarf as it receives 1.4 times our solar flux.[5] Kepler-438, about 470 light-years (145 parsecs, or nearly 4.5×1015 km) from Earth in the constellation Lyra.[1][2] The planet was discovered by NASA's Kepler spacecraft using the transit method, in which the dimming effect that a planet causes as it crosses in front of its star is measured. NASA announced the confirmation of the exoplanet on 6 January 2015.[1] Kepler-438b is approximately 470 light years from Earth.

Characteristics

Mass, radius and temperature

Kepler-438b is an Earth-sized planet, an exoplanet that has a mass and radius close to that of Earth. It has a radius of 1.12 R⊕, and an unknown mass. It has an equilibrium temperature of 276 K (3 °C; 37 °F), close to that of Earth.

Host star

The planet orbits a (M-type) red dwarf star named Kepler-438. The star has a mass of 0.54 M☉ and a radius of 0.52 R☉, both lower than those of the Sun by almost half. It has a surface temperature of 3748 K and is estimated to be about 4.4 billion years old,[3] only 200 million years younger than the Sun.[6] and the Sun has a surface temperature of 5778 K.[7]

The star's apparent magnitude, or how bright it appears from Earth's perspective, is 14.467. Therefore, it is too dim to be seen with the naked eye.

Orbit and possible moons

Kepler-438b orbits its parent star once every 35.2 days.[1][2] It is likely tidally locked due to its close distance to its star.[8] A search for exomoons by the Hunt for Exomoons with Kepler project around Kepler-438b placed a maximum mass on a hypothetical moon at 29% that of the planet.[9]

Habitability

Kepler-438b is prone to large amounts of radiation from its star – its host star is a flare star, emitting stellar flares far more powerful than those from the Sun, as depicted in this artist's conception.

The planet was announced as orbiting within the habitable zone of Kepler-438, a region where liquid water could exist on the surface of the planet. However it has been found that this planet is subjected to powerful radiation activity from its parent star every 100 days, much more violent storms than the stellar flares emitted by the Sun and which would be capable of sterilizing life on Earth.[10]

Researchers at the University of Warwick say that Kepler-438b is not habitable due to the large amount of radiation it receives.[11] The question of what makes a planet habitable is much more complex than having a planet located at the right distance from its host star so that water can be liquid on its surface: various geophysical and geodynamical aspects, the radiation, and the host stars plasma environment can influence the evolution of planets and life, if it originated.[12] The planet is more likely to resemble a larger and cooler version of Venus.

Discovery and follow-up studies

In 2009, NASA's Kepler spacecraft was completing observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed 50000 stars in the Kepler Input Catalog, including Kepler-62; the preliminary light curves were sent to the Kepler science team for analysis, who chose obvious planetary companions from the bunch for follow-up at observatories. Observations for the potential exoplanet candidates took place between 13 May 2009 and 17 March 2012. After observing the respective transits, which for Kepler-438b occurred roughly every 35 days (its orbital period), it was eventually concluded that a planetary body was responsible for the periodic 35-day transits. The discovery, along with the planetary systems of the stars Kepler-442, Kepler-440 and Kepler-443 were announced on January 6, 2015.[1]

At nearly 460 light-years (140 pc) distant, Kepler-438b is too far from Earth for either current telescopes, or even the next generation of planned telescopes, to accurately determine its mass or whether it has an atmosphere. The Kepler spacecraft can only focus on a small, fixed region of the sky, but the next generation of planet-hunting space telescopes, such as TESS and CHEOPS, will have more flexibility. Exoplanetary systems, with stars less distant than Kepler 438, can then be studied in tandem with the upcoming James Webb Space Telescope and ground-based observatories like the future Square Kilometer Array.[13]

Notable Exoplanets – Kepler Space Telescope
Confirmed small exoplanets in habitable zones.
(Kepler-62e, Kepler-62f, Kepler-186f, Kepler-296e, Kepler-296f, Kepler-438b, Kepler-440b, Kepler-442b)
(Kepler Space Telescope; 6 January 2015).[1]

See also

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 5 Sample, Ian (7 January 2015). "Kepler 438b: Most Earth-like planet ever discovered could be home for alien life". The Guardian. Retrieved 7 January 2015.
  3. 1 2 3 4 Torres, Guillermo; Kipping, David M.; Fressin, Francois; Caldwell, Douglas A.; Twicken, Joseph D.; Ballard, Sarah; Batalha, Natalie M.; Bryson, Stephen T.; Ciardi, David R.; Henze, Christopher E.; Howell, Steve B.; Isaacson, Howard T.; Jenkins, Jon M.; Muirhead, Philip S.; Newton, Elisabeth R.; Petigura, Erik A.; Barclay, Thomas; Borucki, William J.; Crepp, Justin R.; Everett, Mark E.; Horch, Elliott P.; Howard, Andrew W.; Kolbl, Rea; Marcy, Geoffrey W.; McCauliff, Sean; Quintana, Elisa V. (2015). "Validation of Twelve Small Kepler Transiting Planets in the Habitable Zone". The Astrophysical Journal. 800 (2): 99. arXiv:1501.01101 [astro-ph.EP]. Bibcode:2015ApJ...800...99T. doi:10.1088/0004-637X/800/2/99. Cite uses deprecated parameter |class= (help)
  4. ↑ Staff (2015). "Planet Kepler-438 b". The Extrasolar Planets Encyclopaedia. Retrieved 11 January 2015.
  5. ↑ Gilster, Paul (6 January 2015). "AAS: 8 New Planets in Habitable Zone". Centauri-dreams.org. Retrieved 9 January 2015.
  6. ↑ Fraser Cain (16 September 2008). "How Old is the Sun?". Universe Today. Retrieved 19 February 2011.
  7. ↑ Fraser Cain (15 September 2008). "Temperature of the Sun". Universe Today. Retrieved 19 February 2011.
  8. ↑ "Kepler-438b: Astronomers Find Most Earth-Like Exoplanet Yet". Sci News. January 8, 2015. Retrieved June 13, 2016.
  9. ↑ Kipping, D. M.; et al. (2014). "The Hunt for Exomoons with Kepler (HEK). IV. A Search for Moons around Eight M Dwarfs". The Astrophysical Journal. 784 (1). 28. arXiv:1401.1210. Bibcode:2014ApJ...784...28K. doi:10.1088/0004-637X/784/1/28.
  10. ↑ Perkins, Sid (2015). "Earth-like planet may be not so hospitable after all, thanks to blasts of radiation". Science. doi:10.1126/science.aad7455. ISSN 0036-8075.
  11. ↑ 'Earth-like' Exoplanet Likely Not Habitable
  12. ↑ Lammer, H.; Bredehöft, J. H.; Coustenis, A.; Khodachenko, M. L.; et al. (2009). "What makes a planet habitable?" (PDF). The Astronomy and Astrophysics Review. 17 (2): 181–249. Bibcode:2009A&ARv..17..181L. doi:10.1007/s00159-009-0019-z. Archived from the original (PDF) on 2 June 2016. Retrieved 3 May 2016.
  13. ↑ 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:1302.0845. Bibcode:2013ApJ...767...94S. doi:10.1088/0004-637X/767/1/94.
Preceded by
Gliese 667 Cc		 Highest ESI for an exoplanet
2015–present		 Succeeded by
none

Coordinates: 18h 46m 35.000s, +41° 57′ 03.93″

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