Kepler-70c

Kepler-70c (formerly called KOI-55.02; sometimes listed as KOI-55 c) is one of two postulated exoplanets orbiting the sdB star Kepler-70.[1]

Kepler-70c
Discovery
Discovered byCharpinet et al.[1]
Discovery siteKepler telescope
Discovery date12/22/2011 (announced)[1]
Reflection/emission modulations
Orbital characteristics
0.0076 AU (1,140,000 km)
0.34289 d
Inclination~60
StarKepler-70
Physical characteristics
Mean radius
0.867[note 1][2] R⊕
Mass0.655 M⊕
8.55 m/s2
9.73 km/s
Temperature6,807 K (6,534 °C; 11,793 °F) [note 2][3]
  1. Assuming an albedo of 0.1.
  2. Assuming an albedo of 0.1.

Their discovery was announced in 2011.[1] However, later research[4][5] suggests that the two exoplanets probably do not exist, and that "pulsation modes visible beyond the cut-off frequency of the star" were a more likely explanation for the signals believed to indicate exoplanets. This is not proven with certainty one way or the other.

If it exists, Kepler-70c orbits its host along with another planet, Kepler-70b. Both of these planets orbit very close to their host star. Kepler-70c completes one orbit around its star in just 8.232 hours. It is also one of the hottest exoplanets as of mid-2013. It has a high density, suggesting that it is largely composed of metals.[6]

Kepler-70b passes 240,000 km away from Kepler-70c during their closest approach. This is currently the closest recorded approach between planets. Such orbital configuration is relatively stable due to orbital resonance between planets and small Hill spheres of planets due to proximity of the star.

According to the main author of the paper in Nature which announced the discovery of the two planets, Stephane Charpinet, the two planets "probably plunged deep into the star's envelope during the red giant phase, but survived."[7] However, this is not the first sighting of planets orbiting a post-red giant star - numerous pulsar planets have been observed, including one that orbits closer to its host star, and consequently in a shorter time than, any other planet.

Origins

The two planets may have started out as a pair of gas giants which spiraled inward toward their host star, which subsequently became a red giant. This engulfed the planets, evaporating all but their solid cores, which now orbit the sdB star.[7] Alternatively, there may only have been one gas giant engulfed in this way, with the rocky/metallic core having survived evaporation but fragmented inside the star.[8] If this theory is correct, the two planets would be two large sections of the gas giant's core.

According to the Extrasolar Planets Encyclopedia, the star left the red giant stage 18.4 million years ago.[2]

See also

Notes

    References
    1. Charpinet, S.; et al. (December 21, 2011), "A compact system of small planets around a former red-giant star", Nature, 480 (7378): 496–499, Bibcode:2011Natur.480..496C, doi:10.1038/nature10631, PMID 22193103
    2. "Notes for Planet KOI-55 b". Extrasolar Planet Database. Archived from the original on 19 January 2012. Retrieved 1 January 2012.
    3. http://phl.upr.edu/projects/habitable-exoplanets-catalog/calculators
    4. Krzesinski, J. (August 25, 2015), "Planetary candidates around the pulsating sdB star KIC 5807616 considered doubtful", Astronomy & Astrophysics, 581: A7, Bibcode:2015A&A...581A...7K, doi:10.1051/0004-6361/201526346
    5. Blokesz, A.; Krzesinski, J.; Kedziora-Chudczer, L. (4 July 2019), "Analysis of putative exoplanetary signatures found in light curves of two sdBV stars observed by Kepler", Astronomy & Astrophysics, 627: A86, arXiv:1906.03321, Bibcode:2019A&A...627A..86B, doi:10.1051/0004-6361/201835003
    6. "Kepler mission discoveries". Retrieved 3 July 2013.
    7. "Two More Earth-Sized Planets Discovered by Kepler, Orbiting Former Red Giant Star". Universe Today. Retrieved 1 January 2012.
    8. Bear, E.; Soker, N. (26 March 2012), "A tidally destructed massive planet as the progenitor of the two light planets around the SDB star KIC 05807616", The Astrophysical Journal Letters, 749 (1): L14, arXiv:1202.1168, Bibcode:2012ApJ...749L..14B, doi:10.1088/2041-8205/749/1/L14
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.