Astronomy:S Canis Minoris

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Short description: Variable star in the constellation Canis Minor
S Canis Minoris
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The visual band light curve of S Canis Minoris, from AAVSO data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Canis Minor[2]
Right ascension  07h 32m 43.06942s[3]
Declination +08° 19′ 05.1975″[3]
Apparent magnitude (V) 6.5 to 13.7[4]
Characteristics
Evolutionary stage AGB[5]
Spectral type M7-8e[6]
B−V color index 1.50±0.51[2]
Variable type Mira variable[7][4]
Astrometry
Radial velocity (Rv)68.0±4.8[8] km/s
Proper motion (μ) RA: −10.785[3] mas/yr
Dec.: −12.827[3] mas/yr
Parallax (π)2.440 ± 0.098[9] mas
Distance1,340 ± 50 ly
(410 ± 20 pc)
Details
Radius378 – 402[9] R☉
Luminosity6,174+402
−378[9] L☉
Surface gravity (log g)−0.46 to −0.51[9] cgs
Temperature2,854 – 2,872[9] K
Metallicity [Fe/H]+0.39[10] dex
Other designations
S CMi, BD+08°1800, HD 59950, HIP 36675, SAO 115591[11]
Database references
SIMBADdata

S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of 6.5, so not normally visible to the naked eye. The star is located at a distance of approximately 1,340 light-years from the Sun based on stellar parallax, and is drifting further away with a radial velocity of about +68 km/s.

In 1856, John Russell Hind discovered that S Canis Minoris is a variable star.[12] This is an aging red giant star with a stellar classification of M7-8e,[6] where the 'e' suffix indicates emission lines in the spectrum. It is a Mira-type[7] long period variable that varies by an amplitude of 4.27 in visual magnitude over a period of 327.77±2.78 d.[13] Evidence has been found of asymmetry in this star, suggesting a non-spherical shape.[5] Abundance-wise, it is an oxygen-rich[14] giant and the emission feature is of the oxygen-rich silicate class as it sheds silicate dust from its atmosphere.[15] The star is shedding mass at the rate of 4.9×10−8 M☉/yr.[5]

References

  1. ↑ "Download Data". AAVSO. https://www.aavso.org/data-download. 
  2. ↑ 2.0 2.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  3. ↑ 3.0 3.1 3.2 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.
  4. ↑ 4.0 4.1 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. 
  5. ↑ 5.0 5.1 5.2 Danilovich, T. et al. (September 2015). "New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme". Astronomy & Astrophysics 581: 33. doi:10.1051/0004-6361/201526705. A60. Bibcode: 2015A&A...581A..60D. 
  6. ↑ 6.0 6.1 Keenan, Philip C. et al. (1974). "Revised Catalog of Spectra of Mira Variables of Types ME and Se". The Astrophysical Journal Supplement Series 28: 271. doi:10.1086/190318. Bibcode: 1974ApJS...28..271K. 
  7. ↑ 7.0 7.1 Garfinkle, Robert A. (1997). Star-hopping: your Visa to Viewing the Universe. Cambridge, United Kingdom: Cambridge University Press. pp. 78–81. ISBN 978-0-521-59889-7. 
  8. ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 Béguin, E.; Chiavassa, A.; Ahmad, A.; Freytag, B.; Uttenthaler, S. (2024-10-01). "Retrieving stellar parameters and dynamics of AGB stars with Gaia parallax measurements and CO5BOLD RHD simulations" (in en). Astronomy & Astrophysics 690: A125. doi:10.1051/0004-6361/202450245. ISSN 0004-6361. 
  10. ↑ Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardevol, J.; Casamiquela, L.; Figueras, F.; Jimenez-Arranz, O. et al. (2022). "VizieR Online Data Catalog: StarHorse2, Gaia EDR3 photo-astrometric distances (Anders+, 2022)". Vizier Online Data Catalog. Bibcode: 2022yCat.1354....0A. 
  11. ↑ "S CMi". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=S+CMi. 
  12. ↑ Cannon, Annie J. (1907). "Second catalogue of variable stars". Annals of Harvard College Observatory 55: 1–94. Bibcode: 1907AnHar..55....1C. 
  13. ↑ Vogt, N.; Contreras-Quijada, A.; Fuentes-Morales, I.; Vogt-Geisse, S.; Arcos, C.; Abarca, C.; Agurto-Gangas, C.; Caviedes, M. et al. (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): 13. doi:10.3847/0067-0049/227/1/6. 6. Bibcode: 2016ApJS..227....6V. 
  14. ↑ Winters, J. M. et al. (October 2003). "Mass-loss from dusty, low outflow-velocity AGB stars. I. Wind structure and mass-loss rates". Astronomy and Astrophysics 409 (2): 715–735. doi:10.1051/0004-6361:20031110. Bibcode: 2003A&A...409..715W. 
  15. ↑ Sloan, G. C.; Price, S. D. (December 1998). "The Infrared Spectral Classification of Oxygen-rich Dust Shells". The Astrophysical Journal Supplement Series 119 (2): 141–158. doi:10.1086/313156. Bibcode: 1998ApJS..119..141S. 



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