V344 Carinae

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V344 Carinae
V344CarLightCurve.png
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]
Distance 610 ± 20  ly
(186 ± 5  pc)
Absolute magnitude  (MV)−1.84 [3]
Details
Mass 7.1±0.1 [7]   M☉
Radius 3.00±0.06 [8]   R☉
Luminosity 2,328+120
−105 [9]   L☉
Surface gravity (log g)3.79±0.18 [9]   cgs
Temperature 17,660±560 [9]   K
Rotational velocity (v sin i)268±18 [9]  km/s
Age 31.6±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
SIMBAD data

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] In 1951, Alan William James Cousins announced his discovery that the star, then known as f Carinae, is a photometrically variable star. [14] It was given its variable star designation in 1975. [15] Its brightness ranges from 4.4 down to 4.51 in visual magnitude, and it 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]

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HD 90853 is a single star in the southern constellation Carina. It has the Bayer designation s Carinae, while HD 90853 is the identifier from the Henry Draper catalogue. This is a variable star with an apparent visual magnitude that ranges from 3.36 down to 3.51, and thus is bright enough to be visible to the naked eye. It is located at a distance of approximately 1,340 light-years from the Sun based on parallax, and has an absolute magnitude of −4.44. The star is drifting further away with a radial velocity of +9 km/s.

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<span class="mw-page-title-main">V343 Carinae</span> Star in the constellation Carina

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. 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.

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HD 91942 is a single variable star in the constellation Carina. It has the Bayer designation r Carinae, while HD 91942 is the identifier from the Henry Draper catalogue. This orange-hued object is visible to the naked eye with an apparent visual magnitude of 4.45. Based on parallax measurements, it is located at a distance of approximately 1,180 light years from the Sun. The star has an absolute magnitude of −3.77, and is drifting further away with a radial velocity of +9.9 km/s.

HD 83944 is a star system in the constellation Carina. This has the Bayer designation m Carinae, while HD 83944 is the identifier from the Henry Draper catalogue. It is a suspected variable with an apparent visual magnitude that fluctuates around 4.51 with an amplitude of 0.5. The system is located at a distance of approximately 226 light years from the Sun based on parallax, and it has an absolute magnitude of 0.31. It is a member of the Carina association of co-moving stars.

<span class="mw-page-title-main">V520 Carinae</span> Star in the constellation Carina

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<span class="mw-page-title-main">V345 Carinae</span> Star in the constellation Carina

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. Its actual brightness varies from magnitude +4.67 to +4.78 with a period of 137.7 days. Based on parallax measurements, it is located at a distance of approximately 1,010 light years from the Sun. It is drifting further away with a radial velocity of around +19 km/s.

<span class="mw-page-title-main">V448 Carinae</span> Star in the constellation Carina

V448 Carinae is a single star in the constellation Carina. It has the Bayer designation O Carinae, while V448 Carinae is the variable star designation. This object has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude that fluctuates around 5.60. It is located at a distance of approximately 680 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +26 km/s.

<span class="mw-page-title-main">V518 Carinae</span> Blue-hued variable star in the constellation Carina

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<span class="mw-page-title-main">7 Ceti</span> Star in the constellation Cetus

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KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of 2.19″±0.03″. Based upon an annual parallax shift of 7.6 mas as seen from Earth's orbit, it is located 430 light-years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Upper Centaurus-Lupus sub-group of the Scorpius–Centaurus association.

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 5 6 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. 1 2 3 4 5 6 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 "V344 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, 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. 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 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. 1 2 3 4 5 6 7 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.
  14. ↑ Cousins, A. W. J. (October 1951). "Bright variable stars in southern hemisphere (first list)". The Observatory. 71: 199–201. Bibcode:1951Obs....71..199C . Retrieved 9 January 2025.
  15. ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (January 1975). "60th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 961: 1–15. Bibcode:1975IBVS..961....1K . Retrieved 9 January 2025.
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