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Omega Octantis

From Wikipedia, the free encyclopedia
Star in the constellation of Octans
ω Octantis
Location of ω Oct (circled)
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationOctans
Right ascension15h 11m 08.79214s[1]
Declination−84° 47′ 16.0295″[1]
Apparent magnitude (V)5.87±0.01[2]
Characteristics
Evolutionary stagemain sequence[3]
Spectral typeB9.5 V[4]
U−Bcolor index−0.13[5]
B−Vcolor index−0.06[5]
Astrometry
Radial velocity (Rv)−7.6±3[6] km/s
Proper motion (μ)RA: +2.984mas/yr[1]
Dec.: −9.385mas/yr[1]
Parallax (π)9.9406±0.0591 mas[1]
Distance328 ± 2 ly
(100.6 ± 0.6 pc)
Absolute magnitude (MV)+0.94[7]
Details
Mass2.54[3] M
Radius2.35±0.06[8] R
Luminosity50.5+2.5
−2.4
[3] L
Surface gravity (log g)4.21[9] cgs
Temperature10,759±366[9] K
Metallicity [Fe/H]0.00[10] dex
Rotational velocity (v sin i)36[11] km/s
Age197[9] Myr
Other designations
ω Oct,23 G. Octantis[12],CPD−84°490,GC 20223,HD 131596,HIP 74296,HR 5557,SAO 258717[13]
Database references
SIMBADdata

Omega Octantis, (latinized fromω Octantis), is a solitary,[14] bluish-white huedstar located in the southerncircumpolar constellationOctans. It has anapparent magnitude of 5.87,[2] allowing it to be faintly seen with thenaked eye. Based on the object'sparallax measurements, it is estimated to be 328light years distant.[1] However, it is drifting closer with a heliocentricradial velocity−7.6 km/s.[6]

Omega Octantis has astellar classification of B9.5 V,[4] indicating that it is amain-sequence star between the B9 and A0 classes.Helmut A. Abt &Nidia I. Morrell gave a slightly updated class of B9.5 Vs,[15] which includes sharp (narrow)absorption lines in Omega Octantis'spectrum due to slow rotation. It has amass 2.54 times that of theSun[3] and is calculated to be 197million years old,[9] having completed 40% of itsmain sequence lifetime.[3] It has aluminosity of 50.5 L,[3] which comes from aradius of 2.35 R and aneffective temperature of10,759 K. In 2012, George A. Gontcharov calculated a solarmetallicity for Omega Octantis,[10] and it is spinning modestly with aprojected rotational velocity of36 km/s.[11] The slow rotation is consistent with the spectral classification from Abt & Morell (1995).[15]

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. ^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. ^abcdefZorec, J.; Royer, F. (January 2012)."Rotational velocities of A-type stars. IV. Evolution of rotational velocities".Astronomy and Astrophysics.537: A120.arXiv:1201.2052.Bibcode:2012A&A...537A.120Z.doi:10.1051/0004-6361/201117691.ISSN 0004-6361.S2CID 55586789.
  4. ^abHouk, 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.
  5. ^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.
  6. ^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.
  7. ^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.
  8. ^Stassun, 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. ^abcdDavid, Trevor J.; Hillenbrand, Lynne A. (12 May 2015)."The Ages of Early-type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets".The Astrophysical Journal.804 (2): 146.arXiv:1501.03154.Bibcode:2015ApJ...804..146D.doi:10.1088/0004-637X/804/2/146.eISSN 1538-4357.
  10. ^abGontcharov, G. A. (December 2012). "Dependence of kinematics on the age of stars in the solar neighborhood".Astronomy Letters.38 (12):771–782.arXiv:1606.08814.Bibcode:2012AstL...38..771G.doi:10.1134/S1063773712120031.ISSN 0320-0108.S2CID 118345778.
  11. ^abLevato, H.; Grosso, M. (June 2004). "New Projected Rotational Velocities of All Southern B-type Stars of the Bright Star Catalogue".Astronomical Society of the Pacific.215: 51.Bibcode:2004IAUS..215...51L.
  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. ^"Omega Oct".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedAugust 21, 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.
  15. ^abAbt, Helmut A.; Morrell, Nidia I. (July 1995)."The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars".The Astrophysical Journal Supplement Series.99: 135.Bibcode:1995ApJS...99..135A.doi:10.1086/192182.ISSN 0067-0049.
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