V343 Carinae

Last updated
V343 Carinae
Carina constellation map.svg
Red circle.svg
Location of V343 Carinae (circled in red)
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 08h 40m 37.02758s [1]
Declination −59° 45′ 39.6067″ [1]
Apparent magnitude  (V)4.31 [2]
Characteristics
Spectral type B1.5III [3]
B−V color index −0.117±0.005 [2]
Variable type Constant [4]
Astrometry
Radial velocity (Rv)+12.9±0.7 [2] km/s
Proper motion (μ)RA: −6.63 [1] mas/yr
Dec.: +5.32 [1] mas/yr
Parallax (π)2.26±0.11  mas [1]
Distance 1,440 ± 70  ly
(440 ± 20  pc)
Absolute magnitude  (MV)−3.91 [2]
Details
Mass 12.5±0.6 [5]   M☉
Luminosity 6,322.92 [2]   L☉
Temperature 27,600±3,630 [6]   K
Age 15.7±0.1 [5]   Myr
Other designations
d Car, V343 Car, CPD−59°1080, FK5 2685, GC 11964, HD 74375, HIP 42568, HR 3457, SAO 236181, CCDM J08406-5946, WDS J08406-5946A [7]
Database references
SIMBAD data

V343 Carinae is a blue-white star or star system in the southern constellation of Carina. It has the Bayer designation d Carinae, while V343 Carinae is a variable star designation. The star is visible to the naked eye with an apparent visual magnitude of 4.31. [2] The distance to this object is approximately 1,440  light years based on parallax. It is drifting further away with a radial velocity of +13 km/s. [2]

A light curve for V343 Carinae, plotted from TESS data V343CarLightCurve.png
A light curve for V343 Carinae, plotted from TESS data

This star was originally thought to be a Beta Cephei variable and a suspected eclipsing binary [9] with an orbital period of 133.92 days. It is now considered as probably constant. [10] [4] Measurements indicate that at most it is a microvariable star with an amplitude of 0.0041 in visual magnitude and a period of 0.42029 cycles per day. [11] Eggleton and Tokovinin (2008) catalogued this as a single star, albeit with some uncertainty. [12] However, Chini et al. (2012) listed it as a single-lined spectroscopic binary system. [13]

The visible component of V343 Carinae has a stellar classification of B1.5III, [3] matching a massive blue giant. It has 12.5 [5] times the mass of the Sun and is an estimated 16 [5]  million years old. The star is radiating 6,323 [2] times the Sun's luminosity from its photosphere at an effective temperature of 27,600 K. [6] It has a visual magnitude 13.3 companion at an angular separation of 16.4″ along a position angle of 339°, as of 2010. [14]

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 4 5 6 7 8 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.
  3. 1 2 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.
  4. 1 2 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.
  5. 1 2 3 4 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.
  6. 1 2 Sokolov, N. A. (May 1995), "The determination of Teff of B, A and F main sequence stars from the continuum between 3200 A and 3600 A.", Astronomy and Astrophysics Supplement, 110: 553, Bibcode:1995A&AS..110..553S.
  7. ↑ "d Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 19 March 2016.
  8. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  9. ↑ van Hoof, A. (June 1973), "Six New Variable B-Stars", Information Bulletin on Variable Stars, 807: 1, Bibcode:1973IBVS..807....1V.
  10. ↑ Waelkens, C.; Rufener, F. (May 1983), "An observational study of the influence of close companions on the pulsations of beta Cephei stars", Astronomy and Astrophysics, 121: 45–50, Bibcode:1983A&A...121...45W.
  11. ↑ Koen, Chris; Eyer, Laurent (March 2002), "New periodic variables from the Hipparcos epoch photometry", Monthly Notices of the Royal Astronomical Society, 331 (1): 45–59, arXiv: astro-ph/0112194 , Bibcode:2002MNRAS.331...45K, doi: 10.1046/j.1365-8711.2002.05150.x , S2CID   10505995.
  12. ↑ 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.
  13. ↑ Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv: 1205.5238 , Bibcode:2012MNRAS.424.1925C, doi: 10.1111/j.1365-2966.2012.21317.x , S2CID   119120749.
  14. ↑ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 .
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.