Astronomy:R Carinae

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Short description: Variable star in the constellation Carina
This page is about the variable star. For r Carinae, see HD 91942.
R Carinae
250px
The visual band light curve of R Carinae, from AAVSO data[1]
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas/yr
Dec.: +19.535[2] mas/yr
Parallax (π)5.5018 ± 0.3345[2] mas
Distance590 ± 40 ly
(180 ± 10 pc)
Absolute magnitude (MV)1.48[6] (at mv = 7.43)
Details
Mass0.87+0.47
−0.31[4] M☉
Radius400±2 (2013)[7] R☉
581–652 (2018)[8] R☉
540±50 (2020)[7] R☉
Luminosity4,571+1,331
−1,031[4] L☉
Temperature2,800[9] K
Other designations
R Car, CD−62°396, GC 13192, HD 82901, HIP 46806, HR 3816, SAO 250614, CCDM J09322-6247, WDS J09322-6247AB[10]
Database references
SIMBADdata

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. https://www.aavso.org/data-download. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  4. ↑ 4.0 4.1 4.2 4.3 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, doi:10.1093/pasj/65.3.60, Bibcode: 2013PASJ...65...60T. 
  5. ↑ 5.0 5.1 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. ↑ 6.0 6.1 6.2 6.3 6.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  7. ↑ 7.0 7.1 7.2 Rosales-Guzmán, A.; Sanchez-Bermudez, J.; Paladini, C.; Freytag, B.; Wittkowski, M.; Alberdi, A.; Baron, F.; Berger, J.-P. et al. (2024-08-01), "A new dimension in the variability of AGB stars: Convection patterns size changes with pulsation" (in en), Astronomy & Astrophysics 688: A124, 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. et al. (2023-06-01). "Imaging the innermost gaseous layers of the Mira star R Car with GRAVITY-VLTI" (in en). Astronomy & Astrophysics 674: A62. doi:10.1051/0004-6361/202245370. ISSN 0004-6361. https://www.aanda.org/articles/aa/full_html/2023/06/aa45370-22/aa45370-22.html. 
  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, doi:10.1111/j.1365-2966.2012.21873.x, Bibcode: 2012MNRAS.427..343M. 
  10. ↑ "R Car". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=R+Car. 
  11. ↑ 11.0 11.1 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, doi:10.3847/0067-0049/227/1/6, Bibcode: 2016ApJS..227....6V. 
  12. ↑ Cannon, Annie J. (1907), "Second catalogue of variable stars", Annals of Harvard College Observatory 55: 1-94, Bibcode: 1907AnHar..55....1C, https://articles.adsabs.harvard.edu/pdf/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, doi:10.1111/j.1365-2966.2005.09181.x, Bibcode: 2005MNRAS.361..337I. 
  14. ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M. 



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