Astronomy:S Cephei

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Short description: Variable star in the constellation Cepheus
S Cephei
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S Cephei, as seen by WISE (false colour infrared)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cepheus
Right ascension  21h 35m 12.8233s[1]
Declination +78° 37′ 28.185″[1]
Apparent magnitude (V) 6.6 - 12.5[2]
Characteristics
Evolutionary stage AGB[3]
Spectral type C7,3e[4]
Variable type Mira[2]
Astrometry
Proper motion (μ) RA: 8.278[1] mas/yr
Dec.: 0.748[1] mas/yr
Parallax (π)2.0452 ± 0.0697[1] mas
Distance1,590 ± 50 ly
(490 ± 20 pc)
Details
Mass5.4[5] M☉
Radius254[6] R☉
Luminosity5,417[6] L☉
Surface gravity (log g)3.61[5] cgs
Temperature4,032[5] K
Metallicity [Fe/H]−0.54[5] dex
Other designations
BD+77°827, HD 206362, HIP 106583, SAO 10100[7]
Database references
SIMBADdata

S Cephei (S Cep), also designated as HD 206362, is a carbon star and Mira-type variable in the constellation Cepheus. Based on the measurement of its annual parallax by the Gaia satellite, the star is approximately ~1,590 ly (~490 pc) away from Earth.

A visual band light curve for S Cephei, plotted from ASAS-SN data[8]

S Cephei is a carbon star of spectral type C7.3e.[9] It is also a Mira-type variable star whose apparent magnitude varies from 6.6 to 12.5 in the form of a pulsation over a period of 484 days.[2] Its variability was discovered by Karl Hencke in 1858.[10]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 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.
  2. ↑ 2.0 2.1 2.2 Samus, N.N.; Kazarovets, E.V.; Durlevich, O.V.; Kireeva, N.N.; Pastukhova, E.N.. "S Cep". Lomonosov Moscow State University. http://www.sai.msu.su/gcvs/cgi-bin/search2.cgi?search=S+Cep. 
  3. ↑ McDonald, I.; De Beck, E.; Zijlstra, A. A.; Lagadec, E. (2018). "Pulsation-triggered dust production by asymptotic giant branch stars". Monthly Notices of the Royal Astronomical Society 481 (4): 4984. doi:10.1093/mnras/sty2607. Bibcode: 2018MNRAS.481.4984M. 
  4. ↑ Yamashita, Y. (1975). "The C-classification of spectra of carbon stars, II". Annals of the Tokyo Astronomical Observatory 15: 47. Bibcode: 1975AnTok..15...47Y. 
  5. ↑ 5.0 5.1 5.2 5.3 Khalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G. et al. (2024). "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost". Astronomy and Astrophysics 691: A98. doi:10.1051/0004-6361/202451427. Bibcode: 2024A&A...691A..98K. 
  6. ↑ 6.0 6.1 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society 471 (1): 770. doi:10.1093/mnras/stx1433. Bibcode: 2017MNRAS.471..770M. 
  7. ↑ "V* S Cep". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V%2A+S+Cep. 
  8. ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup. 
  9. ↑ Yamashita, Y. (1975). "The C-classification of spectra of carbon stars, II". Annals of the Tokyo Astronomical Observatory 15: 47-58. Bibcode: 1975AnTok..15...47Y. https://ui.adsabs.harvard.edu/abs/1975AnTok..15...47Y/abstract. Retrieved 17 December 2024. 
  10. ↑ "VSX : Detail for S Cephei" (in en). AAVSO. https://www.aavso.org/vsx/index.php?view=detail.top&oid=8354. 



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