Movatterモバイル変換

[0]ホーム
URL:

Jump to content
WikipediaThe Free Encyclopedia
Search

V399 Carinae

From Wikipedia, the free encyclopedia
Star in the constellation Carina
This article is about P Carinae. For p Carinae, seePP Carinae.
V399 Carinae
Location of V399 Carinae (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationCarina
Right ascension10h 27m 24.47049s[1]
Declination−57° 38′ 19.6984″[1]
Apparent magnitude (V)+4.63 to +4.72[2]
Characteristics
Spectral typeA5Iae[3] or F0Ia[4]
U−Bcolor index+0.22[5]
B−Vcolor index+0.46[5]
Variable typeSRd?[2]
Astrometry
Proper motion (μ)RA: −7.377[1]mas/yr
Dec.: +3.688[1]mas/yr
Parallax (π)0.4976±0.1151 mas[1]
Distanceapprox. 7,000 ly
(approx. 2,000 pc)
Absolute magnitude (MV)−8.8[6]
Details
Mass22.6[7] M☉
Radius206[8] R☉
Luminosity73,000[9] L☉
Surface gravity (log g)1.00[10] cgs
Temperature8,000[11] K
Metallicity [Fe/H]−0.06[10] dex
Age12[12] Myr
Other designations
P Carinae,[13]195 G. Carinae,[14]HR 4110,HD 90772,CP−57°3256,HIP 51192,SAO 238077,GC 14373,IC 2581 1
Database references
SIMBADdata

V399 Carinae (V399 Car,P Carinae, P Car, 195 G. Carinae) is avariable star in theconstellationCarina. It is visible to thenaked eye.

Thespectral type of V399 Carinae has been variously assigned between A5 and F0,[15] being a bright,luminous supergiant.[16] Itsspectrum is described as having a non-photospheric continuum and siliconabsorption lines, indicative of high mass loss.[17]

Avisual bandlight curve for V399 Carinae, adapted from Berdnikov and Turner (1997)[6]

V399 Carinae has long been suspected to be variable.[18] A 1981 study of yellow supergiants fit observations to a Cepheid-like light curve with a period of 58.8 days, although the luminosity and spectral type do not place the star near the Cepheidinstability strip.[15] It was listed in theGeneral Catalogue of Variable Stars as a possibleδ Cep variable.[19] Further observations refined the period to 47.25 days.[6] TheHipparcos catalogue classified V399 Car as asemiregular variable with a period of 88 days and a mean amplitude of only 0.04 magnitudes.[20] An automated classification from Hipparos photometry suggested it is anα Cygni variable.[21] The observed brightness varies from magnitude +4.63 to +4.72.[2]

V399 Carinae lies amongst the stars of theopen cluster IC 2581, by far the brightest member of the cluster. It is about 7,500 light years fromEarth assuming it is a member of IC 2581, which is given a 62.9% probability.[22] Itsangular diameter has been estimated at0.954±0.09 milliarcseconds,[23] which, at the estimated distance of 2009parsecs,[1] gives it a radius 206 times thesolar radius.[8]

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. ^abcWatson, C. L. (2006). "The International Variable Star Index (VSX)".The Society for Astronomical Sciences 25th Annual Symposium on Telescope Science. Held May 23–25.25: 47.Bibcode:2006SASS...25...47W.
  3. ^Gray, R. O.; Garrison, R. F. (1989)."The late A-type stars - Refined MK classification, confrontation with Stromgren photometry, and the effects of rotation".Astrophysical Journal Supplement Series.70: 623.Bibcode:1989ApJS...70..623G.doi:10.1086/191349.
  4. ^Dambis, A. K. (February 2013)."Revisiting the absolute-magnitude calibration of F-type supergiants and bright giants as a function of the equivalent width of the OIλ7774Å triplet".Proceedings of the International Astronomical Union.289: 379−381.Bibcode:2013IAUS..289..379D.doi:10.1017/S1743921312021758.
  5. ^abSchild, R. E.; Garrison, R. F.; Hiltner, W. A. (1983). "UBV photometry for southern OB stars".Astrophysical Journal Supplement Series.51: 321.Bibcode:1983ApJS...51..321S.doi:10.1086/190852.
  6. ^abcBerdnikov, L. N.; Turner, D. G. (1997). "Photoelectric VIc and New Elements for V399 Carinae = HR 4110".Information Bulletin on Variable Stars.4456: 1.Bibcode:1997IBVS.4456....1B.
  7. ^Kervella, 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.
  8. ^abLang, Kenneth R. (2006),Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3 ed.),Birkhäuser,ISBN 978-3-540-29692-8. The radius (R*) is given by:
    2⋅R∗=(2009⋅0.954⋅10−3) UA0.0046491 UA/R⨀≈412.25⋅R⨀{\displaystyle {\begin{aligned}2\cdot R_{*}&={\frac {(2009\cdot 0.954\cdot 10^{-3})\ {\text{UA}}}{0.0046491\ {\text{UA}}/R_{\bigodot }}}\\&\approx 412.25\cdot R_{\bigodot }\end{aligned}}}
  9. ^Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015.S2CID 119257644.
  10. ^abLuck, R. Earle (2014)."Parameters and Abundances in Luminous Stars".The Astronomical Journal.147 (6): 137.Bibcode:2014AJ....147..137L.doi:10.1088/0004-6256/147/6/137.
  11. ^Rest, A.; Prieto, J. L.; Walborn, N. R.; Smith, N.; Bianco, F. B.; Chornock, R.; Welch, D. L.; Howell, D. A.; Huber, M. E.; Foley, R. J.; Fong, W.; Sinnott, B.; Bond, H. E.; Smith, R. C.; Toledo, I.; Minniti, D.; Mandel, K. (2012). "Light echoes reveal an unexpectedly cool η Carinae during its nineteenth-century Great Eruption".Nature.482 (7385):375–8.arXiv:1112.2210.Bibcode:2012Natur.482..375R.doi:10.1038/nature10775.PMID 22337057.S2CID 205227548.
  12. ^Luck, R. Earle (1994). "Open cluster chemical composition. 1: Later type stars in eight clusters".Astrophysical Journal Supplement Series.91: 309.Bibcode:1994ApJS...91..309L.doi:10.1086/191940.
  13. ^Kostjuk, N. D. (2004). "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)".VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002).4027.Bibcode:2004yCat.4027....0K.
  14. ^Benjamin Apthorp Gould (1879).Uranometria Argentina: Brightness and Position of Every Fixed Star, Down to the Seventh Magnitude, Within One Hundred Degrees of the South Pole. Coni. pp. 159–.
  15. ^abArellano Ferro, A. (1981)."A survey of variable yellow supergiants in the southern Milky Way".Astronomical Society of the Pacific.93: 351.Bibcode:1981PASP...93..351A.doi:10.1086/130837.S2CID 250812474.
  16. ^Evans, L.; Francis, Ch. (1969)."The open cluster IC 2581".Monthly Notices of the Royal Astronomical Society.146 (5): 101.Bibcode:1969MNRAS.146..101L.doi:10.1093/mnras/146.2.101.
  17. ^Ardila, David R.; Van Dyk, Schuyler D.; Makowiecki, Wojciech; Stauffer, John; Song, Inseok; Rho, Jeonghee; Fajardo-Acosta, Sergio; Hoard, D. W.; Wachter, Stefanie (2010)."The Spitzer Atlas of Stellar Spectra (SASS)".The Astrophysical Journal Supplement.191 (2): 301.Bibcode:2010ApJS..191..301A.doi:10.1088/0067-0049/191/2/301.S2CID 22689941.
  18. ^Arp, H. C. (1958)."Southern hemisphere photometry II Photoelectric measures of bright stars".Astronomical Journal.63: 118.Bibcode:1958AJ.....63..118A.doi:10.1086/107703.
  19. ^Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Perova, N. B. (1985). "The 67th Name-List of Variable Stars".Information Bulletin on Variable Stars.2681: 1.Bibcode:1985IBVS.2681....1K.
  20. ^Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; Hoeg, E.; Bastian, U.; Bernacca, P. L.; Crézé, M.; Donati, F.; Grenon, M.; Grewing, M.; Van Leeuwen, F.; Van Der Marel, H.; Mignard, F.; Murray, C. A.; Le Poole, R. S.; Schrijver, H.; Turon, C.; Arenou, F.; Froeschlé, M.; Petersen, C. S. (1997). "The HIPPARCOS Catalogue".Astronomy and Astrophysics.323: L49.Bibcode:1997A&A...323L..49P.
  21. ^Dubath, 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. (2011)."Random forest automated supervised classification of Hipparcos periodic variable stars".Monthly Notices of the Royal Astronomical Society.414 (3): 2602.arXiv:1101.2406.Bibcode:2011MNRAS.414.2602D.doi:10.1111/j.1365-2966.2011.18575.x.S2CID 118560311.
  22. ^Baumgardt, H.; Detbarn, C.; Wielen, R. (2000). "Absolute proper motions of open clusters. I. Observational data".Astronomy and Astrophysics Supplement.146 (2): 251.arXiv:astro-ph/0010306.Bibcode:2000A&AS..146..251B.doi:10.1051/aas:2000362.S2CID 7180188.
  23. ^Cruzalèbes, P.; Petrov, R. G.; Robbe-Dubois, S.; Varga, J.; Burtscher, L.; Allouche, F.; Berio, P.; Hofmann, K. -H.; Hron, J.; Jaffe, W.; Lagarde, S.; Lopez, B.; Matter, A.; Meilland, A.; Meisenheimer, K. (2019-12-01)."A catalogue of stellar diameters and fluxes for mid-infrared interferometry".Monthly Notices of the Royal Astronomical Society.490 (3):3158–3176.arXiv:1910.00542.Bibcode:2019MNRAS.490.3158C.doi:10.1093/mnras/stz2803.ISSN 0035-8711.
Stars
Bayer
Variable
HR
HD
Other
Exoplanets
Star
clusters
NGC
Other
Nebulae
NGC
Other
Galaxies
NGC
Other
Galaxy clusters
Astronomical events
Retrieved from "https://en.wikipedia.org/w/index.php?title=V399_Carinae&oldid=1264439115"
Categories:
Hidden categories:
[8]ページ先頭
©2009-2025 Movatter.jp