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WZ Columbae

From Wikipedia, the free encyclopedia
Star in the constellation of Columba
WZ Columbae

Alight curve for WZ Columbae, plotted fromTESS data[1]
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationColumba
Right ascension05h 42m 15.19447s[2]
Declination−34° 40′ 04.1399″[2]
Apparent magnitude (V)5.28±0.01[3]
Characteristics
Evolutionary stagemain sequence[4]
Spectral typeB9/9.5 V[5]
B−Vcolor index−0.05[6]
Variable typeSPB[7] orα2 CVn[8]
Astrometry
Radial velocity (Rv)36.3±0.6[9] km/s
Proper motion (μ)RA: +5.081mas/yr[2]
Dec.: +51.365mas/yr[2]
Parallax (π)8.929±0.08896 mas[2]
Distance365 ± 4 ly
(112 ± 1 pc)
Absolute magnitude (MV)−0.3[10]
Details
Mass3.07±0.05[4] M
Radius3.47[11] R
Luminosity124[12] L
Surface gravity (log g)3.79±0.07[13] cgs
Temperature10,000+256
−250
[4] K
Metallicity [Fe/H]+0.51[14] dex
Rotational velocity (v sin i)65±5[15] km/s
Age394+10
−17
[16] Myr
Other designations
42 G. Columbae[17],WZ Col,CD−34°2401,CPD−34°711,GC 7150,HD 38170,HIP 26868,HR 1973,SAO 196098[18]
Database references
SIMBADdata

WZ Columbae, also known asHD 38170, is a solitary,[19] bluish-white huedstar located in the southernconstellationColumba, the dove. It has anapparent magnitude of 5.28,[3] allowing it to be faintly visible to thenaked eye. Based onparallax measurements from theGaia spacecraft, the object is about 365light years distant.[2] It appears to be receding from theSolar System, having a heliocentricradial velocity of36.3 km/s.[9]

The star was discovered to be avariable star when theHipparcos data was analyzed. It was given itsvariable star designation in 1999.[20] WZ Columbae was originally listed as aslowly pulsating B-type star by theGeneral Catalogue of Variable Stars. However, observations from Hempel & Howlger (2003) reveal it to be overabundant instrontium andbarium.[14] Combined with Hipparcos photometry, this led to the object being reclassified as anAlpha2 Canum Venaticorum variable.[8] Based on data collected in theHipparcos passband, it fluctuates betweenmagnitudes 5.27 and 5.29 over 1.38days.[7][21] However,TESS data suggests a period of2.76618±0.00004 days; double that of the earlier data.[16]

Thestellar classification of WZ Columbae is B9/9.5 V[5] — amain-sequence star with the characteristics of a B9 and B9.5 star. It has 3.07[4] times themass of the Sun and is estimated to be 394million years old,[16] having completed 89.2% of itsmain sequence lifetime.[4] It has a slightly enlargedradius of 3.47 R[11] and aneffective temperature of10,000 K.[4] This yields aluminosity 124 times that of theSun[12] from itsphotosphere. Like mostchemically peculiar stars, WZ Columbae has a relatively slowprojected rotational velocity at65 km/s.[15]

References

[edit]
  1. ^"MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved15 September 2022.
  2. ^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.
  3. ^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.
  4. ^abcdefZorec, J.; Royer, F. (January 2012)."Rotational velocities of A-type stars".Astronomy & Astrophysics.537: A120.arXiv:1201.2052.Bibcode:2012A&A...537A.120Z.doi:10.1051/0004-6361/201117691.eISSN 1432-0746.ISSN 0004-6361.
  5. ^abHouk, N. (1982).Michigan Catalogue of Two-dimensional Spectral Types for the HD stars III: Declinations −40° to −26°.Bibcode:1982mcts.book.....H.
  6. ^Stoy, R. H. (1968). "Photoelectric Magnitudes and Colours for Bright Southern Stars".Monthly Notes of the Astronomical Society of South Africa.27: 119.Bibcode:1968MNSSA..27..119S.ISSN 0024-8266.
  7. ^abSamus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1".Astronomy Reports.61 (1):80–88.Bibcode:2017ARep...61...80S.doi:10.1134/S1063772917010085.eISSN 1562-6881.ISSN 1063-7729.S2CID 125853869.
  8. ^abDubath, P.; Rimoldini, L.; Süveges, M.; Blomme, J.; López, M.; Sarro, L. M.; De Ridder, J.; Cuypers, J.; Guy, L.; Lecoeur, I.; Nienartowicz, K.; Jan, A.; Beck, M.; Mowlavi, N.; De Cat, P.; Lebzelter, T.; Eyer, L. (9 May 2011)."Random forest automated supervised classification of Hipparcos periodic variable stars".Monthly Notices of the Royal Astronomical Society.414 (3):2602–2617.arXiv:1101.2406.Bibcode:2011MNRAS.414.2602D.doi:10.1111/j.1365-2966.2011.18575.x.ISSN 0035-8711.
  9. ^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.
  10. ^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.
  11. ^abKervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022)."Stellar and substellar companions fromGaia EDR3".Astronomy & Astrophysics.657: A7.arXiv:2109.10912.Bibcode:2022A&A...657A...7K.doi:10.1051/0004-6361/202142146.eISSN 1432-0746.ISSN 0004-6361.
  12. ^abMcDonald, I.; Zijlstra, A. A.; Watson, R. A. (15 June 2017)."Fundamental parameters and infrared excesses of Tycho–Gaia stars".Monthly Notices of the Royal Astronomical Society.471 (1):770–791.arXiv:1706.02208.Bibcode:2017MNRAS.471..770M.doi:10.1093/mnras/stx1433.eISSN 1365-2966.ISSN 0035-8711.
  13. ^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.
  14. ^abHempel, M.; Holweger, H. (September 2003)."Abundance analysis of late B stars".Astronomy & Astrophysics.408 (3):1065–1076.Bibcode:2003A&A...408.1065H.doi:10.1051/0004-6361:20030889.eISSN 1432-0746.ISSN 0004-6361.
  15. ^abRoyer, F.; Gerbaldi, M.; Faraggiana, R.; Gómez, A. E. (January 2002)."Rotational velocities of A-type stars".Astronomy & Astrophysics.381 (1):105–121.arXiv:astro-ph/0110490.Bibcode:2002A&A...381..105R.doi:10.1051/0004-6361:20011422.eISSN 1432-0746.ISSN 0004-6361.
  16. ^abcDavid-Uraz, A; Shultz, M E; Petit, V; Bowman, D M; Erba, C; Fine, R A; Neiner, C; Pablo, H; Sikora, J; ud-Doula, A; Wade, G A (1 April 2021)."MOBSTER – IV. Detection of a new magnetic B-type star from follow-up spectropolarimetric observations of photometrically selected candidates★".Monthly Notices of the Royal Astronomical Society.504 (4):4841–4849.arXiv:2004.09698.Bibcode:2021MNRAS.504.4841D.doi:10.1093/mnras/stab899.eISSN 1365-2966.ISSN 0035-8711.
  17. ^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.
  18. ^"WZ Columbae".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedSeptember 7, 2022.
  19. ^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.
  20. ^Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (January 1999)."The 74th Special Name-list of Variable Stars"(PDF).Information Bulletin on Variable Stars.4659:1–27.Bibcode:1999IBVS.4659....1K. Retrieved27 January 2025.
  21. ^"WZ Col".The International Variable Star Index. American Association of Variable Star Observers. Retrieved2022-09-16.
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