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HD 86267

From Wikipedia, the free encyclopedia
Star in the constellation of Antlia
HD 86267
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationAntlia
Right ascension09h 56m 35.4937s[1]
Declination−33° 25′ 06.587″[1]
Apparent magnitude (V)5.82±0.01[2]
Characteristics
Evolutionary stageRGB[1]
Spectral typeK1 III[3]
B−Vcolor index+1.2[4]
Astrometry
Radial velocity (Rv)3.7±0.4[5] km/s
Proper motion (μ)RA: +34.064mas/yr[1]
Dec.: +22.102mas/yr[1]
Parallax (π)6.3494±0.0453 mas[1]
Distance514 ± 4 ly
(157 ± 1 pc)
Absolute magnitude (MV)−0.15[6]
Details
Mass1.73+1.24
−0.71
[7] M
Radius19.7[8] R
Luminosity158±11[7] L
Surface gravity (log g)1.86[9] cgs
Temperature4430±110[7] K
Metallicity [Fe/H]−0.15[10] dex
Rotational velocity (v sin i)<1[11] km/s
Other designations
36 G. Antliae[12],CD−32°6895,CPD−32°2771,FK5 2796,GC 13695,HD 86267,HIP 48748,HR 3932,SAO 200889[13]
Database references
SIMBADdata

HD 86267, also known asHR 3932, is a solitary[14] orange-huedstar located in the southernconstellationAntlia. It has anapparent magnitude of 5.82,[2] allowing it to be faintly seen with thenaked eye.Parallax measurements place it a distance of 514light years[1] and it is currently receding with a heliocentricradial velocity of3.7 km/s.[5]

HD 86267 has astellar classification of K1 III,[3] indicating that it is ared giant. At present it has 1.73 times themass of the Sun[7] but has expanded to 19.7 times its girth.[8] It shines with aluminosity of158 L from its enlargedphotosphere at aneffective temperature of4,430 K.[7] It is a member of the old disk population, having ametallicity 71% that of theSun.[10] The value means that it is metal deficient. Its currentrotation rate is too low to be measured accurately.[11]

References

[edit]
  1. ^abcdefVallenari, 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. ^abHouk, N. (1982).Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Volume_3. Declinations −40° to −26°.Bibcode:1982mcts.book.....H.
  4. ^Johnson, 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 255204555.
  7. ^abcdeCharbonnel, C.; Lagarde, N.; Jasniewicz, G.; North, P. L.; Shetrone, M.; Krugler Hollek, J.; Smith, V. V.; Smiljanic, R.; Palacios, A.; Ottoni, G. (January 2020)."Lithium in red giant stars: Constraining non-standard mixing with large surveys in theGaia era".Astronomy & Astrophysics.633: A34.arXiv:1910.12732.Bibcode:2020A&A...633A..34C.doi:10.1051/0004-6361/201936360.eISSN 1432-0746.ISSN 0004-6361.
  8. ^abStassun, Keivan G.; et al. (9 September 2019)."The RevisedTESS Input Catalog and Candidate Target List".The Astronomical Journal.158 (4): 138.arXiv:1905.10694.Bibcode:2019AJ....158..138S.doi:10.3847/1538-3881/ab3467.eISSN 1538-3881.
  9. ^Anders, F.; et al. (August 2019)."Photo-astrometric distances, extinctions, and astrophysical parameters forGaia DR2 stars brighter thanG = 18".Astronomy & Astrophysics.628: A94.arXiv:1904.11302.Bibcode:2019A&A...628A..94A.doi:10.1051/0004-6361/201935765.eISSN 1432-0746.ISSN 0004-6361.
  10. ^abEggen, Olin J. (April 1989)."Large and kinematically unbiased samples of G- and K-type stars. IV - Evolved stars of the old disk population".Publications of the Astronomical Society of the Pacific.101: 366.Bibcode:1989PASP..101..366E.doi:10.1086/132442.eISSN 1538-3873.ISSN 0004-6280.
  11. ^abDe 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: V. Southern stars⋆⋆⋆".Astronomy & Astrophysics.561: A126.arXiv:1312.3474.Bibcode:2014A&A...561A.126D.doi:10.1051/0004-6361/201220762.ISSN 0004-6361.
  12. ^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.
  13. ^"HR 3932".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved4 August 2022.
  14. ^Eggleton, P. P.; Tokovinin, A. A. (11 September 2008)."A catalogue of multiplicity among bright stellar systems".Monthly Notices of the Royal Astronomical Society.389 (2):869–879.arXiv:0806.2878.Bibcode:2008MNRAS.389..869E.doi:10.1111/j.1365-2966.2008.13596.x.eISSN 1365-2966.ISSN 0035-8711.
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