Astronomy:W Andromedae

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Short description: Variable star in the constellation Andromeda
W Andromedae
WAndLightCurve.png
The visual band light curve of W Andromedae, from AAVSO data[1]
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  02h 17m 32.96122s[2]
Declination +44° 18′ 17.7573″[2]
Apparent magnitude (V) 6.7 – 14.6[3]
Characteristics
Spectral type S6,1e-S9,2e[3]
Variable type Mira[3]
Astrometry
Radial velocity (Rv)−38.19±0.4[4] km/s
Proper motion (μ) RA: −0.162[2] mas/yr
Dec.: −2.516[2] mas/yr
Parallax (π)2.2125 ± 0.0953[2] mas
Distance1,470 ± 60 ly
(450 ± 20 pc)
Absolute magnitude (MV)−5.27[5]
Details
Mass5.6[6] M☉
Luminosity8,394[7] L☉
Surface gravity (log g)−0.61[6] cgs
Temperature3,030[6] K
Metallicity [Fe/H]0.003[6] dex
Other designations
HD 14028, BD+43 461a, HIP 10687, HR 663
Database references
SIMBADdata

W Andromedae is a variable star in the constellation of Andromeda. It is classified as a Mira variable and S-type star,[8] and varies from an apparent visual magnitude of 14.6 at minimum brightness to a magnitude of 6.7 at maximum brightness, with a period of approximately 397.3 days.[3] The star is losing mass due to stellar winds at a rate of 2.79×10−7 M☉/yr.[5]

References

  1. ↑ "Download Data". AAVSO. https://www.aavso.org/data-download. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 3.2 3.3 Samus, N. N. 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: B/gcvs. Bibcode: 2009yCat....102025S. 
  4. ↑ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (December 2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics 340: 165–186. doi:10.1051/0004-6361:20041272. Bibcode: 2005A&A...430..165F. 
  5. ↑ 5.0 5.1 Guandalini, R. (April 2010). "Infrared photometry and evolution of mass-losing AGB stars. III. Mass loss rates of MS and S stars". Astronomy and Astrophysics 513: A4. doi:10.1051/0004-6361/200911764. Bibcode: 2010A&A...513A...4G. 
  6. ↑ 6.0 6.1 6.2 6.3 Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardevol, J.; Casamiquela, L.; Figueras, F.; Jimenez-Arranz, O. (2022). "VizieR Online Data Catalog: StarHorse2, Gaia EDR3 photo-astrometric distances (Anders+, 2022)". Vizier Online Data Catalog. Bibcode: 2022yCat.1354....0A. 
  7. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (21 November 2012). "Fundamental parameters and infrared excesses of Hipparcos stars: Parameters and IR excesses from Hipparcos". Monthly Notices of the Royal Astronomical Society 427 (1): 343–357. doi:10.1111/j.1365-2966.2012.21873.x. ISSN 0035-8711. Bibcode: 2012MNRAS.427..343M. 
  8. ↑ "W And". AAVSO. http://www.aavso.org/vsx/index.php. 




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