R Capricorni
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Capricornus |
| Right ascension | 20h 11m 18.39s[2] |
| Declination | −14° 16′ 04.4″[2] |
| Apparent magnitude (V) | 9.4 to 14.9[3] |
| Characteristics | |
| Spectral type | Cev[2] |
| Variable type | M[3] |
| Astrometry | |
| Proper motion (μ) | RA: 4[2] mas/yr Dec.: −6[2] mas/yr |
| Other designations | |
| Database references | |
| SIMBAD | data |
R Capricorni (R Cap) is a star in the constellation of Capricornus.[2] 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.[4]
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.[4]
R Capricorni is losing mass at rate of 2.8*10−6M☉/year.[5]
References[edit]
- ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
- ^ a b c d e f g V* R Cap -- Variable Star of Mira Cet type, database entry, SIMBAD. Accessed on line November 9, 2009.
- ^ 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.
- ^ a b 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.
- ^ 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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