R Volantis is a single variable star in the southern circumpolar constellation Volans. It has an average apparent magnitude of 8.7,[11] making it readily visible in amateur telescopes but not to the naked eye. The object is relatively far at a distance of about 2,300 light years but is drifting closer with a radial velocity of −5 km/s.
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Volans |
| Right ascension | 07h 05m 36.2081s[2] |
| Declination | −73° 00′ 52.0345″[2] |
| Apparent magnitude (V) | 8.78 - 11.50[3] |
| Characteristics | |
| Evolutionary stage | AGB[4] |
| Spectral type | Ce[5] |
| Variable type | Mira[6] |
| Astrometry | |
| Radial velocity (Rv) | −4.7[7] km/s |
| Proper motion (μ) | RA: −14.298 mas/yr[2] Dec.: +19.462 mas/yr[2] |
| Parallax (π) | 1.3931 ± 0.0631 mas[2] |
| Distance | 2,317+97 −96 ly (710.7+29.9 −29.5 pc)[8] |
| Details | |
| Mass | 0.75[9] M☉ |
| Radius | 687[10][a] R☉ |
| Luminosity | 6,800[10] L☉ |
| Temperature | 2,000[10] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
R Volantis' peculiarity was first observed in 1954 when it was found to have emission lines in its spectrum.[12] Observations from 1955 to 1967 reveal that the star was a probable Mira variable[13] and was given its current designation. However, its nature as a carbon star wasn't discovered until 1968 by Pik-Sin The. In the paper, R Volantis and V1163 Centauri (HD 114586) had their spectrums studied and revealed that the former is a carbon star while the latter is an S-type star.[14]
R Volantis has a stellar classification of Ce,[5] indicating that it is a carbon star with emission lines. It is a giant star on the asymptotic giant branch,[4] meaning that it is generating energy via hydrogen and helium shells around an inert carbon core. As a result, it has expanded to 687 times the radius of the Sun and now radiates a luminosity of 6800 L☉.[10] R Vol has an effective temperature of 2,000 K, giving a deep red hue.[10]
It fluctuates between magnitude 8.7 and 15.4 and has a period of 445 days.[3]
Notes
edit- ^ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
- .
References
edit- ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
- ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b Vogt, N.; Contreras-Quijada, A.; Fuentes-Morales, I.; Vogt-Geisse, S.; Arcos, C.; Abarca, C.; Agurto-Gangas, C.; Caviedes, M.; DaSilva, H.; Flores, J.; Gotta, V.; Peñaloza, F.; Rojas, K.; Villaseñor, J. I. (10 November 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. eISSN 1538-4365.
- ^ a b Montez, Rodolfo; Ramstedt, Sofia; Kastner, Joel H.; Vlemmings, Wouter; Sanchez, Enmanuel (22 May 2017). "A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars". The Astrophysical Journal. 841 (1): 33. arXiv:1705.05371. Bibcode:2017ApJ...841...33M. doi:10.3847/1538-4357/aa704d. eISSN 1538-4357.
- ^ a b Henize, K. G. (April 1976). "Observations of southern emission-line stars". The Astrophysical Journal Supplement Series. 30: 491. Bibcode:1976ApJS...30..491H. doi:10.1086/190369. eISSN 1538-4365. ISSN 0067-0049.
- ^ Samus’, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (January 2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. ISSN 1063-7729. S2CID 125853869.
- ^ Menzies, John W.; Feast, Michael W.; Whitelock, Patricia A. (5 May 2006). "Carbon-rich Mira variables: radial velocities and distances". Monthly Notices of the Royal Astronomical Society. 369 (2): 783–790. arXiv:astro-ph/0603505. Bibcode:2006MNRAS.369..783M. doi:10.1111/j.1365-2966.2006.10323.x. ISSN 0035-8711.
- ^ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021-03-01). "Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. ISSN 0004-6256. Data about this star can be seen here.
- ^ Rau, G.; Hron, J.; Paladini, C.; Aringer, B.; Eriksson, K.; Marigo, P.; Nowotny, W.; Grellmann, R. (2017-04-01). "The adventure of carbon stars. Observations and modeling of a set of C-rich AGB stars". Astronomy and Astrophysics. 600: A92. arXiv:1701.04331. Bibcode:2017A&A...600A..92R. doi:10.1051/0004-6361/201629337. ISSN 0004-6361.
- ^ a b c d e Siderud, Emelie (2020). Dust emission modelling of AGB stars.
- ^ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
- ^ Bidelman, William P. (November 1954). "Catalogue and Bibliography of Emission-Line Stars of Types Later than B." The Astrophysical Journal Supplement Series. 1: 175. Bibcode:1954ApJS....1..175B. doi:10.1086/190007. eISSN 1538-4365. ISSN 0067-0049.
- ^ Feuchter, A. Ch. (August 1967). "On several statistical characteristics of Mira variables". The Astronomical Journal. 72: 702. Bibcode:1967AJ.....72..702F. doi:10.1086/110295. ISSN 0004-6256.
- ^ The, Pik-Sin (February 1968). "The Spectrum of the Variables R Vol and HD 114586". Publications of the Astronomical Society of the Pacific. 80 (472): 104. Bibcode:1968PASP...80..104T. doi:10.1086/128597. eISSN 1538-3873. ISSN 0004-6280.