Kepler-737
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus[1]
Right ascension 19h 27m 27.085s[2]
Declination +46° 25′ 45.29″[2]
Characteristics
Evolutionary stage main-sequence[3]
Spectral type M0V[3]
Apparent magnitude (G) 15.127694[4]
Apparent magnitude (J) 12.910[4]
Apparent magnitude (H) 12.293[4]
Apparent magnitude (K) 12.097[4]
Apparent magnitude (B) 17.861[5]
Apparent magnitude (V) 15.971[5]
Apparent magnitude (W) 11.969[5]
Astrometry
Proper motion (μ) RA: 20.094[2] mas/yr
Dec.: −19.889[2] mas/yr
Parallax (π)4.8590 ± 0.0194 mas[2]
Distance671 ± 3 ly
(205.8 ± 0.8 pc)
Details
Mass0.510+0.0026
−0.0027[1] M☉
Radius0.480+0.0026
−0.0024[1] R☉
Luminosity~0.045[5] L☉
Surface gravity (log g)4.722±0.008[5] cgs
Temperature3,813+40.127
−38.492[3] K
Metallicity [Fe/H]−0.24+0.087
−0.081[5] dex
Age3.89[5] Gyr
Other designations
Gaia DR2 2126820324123177472, KOI-947, KIC 9710326, TIC 63068329, 2MASS J19272708+4625453, WISE J192727.10+462545.1
Database references
SIMBADdata

Kepler-737 is an M-type main-sequence red dwarf located 671 light-years away on the border of the constellation Cygnus. [6]

Physical properties

General properties

Kepler-737 is around half the size of the Sun, with a mass of 0.51 solar masses and a radius of 0.48 solar radii.[1] Its spectral class is M0V, its temperature is about 3,813 Kelvin, and it has a brightness of 0.045 solar luminosity.[5] One Kepler Object of Interest (KOI) table claimed the star to be ~14 billion years old.[5]

As for the logarithm of the relative abundance of iron and hydrogen, its metallicity [Fe/H] is −0.24+0.087
−0.081 dex, significantly lower than the Sun's. Its density is roughly 5.239±0.265 g/cm3, or about 3 times denser than the Sun;[5] while its surface gravity is stronger than the Sun, with log g of 4.722±0.008 cgs.[5]

Astrometry and characteristics

SIMBAD data indicate that its proper motion is 20.094 mas/yr for right ascension, −19.889 mas/yr for declination, its parallax is 4.859 mas.[4]

Planetary system

The star has one known planet, Kepler-737b.

The Kepler-737 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius[6]
b ~4.5 M🜨 0.035 28.592 0 89.99° 1.96±0.11 R🜨

Main article: Kepler-737b

Kepler-737b[6] was confirmed on May 18, 2016 from data collected earlier by the Kepler space telescope, notable for orbiting in the habitable zone but not likely to be habitable because it is tidally locked.[7][8][9] It may, however, have atmospheric circulation that would distribute the heat around the planet, potentially making a large portion of it habitable, although given its stellar flux the most likely scenario is that the planet's surface is too hot to be habitable. Water on its surface could also distribute heat.

On the note of the Exoplanet Archive, Kepler-737b was dedicated that orbital period, transit mid-point, transit duration, Rp/Rs, and their errors are taken from DR24 KOI table.[5]

References

  1. ^ a b c d "Kepler-737". Universe Guide. Retrieved May 18, 2016.
  2. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. ^ a b c "Kepler-737". Exoplanet Kyoto. Retrieved May 18, 2016.
  4. ^ a b c d e "Kepler-737". SIMBAD. Retrieved May 18, 2016.
  5. ^ a b c d e f g h i j k l "Kepler-737's Documentary in NASA Exoplanet Archive". NASA Exoplanet Archive. Retrieved May 18, 2016.
  6. ^ a b c "Planet beyond our solar system: Kepler-737b". Exoplanet Exploration. Retrieved May 18, 2016.
  7. ^ "Tidally locked exoplanets may be more common than previously thought". UW News. Retrieved 2021-05-18.
  8. ^ Hammond, Mark; Lewis, Neil T. (2021-03-30). "The rotational and divergent components of atmospheric circulation on tidally locked planets". Proceedings of the National Academy of Sciences. 118 (13): e2022705118. arXiv:2102.11760. Bibcode:2021PNAS..11822705H. doi:10.1073/pnas.2022705118. ISSN 0027-8424. PMC 8020661. PMID 33753500.
  9. ^ Sutter, Paul (2021-03-08). "Can super-rotating oceans cool off extreme exoplanets?". Space.com. Retrieved 2021-05-18.
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