R Volantis

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R Volantis
RVolLightCurve.png
A visual band light curve for R Volantis, plotted from AAVSO data [1]
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
Radius 687 [9] [lower-alpha 1]   R☉
Luminosity 6,800 [9]   L☉
Temperature 2,000 [9]   K
Other designations
R Vol, CD−72°378, 2MASS J07053619-7300519
Database references
SIMBAD data

R Volantis is a single variable star in the southern circumpolar constellation Volans. It has an average apparent magnitude of 8.7, [10] 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 .

R Volantis' peculiarity was first observed in 1954 when it was found to have emission lines in its spectrum. [11] Observations from 1955 to 1967 reveal that the star was a probable Mira variable [12] 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. [13]

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☉ . [9] R Vol has an effective temperature of 2,000  K , giving a deep red hue. [9]

It fluctuates between magnitude 8.7 and 15.4 and has a period of 445 days. [3]

Notes

  1. ↑ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772  K:
    .

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References

  1. ↑ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  2. 1 2 3 4 5 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.
  3. 1 2 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.
  4. 1 2 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.
  5. 1 2 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.
  6. ↑ 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.
  7. ↑ 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.
  8. ↑ 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.
  9. 1 2 3 4 5 Siderud, Emelie (2020). Dust emission modelling of AGB stars.
  10. ↑ 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.
  11. ↑ 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.
  12. ↑ 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.
  13. ↑ 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.
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