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HD 222155

Coordinates:Sky map23h 38m 00.3072s, +48° 59′ 47.4865″
From Wikipedia, the free encyclopedia
Old G-type main sequence star in the constellation Andromeda
HD 222155
Observation data
Epoch J2000      Equinox J2000
ConstellationAndromeda
Right ascension23h 38m 00.30719s[1]
Declination+48° 59′ 47.4874″[1]
Apparent magnitude (V)7.1[2]
Characteristics
Evolutionary stagemain sequence star
Spectral typeG0V
B−Vcolor index0.64
Astrometry
Radial velocity (Rv)−44.00±0.12[1] km/s
Proper motion (μ)RA: 195.306mas/yr[1]
Dec.: -117.335mas/yr[1]
Parallax (π)19.8020±0.0160 mas[1]
Distance164.7 ± 0.1 ly
(50.50 ± 0.04 pc)
Details[2][3][4]
Mass1.21±0.10 M
Radius1.85±0.04 R
Luminosity3.2 L
Surface gravity (log g)4.10±0.13 cgs
Temperature5720±44 K
Metallicity [Fe/H]-0.11±0.05 dex
Rotational velocity (v sin i)3.2±1.0 km/s
Age8.2±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
SIMBADdata

HD 222155 is astar in the northernconstellation ofAndromeda.[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 anapparent visual magnitude of 7.1. The imaging survey in 2017 did not detect any stellar companions to HD 222155.[6]

This is an oldmain sequence star with astellar 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

[edit]

Based on radial velocity data gathered in 2007–2011, the discovery of asuperjovian 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 viaastrometry.[9]

The HD 222155 planetary system[9]
Companion
(in order from star)
MassSemimajor axis
(AU)
Orbital period
(days)
EccentricityInclinationRadius
b2.1+0.3
−0.2
 MJ
4.7±0.13470+102
−106
0.34±0.0966+14
−11
or115+13
−16
°

References

[edit]
  1. ^abcdeVallenari, 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 atVizieR.
  2. ^abcdBoisse, 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. ^abcStassun, 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. ^abKokaia, 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. ^abc"HD 222155".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved17 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. ^abPhilipot, 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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