S Cassiopeiae

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S Cassiopeiae
Cassiopeia constellation map.svg
Location of S Cas
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia
Right ascension  01h 19m 41.99s[1]
Declination 72° 36′ 40.8″[1]
Apparent magnitude (V) +7.9 – +16.1[2]
Characteristics
Spectral type S3,4 – S5,8[3]
Variable type Mira[2]
Astrometry
Proper motion (μ) RA: 3.201[4] mas/yr
Dec.: 1.056[4] mas/yr
Parallax (π)0.8585 ± 0.1626[4] mas
Distance460[5] pc
Details
Radius930[6] R
Luminosity5,210[5] L
Temperature1,800[7] K
Other designations
S Cas, HD 7769, BD+71°66, 2MASS J01194198+7236407, GSC 04305-01322, IRAS 01159+7220, IRC+70024, AAVSO 0112+72
Database references
SIMBADdata

S Cassiopeiae (S Cas, HD 7769) is a Mira variable and S-type star in the constellation Cassiopeia. It is an unusually cool star, rapidly losing mass and surrounded by dense gas and dust producing masers.

Distance[edit]

In the absence of a measure of its parallax by the Hipparcos satellite, its distance from the solar system was estimated between 1,860 and 2,770 light-years.[7][8] Gaia Data Release 2 published a parallax of 0.8585±0.1626 mas, indicating a distance around 1200 pc,[4] but the observations have a very high noise level and are considered unreliable. A distance of 460 pc is preferred.[5]

Spectral type[edit]

With a spectral type of S3,4e-S5,8e, S Cassiopeiae is an S-type star similar to χ Cygni; these are asymptotic giant branch (AGB) stars similar to those of class M except that the dominant spectral bands of metal oxides are formed by metals of the fifth period of the periodic table as zirconium or yttrium. Another feature of this class of stars is the high mass loss; in the case of S Cassiopeiae it is estimated at 3.5×10−6 M per year.[3]

Characteristics[edit]

S Cassiopeiae has a radius of 930 solar radii; if placed at the center of the Solar System, it would extend past the orbit of Mars and the Asteroid Belt. Its effective temperature is 1,800 K,[7] which is exceptionally cool for any star, and its bolometric luminosity is 8,000 times that of the sun.[5]

S Cassiopeiae is a variable Mira, a pulsating variable star whose visual brightness varies over several magnitudes with a somewhat regular period and amplitude. Its visual magnitude varies between +7.9 and +16.1 over an average period of 612.43 days. Mira variables are stars in the last stages of evolution whose instability comes from pulsations in its surface, causing changes in color and brightness. Some of them, including S Cassiopeiae show SiO maser emission.[9]

See also[edit]

References[edit]

  1. ^ a b Cutri, R. M.; Skrutskie, M. F.; Van Dyk, S.; Beichman, C. A.; Carpenter, J. M.; Chester, T.; Cambresy, L.; Evans, T.; Fowler, J.; Gizis, J.; Howard, E.; Huchra, J.; Jarrett, T.; Kopan, E. L.; Kirkpatrick, J. D.; Light, R. M.; Marsh, K. A.; McCallon, H.; Schneider, S.; Stiening, R.; Sykes, M.; Weinberg, M.; Wheaton, W. A.; Wheelock, S.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C. 2246. Bibcode:2003yCat.2246....0C.
  2. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  3. ^ a b Ramstedt, S.; Schöier, F. L.; Olofsson, H.; Lundgren, A. A. (2006). "Mass-loss properties of S-stars on the AGB". Astronomy and Astrophysics. 454 (2): L103. arXiv:astro-ph/0605664. Bibcode:2006A&A...454L.103R. doi:10.1051/0004-6361:20065285.
  4. ^ a b c d 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.
  5. ^ a b c d 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. arXiv:1809.07965. Bibcode:2018MNRAS.481.4984M. doi:10.1093/mnras/sty2607.
  6. ^ "Circumstellar molecular line emission from S-type AGB stars: mass-loss rates and SiO abundances". Astronomy and Astrophysics. 499 (2): 515–527. 2009. arXiv:0903.1672. Bibcode:2009A&A...499..515R. doi:10.1051/0004-6361/200911730. 515-527.
  7. ^ a b c Ramstedt, S.; Olofsson, H. (2014). "The 12CO/13CO ratio in AGB stars of different chemical type. Connection to the 12C/13C ratio and the evolution along the AGB". Astronomy & Astrophysics. 566: A145. arXiv:1405.6404. Bibcode:2014A&A...566A.145R. doi:10.1051/0004-6361/201423721.
  8. ^ Guandalini, R.; Busso, M. (2008). "Infrared photometry and evolution of mass-losing AGB stars. II. Luminosity and colors of MS and S stars". Astronomy and Astrophysics. 488 (2): 675. arXiv:0806.4591. Bibcode:2008A&A...488..675G. doi:10.1051/0004-6361:200809932.
  9. ^ Herpin, F.; Baudry, A.; Thum, C.; Morris, D.; Wiesemeyer, H. (2006). "Full polarization study of SiO masers at 86 GHz". Astronomy and Astrophysics. 450 (2): 667. arXiv:astro-ph/0601098. Bibcode:2006A&A...450..667H. doi:10.1051/0004-6361:20054255.