V345 Carinae

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V345 Carinae
V345CarLightCurve.png
A light curve for V345 Carinae, plotted from Hipparcos data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 09h 05m 38.37267s [2]
Declination −70° 32′ 18.5832″ [2]
Apparent magnitude  (V)+4.66 [3] (4.67 to 4.78) [4]
Characteristics
Spectral type B2(IV)n [5]
B−V color index −0.149±0.011 [3]
Variable type Be [6]
Astrometry
Radial velocity (Rv)+19.0±7.4 [3]  km/s
Proper motion (μ)RA: −3.017 [2]   mas/yr
Dec.: +8.394 [2]   mas/yr
Parallax (π)3.2440 ± 0.2602 [2]   mas
Distance 1,010 ± 80  ly
(310 ± 20  pc)
Absolute magnitude  (MV)−2.67 [3]
Details
Mass 9.6±0.3 [7]   M☉
Radius 8.70±0.17 [8]   R☉
Luminosity 2,539.73 [3]   L☉
Surface gravity (log g)3.80±0.04 [8]   cgs
Temperature 19,000±190 [8]   K
Rotational velocity (v sin i)140±3 [8]  km/s
Age 20.4±2.3 [7]   Myr
Other designations
E Car, V345 Car, CPD−70°861, GC  12602, HD  78764, HIP  44626, HR  3642, SAO  256583 [9]
Database references
SIMBAD data

V345 Carinae is a star in the constellation Carina. It has the Bayer designation E Carinae; V345 Carinae is the variable star designation. The star has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.66. [3] Its actual brightness varies from magnitude +4.67 to +4.78 with a period of 137.7 days. [4] Based on parallax measurements, it is located at a distance of approximately 1,010  light years from the Sun. [2] It is drifting further away with a radial velocity of around +19 km/s. [3]

This star has a stellar classification of B2(IV)n, [5] matching a suspected B-type subgiant star. The 'n' notation indicates "nebulous" lines caused by rapid rotation: the star is spinning with a projected rotational velocity of 140 km/s. [8] It is a Be star having a circumstellar disk of hot, decreted gas that is inserting emission lines into the spectrum. [6] The star is 20 [7]  million years old with 9.6 [7] times the mass of the Sun and 8.7 [8] times the Sun's radius. It is radiating 2,540 [3] times the luminosity of the Sun from its photosphere at an effective temperature of 19,000 K. [8]

The star displays a complex luminosity variation with a periods of 1.13028 and 137.7 days. Although thought to be a single star, [10] Carrier et al. (2002) suggested the longer period may be caused by some sort of binary interaction with the circumstellar disk or perhaps a light reflecting effect. However, no companion has been detected via radial velocity variations. This suggests that the companion would need to either have less than 1.7 times the mass of the Sun or it is being viewed from nearly pole-on. [11] The short-term variations may be from non-radial pulsations similar to those of ω CMa. [12]

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V1073 Scorpii Variable star in the constellation Scorpius

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References

  1. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. 1 2 3 4 5 6 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  3. 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.
  4. 1 2 "V345 Carinae", Variable Star Index, retrieved 2020-02-19.
  5. 1 2 Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
  6. 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.
  7. 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.
  8. 1 2 3 4 5 6 7 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. ↑ "E Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-02-18.
  10. ↑ 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.
  11. ↑ Carrier, F.; et al. (April 2002), "Search for duplicity in periodic variable Be stars", Astronomy and Astrophysics, 385 (2): 488–502, Bibcode:2002A&A...385..488C, doi: 10.1051/0004-6361:20020174 .
  12. ↑ Rivinius, Th.; et al. (November 2003), "Non-radially pulsating Be stars", Astronomy and Astrophysics, 411 (2): 229–247, Bibcode:2003A&A...411..229R, doi: 10.1051/0004-6361:20031285 .
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