Jump to content

Kepler-737

Add links
Coordinates: Sky map 19h 27m 27.085s, +46° 25′ 45.89″
From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Lithopsian (talk | contribs) at 13:55, 8 April 2022 (short is good, but I think it can't stand to be a little longer). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

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 in the border of the constellation Cygnus. It was discovered by HARPS using the transit method and announced on May 10, 2016.[6] To the naked eye, it appears a single faint star of its magnitude.[4]

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] It's spectral class is M0V, its temperature is about 3,813 Kelvin, with 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, containing Iron and Hydrogen on its core, significantly lower than the Sun's. Its density is rough ~5.239±0.265 g/cm3.[5] Its gravity is weaker than the Sun, with log g of 4.722±0.008 cgs. Its stellar density is about ~5.239±0.265 g/cm3, while the sun has about 1.41 g/cm³.[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] There are many confirmed apparent magnitudes pending on NASA headquarters, these apparent magnitudes employed to measure the brightness of a star Kepler-737 with their filter names. Its distance is alternatively 205.8±0.8 pc.

Planetary System

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🜨

Kepler-737b

File:Lalande 21185.png
An transiting planet orbing a star Kepler-737
Main article: Kepler-737b

Kepler-737b[6] was discovered and suspected since May 18, 2016, for orbiting in the habitable zone but not likely to be inhabitable because Kepler-737b is tidally locked.[7] [8][9] Kepler-737b may instead 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 Kepler-737b's 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 f "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.
Retrieved from "https://en.wikipedia.org/enwiki/w/index.php?title=Kepler-737&oldid=1081607495"