HD 210702

HD 210702
Observation data
Epoch J2000      Equinox J2000
Constellation Pegasus[1]
Right ascension 22h 11m 51.331s[2]
Declination +16° 02′ 26.00″[2]
Apparent magnitude (V) 5.93[1]
Characteristics
Evolutionary stage subgiant[3]
Spectral type K1 III[4] or K1 IV[3]
B−V color index 0.951±0.001[1]
Astrometry
Radial velocity (Rv)18.4593±0.0392[5] km/s
Proper motion (μ) RA: −3.263±0.156 mas/yr[2]
Dec.: −17.296±0.036 mas/yr[2]
Parallax (π)18.4593 ± 0.0392 mas[2]
Distance176.7 ± 0.4 ly
(54.2 ± 0.1 pc)
Absolute magnitude (MV)2.14[3]
Details
Mass1.47±0.04[6] M☉
Radius4.9±0.1[6] R☉
Luminosity12.9±0.1[6] L☉
Surface gravity (log g)3.2200±0.074[7] cgs
Temperature4,946±32[6] K
Metallicity [Fe/H]0.083±0.027[7] dex
Rotational velocity (v sin i)2.50±0.48[7] km/s
Age3.1±0.3[6] Gyr
Other designations
BD+15º4592, HD 210702, HIP 109577, HR 8461, SAO 107729[8]
Database references
SIMBADdata

HD 210702 is a star with an orbiting exoplanet in the northern constellation of Pegasus.[1] It has an apparent visual magnitude of 5.93,[1] which is bright enough that the star is dimly visible to the naked eye. The distance to HD 210702 is 177 light years based on parallax measurements, and it is drifting further away with a radial velocity of 18.5 km/s.[5] It is a probable member of the Ursa Major moving group, an association of co-moving stars.[4]

Although a stellar classification of K1 III[4] suggests this is an evolved giant star, it is more likely to be a subgiant star currently at the based of the red giant branch.[9] Currently 3[6] billion years old, HD 210702 spent its main-sequence life as an A-type star. Consistent with its evolutionary status, it has little or no magnetic activity in its chromosphere.[10] The star has 1.5[6] times the mass of the Sun and has expanded to 4.9 times the Sun's radius. It is radiating 12.9 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,946 K.[6]

Planetary system

The star shows variability in its radial velocity consistent with an exoplanetary companion in a Keplerian orbit,[10] and one was duly discovered in April 2007, from observations at Lick and Keck Observatories in Mount Hamilton (California) and Mauna Kea (Hawai'i), United States. As the inclination of the orbital plane is unknown, only a lower bound on the mass of this object can be estimated. It has at least 1.8 times the mass of Jupiter.[9]

The HD 210702 planetary system[9]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b ≥1.808±0.097 MJ 1.148±0.057 354.10±0.70 0.028±0.034 — —

See also

References

  1. ^ a b c d e Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  2. ^ a b c d Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c Sato, Bun'ei; et al. (2012). "Substellar Companions to Seven Evolved Intermediate-Mass Stars". Publications of the Astronomical Society of Japan. 64 (6). 135. arXiv:1207.3141. Bibcode:2012PASJ...64..135S. doi:10.1093/pasj/64.6.135.
  4. ^ a b c Levato, H.; Abt, H. A. (August 1978). "Spectral types in the Ursa Major stream". Publications of the Astronomical Society of the Pacific. 90: 429−433. Bibcode:1978PASP...90..429L. doi:10.1086/130352.
  5. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ a b c d e f g h Bonfanti, A.; et al. (2016). "Age consistency between exoplanet hosts and field stars". Astronomy & Astrophysics. 585: 14. arXiv:1511.01744. Bibcode:2016A&A...585A...5B. doi:10.1051/0004-6361/201527297. S2CID 53971692. A5.
  7. ^ a b c Hojjatpanah, S.; et al. (2019). "Catalog for the ESPRESSO blind radial velocity exoplanet survey". Astronomy and Astrophysics. 629: A80. arXiv:1908.04627. Bibcode:2019A&A...629A..80H. doi:10.1051/0004-6361/201834729. S2CID 199552090.
  8. ^ "HD 210702". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-15.
  9. ^ a b c Luhn, Jacob K.; et al. (2019). "Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts". The Astronomical Journal. 157 (4). 149. arXiv:1811.03043. Bibcode:2019AJ....157..149L. doi:10.3847/1538-3881/aaf5d0. S2CID 102486961.
  10. ^ a b Johnson, John Asher; et al. (2007). "Retired A Stars and Their Companions: Exoplanets Orbiting Three Intermediate-Mass Subgiants". The Astrophysical Journal. 665 (1): 785–793. arXiv:0704.2455. Bibcode:2007ApJ...665..785J. doi:10.1086/519677.

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