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 [2]   mas
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] 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]

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Chi Carinae Star in the constellation Carina

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V382 Carinae Star in the constellation Carina

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V343 Carinae 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.

N Carinae is a single star in the constellation Carina, just to the northeast of the prominent star Canopus. This object has a white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.35. Based on parallax, it is located at a distance of approximately 1,360 light years from the Sun. It has an absolute magnitude of −3.75, and is drifting further away with a radial velocity of +22.5 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.

V520 Carinae Star in the constellation Carina

V520 Carinae is a single star in the southern constellation of Carina. It has the Bayer designation w Carinae, while V520 Carinae is a variable star designation. The star has an orange hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around +4.58. It is located at a distance of approximately 1,140 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +9 km/s. It is a candidate member of the IC 2391 moving group of co-moving stars.

V533 Carinae Star in the constellation Carina

V533 Carinae is a white A-type supergiant variable star with a mean apparent magnitude of +4.59 in the constellation Carina. It is over 10,000 light years from Earth.

V345 Carinae 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.

T Carinae is a star in the southern constellation of Carina. Although given a variable star designation, it is now thought to be constant; the identifier HD 94776 from the Henry Draper catalogue may be used instead. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.93. The distance to this object is approximately 285 light years based on parallax, and it has an absolute magnitude of 1.08. It is drifting closer to the Sun with a radial velocity of −26 km/s.

V448 Carinae 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.

HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary star system in the southern constellation of Centaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30. The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s. It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association. HD 102776 has a relatively large peculiar velocity of 31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.

Lambda Crucis Star in the constellation Crux

λ Crucis, Latinized as Lambda Crucis, is a single, variable star in the southern constellation Crux, near the constellation border with Centaurus. It is visible to the naked eye as a faint, blue-white hued point of light with an apparent visual magnitude that fluctuates around 4.62. The star is located approximately 384 light-years distant from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s. It is a proper motion member of the Lower-Centaurus Crux sub-group in the Scorpius-Centaurus OB association, the nearest such association of co-moving massive stars to the Sun.

Beta Hydrae, Latinized from β Hydrae, is a double star in the equatorial constellation of Hydra. Historically, Beta Hydrae was designated 28 Crateris, but the latter fell out of use when the IUA defined the permanent constellation boundaries in 1930. The system is faintly visible to the naked eye with a combined apparent visual magnitude that ranges around 4.29. It is located at a distance of approximately 310 light years from the Sun based on parallax.

V518 Carinae Star in the constellation Carina

V518 Carinae is a naked-eye variable star in the constellation Carina. It is a member of the bright open cluster IC 2602 near the Carina Nebula.

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 Lower Centaurus Crux sub-group of the Scorpius–Centaurus Association.

Lambda Pavonis Single, variable star in the constellation Pavo

λ Pavonis, Latinized as Lambda Pavonis, is a single, variable star in the southern constellation of Pavo. It is a blue-white hued star that is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.22. This object is located approximately 1,400 light years from the Sun, based upon parallax. It is a member 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, 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 .
  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.
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