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V669 Cassiopeiae

From Wikipedia, the free encyclopedia

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
Proper motion (μ) RA: −2.813[5] mas/yr
Dec.: −2.147[5] mas/yr
Parallax (π)1.9523 ± 0.7049 mas[5]
Distance2,100[6] pc
Details
Radius859[3] R☉
Luminosity10,000 - 36,000[6] L☉
Temperature2,750[3] K
Database references
SIMBADdata

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]

The distance and physical properties of V559 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.[6]

See also

References

  1. ^ a b c d e 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. ^ a b 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. ^ a b c d e 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. ^ 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.
  5. ^ a b c 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.
  6. ^ a b c 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.
This page was last edited on 25 August 2023, at 12:20
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