V669 Cassiopeiae

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V669 Cassiopeiae
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Cassiopeia
Right ascension 01h 33m 51.21s [1]
Declination 62° 26′ 53.2″ [1]
Apparent magnitude  (V)17.48 [2]
Characteristics
Evolutionary stage AGB [3]
Spectral type M9III [3]
Apparent magnitude  (J)16.747 [1]
Apparent magnitude  (H)11.232 [1]
Apparent magnitude  (K)7.097 [1]
Variable type Mira? [4]
Astrometry
Distance 2,100 [5]   pc
Details
Radius 370 –702 [5]   R☉
Luminosity 10,000 - 36,000 [5]   L☉
Temperature 3,000 [5]   K
Database references
SIMBAD data

V669 Cassiopeiae or V669 Cas is an OH/IR star, a type of particularly cool red giant, with a spectral type of M9III.

With a mean visual apparent magnitude 17.5, V669 Cassiopeiae varies with an amplitude of about half a magnitude. [2] In the mid-infrared L band, its magnitude range is 1.57 to 3.02. It is listed as a possible Mira variable, but with the extremely long period of 1,994 days. [4]

Jan Herman and Harm Jan Habing reported in 1985 that the star's OH maser emission varied in intensity with a 1994 day period. [6] In 1990, Paolo Persi et al. showed that V669 Cassiopeiae varied in infrared brightness, [7] and for that reason it was given its variable star designation in 1993. [8]

The distance and physical properties of V669 Cassiopeiae are highly uncertain. Based on parallax, it is about 1,600 light years away, but a distance of about 20,000 light years has been derived based on observations of masers around the star. [3] Based on a luminosity derived from its pulsations and spectral energy distribution, it would be at a distance of 6,850 light years. [5]

See also

References

  1. 1 2 3 4 5 Cutri, Roc M.; et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  2. 1 2 Jayasinghe, T.; Kochanek, C. S.; Stanek, K. Z.; Shappee, B. J.; Holoien, T. W. -S.; Thompson, Todd A.; Prieto, J. L.; Dong, Subo; Pawlak, M.; Shields, J. V.; Pojmanski, G.; Otero, S.; Britt, C. A.; Will, D. (2018). "The ASAS-SN catalogue of variable stars I: The Serendipitous Survey". Monthly Notices of the Royal Astronomical Society. 477 (3): 3145. arXiv: 1803.01001 . Bibcode:2018MNRAS.477.3145J. doi: 10.1093/mnras/sty838 .
  3. 1 2 3 De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv: 1008.1083 . Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771. S2CID   16131273.
  4. 1 2 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.
  5. 1 2 3 4 5 Lombaert, R.; Decin, L.; De Koter, A.; Blommaert, J. A. D. L.; Royer, P.; De Beck, E.; De Vries, B. L.; Khouri, T.; Min, M. (2013). "H2O vapor excitation in dusty AGB envelopes. A PACS view of OH 127.8+0.0". Astronomy and Astrophysics. 554. arXiv: 1505.07696 . Bibcode:2013A&A...554A.142L. doi:10.1051/0004-6361/201218974. S2CID   98319654.
  6. ↑ Herman, J.; Habing, H. J. (March 1985). "Time variations and shell sizes of OH masers in late-type stars". Astronomy and Astrophysics, Supplement Series. 59: 523–555. Bibcode:1985A&AS...59..523H . Retrieved 29 August 2024.
  7. ↑ Persi, P.; Ferrari-Toniolo, M.; Shivanandan, K.; Ranieri, M.; Marenzi, A. (October 1990). "Infrared photometry up to 34 mu.m of the type II OH/IR sources OH 127.8-0.0 and OH 345.0+15.7". Astronomy and Astrophysics. 237: 153–158. Bibcode:1990A&A...237..153P . Retrieved 29 August 2024.
  8. ↑ Kazarovets, E. V.; Samus, N. N.; Goranskij, V. P. (February 1993). "The 71st Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 3840 (3840): 1. Bibcode:1993IBVS.3840....1K . Retrieved 29 August 2024.
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