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V344 Carinae

From Wikipedia, the free encyclopedia

V344 Carinae

A light curve for V344 Carinae, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Carina
Right ascension 08h 46m 42.54928s[2]
Declination −56° 46′ 11.1922″[2]
Apparent magnitude (V) 4.50[3] (4.40–4.51)[4]
Characteristics
Spectral type B3V(n)[5]
B−V color index −0.169±0.008[3]
Variable type Be[6]
Astrometry
Radial velocity (Rv)+27.0±7.4[3] km/s
Proper motion (μ) RA: −9.29[2] mas/yr
Dec.: +8.85[2] mas/yr
Parallax (π)5.39 ± 0.14 mas[2]
Distance610 ± 20 ly
(186 ± 5 pc)
Absolute magnitude (MV)−1.84[3]
Details
Mass7.1±0.1[7] M☉
Radius3.00±0.06[8] R☉
Luminosity2,328+120
−105[9] L☉
Surface gravity (log g)3.79±0.18[9] cgs
Temperature17,660±560[9] K
Rotational velocity (v sin i)268±18[9] km/s
Age31.6±3.9[7] Myr
Other designations
f Car, V344 Car, CPD−56°1865, FK5 2695, GC 12138, HD 75311, HIP 43105, HR 3498, SAO 236268[10]
Database references
SIMBADdata

V344 Carinae is a single[11] star in the southern constellation of Carina. It has the Bayer designation f Carinae, while V344 Carinae is its variable star designation. This star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 4.50.[3] Historically, it was mentioned in the Almagest, suggesting that some time around 130 BCE it was brighter than its current magnitude.[12] This object is located at a distance of approximately 610 light-years from the Sun based on parallax.[2] The star is drifting further away with a radial velocity of around +27 km/s.[3]

This is a B-type main-sequence star with a stellar classification of B3V(n).[5] It is a Be star; a rapidly rotating star that is hosting a circumstellar disk of hot, decreted gas.[13] It is a photometrically variable Be star, having a brightness that ranges from 4.4 down to 4.51 in visual magnitude, and has been classified as a Gamma Cassiopeiae variable.[4] The star is 32[7] million years old and is spinning with a projected rotational velocity of 268 km/s.[9] It has seven[7] times the mass of the Sun and around 3.0[8] times the Sun's radius. The star is radiating 2,328[9] times the luminosity of the Sun from its photosphere at an effective temperature of 17,660 K.[9]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  3. ^ a b c d e f 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.
  4. ^ a b "V344 Carinae", Variable Star Index, retrieved 2020-02-19.
  5. ^ a b Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  6. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
  7. ^ a b c d Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  8. ^ a b Arcos, C.; et al. (March 2018), "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey", Monthly Notices of the Royal Astronomical Society, 474 (4): 5287–5299, arXiv:1711.08675, Bibcode:2018MNRAS.474.5287A, doi:10.1093/mnras/stx3075, S2CID 74872624.
  9. ^ a b c d e f g Zorec, J.; et al. (November 2016), "Critical study of the distribution of rotational velocities of Be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity", Astronomy & Astrophysics, 595: 26, Bibcode:2016A&A...595A.132Z, doi:10.1051/0004-6361/201628760, hdl:11336/37946.
  10. ^ "f Car". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 19 March 2016.
  11. ^ Eggleton, P. P.; Tokovinin, A. A. (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, S2CID 14878976.
  12. ^ Hertzog, K. P. (August 1984), "Supernova progenitors and Be stars : stellar variability from a 21 century perspective", Monthly Notices of the Royal Astronomical Society, 209 (3): 533–541, Bibcode:1984MNRAS.209..533H, doi:10.1093/mnras/209.3.533.
  13. ^ Touhami, Y.; et al. (March 2011), "The Infrared Continuum Sizes of Be Star Disks", The Astrophysical Journal, 729 (1): 8, arXiv:1101.1698, Bibcode:2011ApJ...729...17T, doi:10.1088/0004-637X/729/1/17, S2CID 119294318, 17.
This page was last edited on 15 January 2024, at 07:41
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