Kepler-70

Kepler-70
Observation data
Epoch       Equinox
Constellation Cygnus[1][note 1]
Right ascension 19h 45m 25s[1]
Declination +41° 5′ 34″[1]
Apparent magnitude (V) 14.87[2]
Characteristics
Spectral type sdB[1]
Apparent magnitude (U) 13.80[2]
Apparent magnitude (B) 14.71[2]
Apparent magnitude (R) 15.43[2]
Apparent magnitude (I) 15.72[2]
Apparent magnitude (J) 15.36[2]
Apparent magnitude (H) 15.59[2]
Astrometry
Distance3849 ± 310[1] ly
(1180 ± 95[1] pc)
Details
Mass0.496 ± 0.002[1] M☉
Radius0.203 ± 0.007[1] R☉
Luminosity (bolometric)22.9 ±  3.1 L☉
Temperature27,730 ± 260[1] K
Other designations
2MASS J19452546+4105339, CMC14 J194525.4+410533, GSC2.3 N2IY060737, KIC 5807616, KOI-55, KPD 1943+4058, UCAC2 46165657, UCAC3 263-170867, USNO-B1.0 1310-00349976.[2]

Kepler-70, formerly known as KOI-55, is a star in the constellation Cygnus with an apparent visual magnitude of 14.87.[2] This is too faint to be seen with the naked eye; viewing it requires a telescope with an aperture of 40 cm (20 in) or more.[3]

A subdwarf B star, KOI-55 passed through the red giant stage some 18.4 million years ago. In its present day state, it is fusing helium in its core. Once it runs out of helium it will contract to form a white dwarf. It has a relatively small radius of about 0.2 times the Sun's radius; white dwarfs are generally much smaller.[4] The star is host to a planetary system with two planets, KOI-55.01 and KOI-55.02.[5]

Planetary system

On December 26, 2011, evidence for two extremely short-period planets was announced. They were detected by the reflection of starlight caused by the planets themselves, rather than through a variation in apparent stellar magnitude caused by them transiting the star.

The measurements also suggested a smaller body between the two confirmed planets; this remains unconfirmed.

Orbits of Kepler-70b and Kepler-70c have 7:10 orbital resonance and have the closest approach between planets of any known planetary system.

The Kepler-70 planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.440 M⊕ 0.0060 0.2401 — 20–80, likely 65 [note 2]° 0.759 R⊕
KOI-55.03 (unconfirmed) 0.222 M⊕ 0.0065  — — — 0.605 R⊕
c 0.655 M⊕ 0.0076 0.34289 — 20–80, likely 65° 0.867 R⊕

Notes

  1. ↑ This is inferred from the RA and declination of the star.
  2. ↑ inclinations are derived from brightness variations and lack of transits.

References

  1. 1 2 3 4 5 6 7 8 9 "Notes for Planet KOI-55 b". Extrasolar Planet Database. Retrieved 1 January 2012.
  2. 1 2 3 4 5 6 7 8 9 "SIMBAD query result". SIMBAD. Retrieved 1 January 2012.
  3. ↑ Sherrod, P. Clay; Koed, Thomas L. (2003), A Complete Manual of Amateur Astronomy: Tools and Techniques for Astronomical Observations, Astronomy Series, Courier Dover Publications, p. 9, ISBN 0-486-42820-6
  4. ↑ Cain, Fraser (4 February 2009). "White Dwarf Stars". Universe Today. Retrieved 8 January 2012.
  5. 1 2 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

External links

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