HD 222155

Last updated
HD 222155
Observation data
Epoch J2000       Equinox J2000
Constellation Andromeda
Right ascension 23h 38m 00.30719s [1]
Declination +48° 59′ 47.4874″ [1]
Apparent magnitude  (V)7.1 [2]
Characteristics
Evolutionary stage main sequence star
Spectral type G0V
B−V color index 0.64
Astrometry
Radial velocity (Rv)−44.00±0.12 [1]  km/s
Proper motion (μ)RA: 195.306  mas/yr [1]
Dec.: -117.335  mas/yr [1]
Parallax (π)19.8020 ± 0.0160  mas [1]
Distance 164.7 ± 0.1  ly
(50.50 ± 0.04  pc)
Details [2] [3] [4]
Mass 1.21±0.10  M☉
Radius 1.85±0.04  R☉
Luminosity 3.2  L☉
Surface gravity (log g)4.10±0.13  cgs
Temperature 5720±44  K
Metallicity [Fe/H]-0.11±0.05  dex
Rotational velocity (v sin i)3.2±1.0 km/s
Age 8.2±0.7  Gyr
Other designations
BD+48 4112, Gaia DR2  1943363751009454976, HD  222155, HIP  116616, SAO  53211, TYC  3646-2286-1, 2MASS J23380027+4859475 [5]
Database references
SIMBAD data

HD 222155 is a star in the northern constellation of Andromeda. [5] It is a yellow star that can be viewed with binoculars or a small telescope, but is too faint to be seen with the naked eye at an apparent visual magnitude of 7.1. The imaging survey in 2017 did not detect any stellar companions to HD 222155. [6]

This is an old main sequence star with a stellar classification of G0V; [5] a star that is nearing an exhaustion of its hydrogen fuel. It is already beginning to expand its gaseous envelope, [2] having radius of 1.85R☉. [3] The star is relatively depleted of heavy elements, having about 80% of solar abundance, and has weak yet noticeable ultraviolet flare activity. [7] [8]

Planetary system

Based on radial velocity data gathered in 2007–2011, the discovery of a superjovian planet b outside the habitable zone [4] was announced in May 2012. [2] The stellar and planetary parameters were refined in 2016. [3] In 2023, the inclination and true mass of HD 222155 b were measured via astrometry. [9]

The HD 222155 planetary system [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 2.1+0.3
−0.2  MJ 		4.7±0.13470+102
−106		0.34±0.0966+14
−11 or 115+13
−16 ° 		—

Related Research Articles

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HD 126614 is a trinary star system in the equatorial constellation of Virgo. The primary member, designated component A, is host to an exoplanetary companion. With an apparent visual magnitude of 8.81, it is too faint to be seen with the naked eye. The system is located at a distance of 239 light years from the Sun based on parallax measurements, but is drifting closer with a radial velocity of −33 km/s.

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HD 164509 is a binary star system in the constellation of Ophiuchus. The primary component has an orbiting exoplanet companion. This system is located at a distance of 175 light years based on parallax measurements, and is drifting further away with a radial velocity of 13.7 km/s. It has an absolute magnitude of 4.64, but at that distance the system has an apparent visual magnitude of 8.10, which is too faint to be seen with the naked eye.

HD 7449 is a binary star system about 126 light-years way. The primary star, HD 7449 A, is a main-sequence star belonging to the spectral class F9.5. It is younger than the Sun. The primary star is slightly depleted of heavy elements, having 80% of solar abundance.

HD 197037 is a binary star system. Its primary or visible star, HD 197037 A, is a F-type main-sequence star. Its surface temperature is 6150±34 K. HD 197037 A is depleted in heavy elements compared to the Sun, with a metallicity Fe/H index of −0.16±0.03, but is younger at an age of 3.408±0.924 billion years.

HD 221420 is a likely binary star system in the southern circumpolar constellation Octans. It has an apparent magnitude of 5.81, allowing it to be faintly seen with the naked eye. The object is relatively close at a distance of 102 light years but is receding with a heliocentric radial velocity of 26.5 km/s.

HD 106315, or K2-109, is a single star with a pair of close-orbiting exoplanets, located in the constellation of Virgo. Based on parallax measurements, this system lies at a distance of 356 light years from the Sun. At that range, the star is too faint to be seen with the naked eye, as it has an apparent visual magnitude of 8.95. But it is slowly drifting closer with a radial velocity of −3 km/s. As of 2020, multiplicity surveys have not detected any stellar companions to HD 106315.

References

  1. 1 2 3 4 5 6 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.
  2. 1 2 3 4 Boisse, Isabelle; Pepe, Francesco; Perrier, Christian; Queloz, Didier; Bonfils, Xavier; Bouchy, François; Santos, Nuno C.; Arnold, Luc; Beuzit, Jean-Luc; Dìaz, Rodrigo F.; Delfosse, Xavier; Eggenberger, Anne; Ehrenreich, David; Forveille, Thierry; Hébrard, Guillaume; Lagrange, Anne-Marie; Lovis, Christophe; Mayor, Michel; Moutou, Claire; Naef, Dominique; Santerne, Alexandre; Ségransan, Damien; Sivan, Jean-Pierre; Udry, Stéphane (2012), "The SOPHIE search for northern extrasolar planets V. Follow-up of ELODIE candidates: Jupiter-analogs around Sun-like stars", Astronomy and Astrophysics, 545: A55, arXiv: 1205.5835 , Bibcode:2012A&A...545A..55B, doi:10.1051/0004-6361/201118419, S2CID   119109836
  3. 1 2 3 Stassun, Keivan G.; Collins, Karen A.; Gaudi, B. Scott (2016), "Accurate empirical radii and masses of planets and their host stars with Gaia parallaxes", The Astronomical Journal, 153 (3): 136, arXiv: 1609.04389 , Bibcode:2017AJ....153..136S, doi: 10.3847/1538-3881/aa5df3 , S2CID   119219062
  4. 1 2 Kokaia, Giorgi; Davies, Melvyn B.; Mustill, Alexander J. (2020), "Resilient habitability of nearby exoplanet systems", Monthly Notices of the Royal Astronomical Society, 492 (1): 352–368, arXiv: 1910.07573 , Bibcode:2020MNRAS.492..352K, doi: 10.1093/mnras/stz3408 , S2CID   204743669
  5. 1 2 3 "HD 222155". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 17 September 2020.
  6. ↑ Wittrock, Justin M.; Kane, Stephen R.; Horch, Elliott P.; Howell, Steve B.; Ciardi, David R.; Everett, Mark E. (2017), "Exclusion of Stellar Companions to Exoplanet Host Stars", The Astronomical Journal, 154 (5): 184, arXiv: 1709.05315v1 , Bibcode:2017AJ....154..184W, doi: 10.3847/1538-3881/aa8d69 , S2CID   55789971
  7. ↑ Evgenya L. Shkolnik, "AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS", 2013
  8. ↑ Viswanath, Gayathri; Narang, Mayank; Manoj, P.; Mathew, Blesson; Kartha, Sreeja S. (2020), "A statistical search for Star-Planet Interaction in the UltraViolet using GALEX", The Astronomical Journal, 159 (5): 194, arXiv: 2003.03349v1 , Bibcode:2020AJ....159..194V, doi: 10.3847/1538-3881/ab7d3b , S2CID   212628609
  9. 1 2 Philipot, F.; Lagrange, A.-M.; et al. (January 2023). "Updated characterization of long-period single companion by combining radial velocity, relative astrometry, and absolute astrometry". Astronomy & Astrophysics. 670: A65. arXiv: 2301.01263 . Bibcode:2023A&A...670A..65P. doi:10.1051/0004-6361/202245396. S2CID   255393653.
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