S Canis Minoris
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canis Minor |
| Right ascension | 07h 32m 43.07002s[1] |
| Declination | 08° 19′ 05.2015″[1] |
| Apparent magnitude (V) | 10.74[2] (6.5 to 13.7)[3] |
| Characteristics | |
| Evolutionary stage | AGB[4] |
| Spectral type | M7-8e[5] |
| B−V color index | 1.50±0.51[2] |
| Variable type | Mira[6][3] |
| Astrometry | |
| Radial velocity (Rv) | 68.0±4.8[7] km/s |
| Proper motion (μ) | RA: −11.471[1] mas/yr Dec.: −13.078[1] mas/yr |
| Parallax (π) | 2.0753 ± 0.1624 mas[1] |
| Distance | 1,600 ± 100 ly (480 ± 40 pc) |
| Details | |
| Luminosity | 6,493[8] L☉ |
| Temperature | 3,292[1] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
S Canis Minoris is a variable star in the equatorial constellation Canis Minor. It has a peak apparent visual magnitude of 7.63±0.37, which lies below the minimum brightness that is normally visible to the naked eye.[10] The star is located at a distance of approximately 1,600 light-years from the Sun based on stellar parallax,[1] and is drifting further away with a radial velocity of about +68 km/s.[7]
This is an aging red giant star with a stellar classification of M7-8e,[5] where the 'e' suffix indicates emission lines in the spectrum. It is a Mira-type[6] long period variable that varies by an amplitude of 4.27 in visual magnitude over a period of 327.77±2.78 d.[10] Evidence has been found of asymmetry in this star, suggesting a non-spherical shape.[4] Abundance-wise, it is an oxygen-rich[8] giant and the emission feature is of the oxygen-rich silicate class as it sheds silicate dust from its atmosphere.[11] The star is shedding mass at the rate of 4.9×10−8 M☉·yr−1.[4]
References
- ^ a b c d e f g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
- ^ a b c 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. arXiv:1506.09065. Bibcode:2015A&A...581A..60D. doi:10.1051/0004-6361/201526705. S2CID 55109956. A60.
- ^ a b 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. Bibcode:1974ApJS...28..271K. doi:10.1086/190318.
- ^ a b 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.
- ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ a b 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. Bibcode:2003A&A...409..715W. doi:10.1051/0004-6361:20031110.
- ^ "S CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-13.
- ^ 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. (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. arXiv:1609.05246. Bibcode:2016ApJS..227....6V. doi:10.3847/0067-0049/227/1/6. S2CID 119295645. 6.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ 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. Bibcode:1998ApJS..119..141S. doi:10.1086/313156.
