R Carinae

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R Carinae
RCarLightCurve.png
The visual band light curve of R Carinae, from AAVSO data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Carina
Right ascension 09h 32m 14.59610s [2]
Declination −62° 47′ 20.0026″ [2]
Apparent magnitude  (V)3.9 - 10.5 [3]
Characteristics
Evolutionary stage AGB [4]
Spectral type M6/7pe [5]
B−V color index 0.906±0.009 [6]
Variable type Mira [3]
Astrometry
Radial velocity (Rv)+28.1±1.0 [6] km/s
Proper motion (μ)RA: −36.291 mas/yr [2]
Dec.: +19.535 mas/yr [2]
Parallax (π)5.5018±0.3345  mas [2]
Distance 590 ± 40  ly
(180 ± 10  pc)
Absolute magnitude  (MV)1.48 [6] (at mv = 7.43)
Details
Mass 0.87+0.47
−0.31 [4]   M☉
Radius 400±2 (2013) [7] R☉
581–652 (2018) [8] R☉
540±50 (2020) [7]   R☉
Luminosity 4,571+1,331
−1,031 [4]   L☉
Temperature 2,800 [9]   K
Other designations
R Car, AAVSO 0929-62, CD−62°396, GC 13192, HD 82901, HIP 46806, HR 3816, SAO 250614, CCDM J09322-6247, WDS J09322-6247AB [10]
Database references
SIMBAD data

R Carinae is a double star in the southern constellation of Carina. The brighter component is a variable star that can be viewed with the naked eye at peak brightness, [11] but is usually too faint to be seen without a telescope, having an apparent visual magnitude that fluctuates around 7.43. [6] This star is located at a distance of approximately 600  light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +28 km/s. [6]

Benjamin Apthorp Gould discovered the variable star, in 1871. It appeared with its variable star designation in Annie Jump Cannon's 1907 work, Second Catalogue of Variable Stars. [12] The main component is an aging red giant star on the asymptotic giant branch [4] with a stellar classification of M6/7pe. [5] It is classified as a pulsating Mira type variable star and its visual brightness varies with an average amplitude of 4.25 magnitudes over a period of 303.99±1.08 d. Its average maximum visual magnitude is 5.05±0.45, [11] but the brightest observed maximum was magnitude 3.9. [3] The pulsations make its size change, in 2014, it was 400 times larger than the Sun, while in 2020 it was 540 times larger. [7] This star is surrounded by a dusty shell, with properties that are consistent with iron-poor silicates or corundum, extending from around three stellar radii outward. [13]

The companion is a magnitude 11.30 star at an angular separation of 2.10″ along a position angle of 132° from the main star, as of 2015. [14]

References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 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.
  4. 1 2 3 4 Takeuti, Mine; et al. (2013), "A Method to Estimate the Masses of Asymptotic Giant Branch Variable Stars", Publications of the Astronomical Society of Japan, 65 (3): 60, Bibcode:2013PASJ...65...60T, doi: 10.1093/pasj/65.3.60 .
  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. 1 2 3 4 5 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.
  7. 1 2 3 Rosales-Guzmán, A.; Sanchez-Bermudez, J.; Paladini, C.; Freytag, B.; Wittkowski, M.; Alberdi, A.; Baron, F.; Berger, J.-P.; Chiavassa, A.; Höfner, S.; Jorissen, A.; Kervella, P.; Bouquin, J.-B. Le; Marigo, P.; Montargès, M. (2024-08-01), "A new dimension in the variability of AGB stars: Convection patterns size changes with pulsation", Astronomy & Astrophysics , 688: A124, arXiv: 2405.10164 , doi:10.1051/0004-6361/202349112, ISSN   0004-6361
  8. ↑ Rosales-Guzmán, A.; Sanchez-Bermudez, J.; Paladini, C.; Alberdi, A.; Brandner, W.; Cannon, E.; González-Torá, G.; Haubois, X.; Henning, Th; Kervella, P.; Montarges, M.; Perrin, G.; Schödel, R.; Wittkowski, M. (2023-06-01). "Imaging the innermost gaseous layers of the Mira star R Car with GRAVITY-VLTI". Astronomy & Astrophysics. 674: A62. arXiv: 2303.00056 . doi:10.1051/0004-6361/202245370. ISSN   0004-6361.
  9. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343, arXiv: 1208.2037 , Bibcode:2012MNRAS.427..343M, doi: 10.1111/j.1365-2966.2012.21873.x , S2CID   118665352.
  10. ↑ "R Car". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-01-30.
  11. 1 2 Vogt, N.; et al. (2016), "Determination of Pulsation Periods and Other Parameters of 2875 Stars Classified As Mira in the All Sky Automated Survey (Asas)", The Astrophysical Journal Supplement Series, 227 (1): 6, arXiv: 1609.05246 , Bibcode:2016ApJS..227....6V, doi: 10.3847/0067-0049/227/1/6 , S2CID   119295645.
  12. ↑ Cannon, Annie J. (1907), "Second catalogue of variable stars", Annals of Harvard College Observatory, 55: 1–94, Bibcode:1907AnHar..55....1C , retrieved 8 January 2025
  13. ↑ Ireland, M. J.; et al. (July 2005), "Dust scattering in the Miras R Car and RR Sco resolved by optical interferometric polarimetry", Monthly Notices of the Royal Astronomical Society, 361 (1): 337–344, arXiv: astro-ph/0505112 , Bibcode:2005MNRAS.361..337I, doi: 10.1111/j.1365-2966.2005.09181.x , S2CID   14724805.
  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 .
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