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HD 210056

From Wikipedia, the free encyclopedia
Star in the constellation of Octans
HD 210056
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationOctans
Right ascension22h 11m 54.98416s[1]
Declination−76° 06′ 57.6788″[1]
Apparent magnitude (V)6.13±0.01[2]
Characteristics
Spectral typeK0 III[3]
U−Bcolor index+0.82[4]
B−Vcolor index+1.00[4]
Astrometry
Radial velocity (Rv)24±1[5] km/s
Proper motion (μ)RA: −59.351mas/yr[1]
Dec.: −40.005mas/yr[1]
Parallax (π)11.1656±0.0205 mas
Distance292.1 ± 0.5 ly
(89.6 ± 0.2 pc)
Absolute magnitude (MV)+1.41[6]
Details[7]
Mass1.59±0.07 M
Radius7.72±0.13 R
Luminosity29.7±0.5 L
Surface gravity (log g)2.86±0.10 cgs
Temperature4,849±37 K
Metallicity [Fe/H]−0.08±0.03 dex
Rotational velocity (v sin i)<1.5[8] km/s
Age2.10±0.22[9] Gyr
Other designations
68 G. Octantis[10],CD−76°1120,CPD−76°1549,GC 31004,HD 210056,HIP 109584,HR 8432,SAO 258006[11]
Database references
SIMBADdata

HD 210056, also known asHR 8432, is a solitary orange huedstar located in the southerncircumpolar constellationOctans. Eggen (1993) listed it as a member of the old disk population.[12]

The object has anapparent magnitude of 6.13,[2] making it barely visible to thenaked eye. Based onparallax measurements from theGaia satellite, the object is estimated to be 292light years distant.[1] It appears to be receding with a heliocentricradial velocity of24 km/s.[5] At its current distance, HD 210056's brightness is diminished by 0.2magnitudes due to interstellar dust. It has anabsolute magnitude of +1.41.[13]

This is an evolvedgiant star with astellar classification of K0 III. It has 1.59 times themass of the Sun but has expanded to 7.72 times itsgirth.[7] It radiates 29.7 times theluminosity of the Sun from its enlargedphotosphere at aneffective temperature of4,849 K.[7] Based onasteroseismologic measurements, HD 210056 is estimated to be 2billion years old.[9] The star has about 90% of theSun'smetallicity — whatastronomers define a star's abundance ofchemical elements heavier thanhelium.[7] It currently spins slowly with aprojected rotational velocity lower than1.5 km/s.[9]

References

[edit]
  1. ^abcdVallenari, 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. ^abHøg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars".Astronomy and Astrophysics.355:L27 –L30.Bibcode:2000A&A...355L..27H.ISSN 0004-6361.
  3. ^Houk, N.; Cowley, A. P. (1975).University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations −90° to −53°.Bibcode:1975mcts.book.....H.
  4. ^abJohnson, H. L.; Mitchell, R. I.; Iriarte, B.; Wisniewski, W. Z. (1966). "UBVRIJKL Photometry of the Bright Stars".Communications of the Lunar and Planetary Laboratory.4:99–110.Bibcode:1966CoLPL...4...99J.
  5. ^abGontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system".Astronomy Letters.32 (11):759–771.arXiv:1606.08053.Bibcode:2006AstL...32..759G.doi:10.1134/S1063773706110065.eISSN 1562-6873.ISSN 1063-7737.S2CID 119231169.
  6. ^Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5):331–346.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015.eISSN 1562-6873.ISSN 1063-7737.S2CID 119257644.
  7. ^abcdOttoni, G.; Udry, S.; Ségransan, D.; Buldgen, G.; Lovis, C.; Eggenberger, P.; Pezzotti, C.; Adibekyan, V.; Marmier, M.; Mayor, M.; Santos, N. C.; Sousa, S. G.; Lagarde, N.; Charbonnel, C. (January 2022)."CORALIE radial-velocity search for companions around evolved stars (CASCADES): I. Sample definition and first results: Three new planets orbiting giant stars".Astronomy & Astrophysics.657: A87.arXiv:2201.01528.Bibcode:2022A&A...657A..87O.doi:10.1051/0004-6361/202040078.eISSN 1432-0746.ISSN 0004-6361.
  8. ^De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014)."A catalog of rotational and radial velocities for evolved stars".Astronomy & Astrophysics.561: A126.arXiv:1312.3474.Bibcode:2014A&A...561A.126D.doi:10.1051/0004-6361/201220762.eISSN 1432-0746.ISSN 0004-6361.
  9. ^abcAguirre, Víctor Silva; et al. (29 January 2020)."Detection and Characterization of Oscillating Red Giants: First Results from theTESS Satellite".The Astrophysical Journal.889 (2): L34.arXiv:1912.07604.Bibcode:2020ApJ...889L..34S.doi:10.3847/2041-8213/ab6443.eISSN 2041-8213.
  10. ^Gould, Benjamin Apthorp (1878). "Uranometria Argentina : brillantez y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral : con atlas".Resultados del Observatorio Nacional Argentino.1.Bibcode:1879RNAO....1.....G.
  11. ^"HD 210056".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedNovember 21, 2022.
  12. ^Eggen, O. J. (July 1993)."Evolved GK stars near the sun. I - The old disk population".The Astronomical Journal.106: 80.Bibcode:1993AJ....106...80E.doi:10.1086/116622.
  13. ^Gontcharov, George A.; Mosenkov, Aleksandr V. (28 September 2017)."Verifying reddening and extinction for Gaia DR1 TGAS main sequence stars".Monthly Notices of the Royal Astronomical Society.472 (4):3805–3820.arXiv:1709.01160.Bibcode:2017MNRAS.472.3805G.doi:10.1093/mnras/stx2219.eISSN 1365-2966.ISSN 0035-8711.
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