R Capricorni

Not to be confused with Rho Capricorni.
R Capricorni

The visual band light curve of R Capricorni, from AAVSO data[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Capricornus
Right ascension 20h 11m 18.35s[2]
Declination −14° 16′ 03.4″[2]
Apparent magnitude (V) 9.4 to 14.9[3]
Characteristics
Spectral type Cev[4]
Variable type M[3]
Astrometry
Proper motion (μ) RA: +1.571[2] mas/yr
Dec.: +1.420[2] mas/yr
Parallax (π)0.5515±0.0362 mas[2]
Distance5,900 ± 400 ly
(1,800 ± 100 pc)
Other designations
R Cap, BD−14 5663, GC 28001, SAO 163323, 2MASS J20111833−1416033[4]
Database references
SIMBADdata

R Capricorni (R Cap) is a star in the constellation of Capricornus.[4] It has an apparent visual magnitude which varies between 9.4 and 14.9.[3] A mira variable and ageing red giant, it is in the asymptotic giant branch stage of its lifespan.[5] It is a carbon star.[5]

John Russell Hind discovered this variable star in 1848. It appeared with its variable star designation, R Capricorni, in Annie Jump Cannon's 1907 work, Second Catalogue of Variable Stars.[6]

R Capricorni is too far from earth for its parallax to be measured effectively; Guandalini and Cristallo calculated the luminosity of Mira variables based on their periods. Using a period of 345.13 days, they calculated the absolute magnitude of R Capricorni to be -4.58.[5]

R Capricorni is losing mass at rate of 2.8×10−6 M☉/year.[7]

References

  1. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. ^ a b c d e 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. ^ a b c R Cap, database entry, The combined table of GCVS Vols I-III and NL 67-78 with improved coordinates, General Catalogue of Variable Stars Archived 2017-06-20 at the Wayback Machine, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line November 9, 2009.
  4. ^ a b c "R Cap". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-08-12.
  5. ^ a b c Guandalini, R.; Cristallo, S. (2013). "Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way". Astronomy & Astrophysics. 555: 7. arXiv:1305.4203. Bibcode:2013A&A...555A.120G. doi:10.1051/0004-6361/201321225. S2CID 54918450. A120.
  6. ^ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory. 55: 1–94. Bibcode:1907AnHar..55....1C. Retrieved 7 January 2025.
  7. ^ Uttenthaler, S.; McDonald, I.; Bernhard, K.; Cristallo, S.; Gobrecht, D. (2019), "Interplay between pulsation, mass loss, and third dredge-up: More about Miras with and without technetium", Astronomy & Astrophysics, 622: A120, arXiv:1812.07434, Bibcode:2019A&A...622A.120U, doi:10.1051/0004-6361/201833794, S2CID 119004841
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