With a mean visual apparent magnitude 17.5, V669 Cassiopeiae varies with an amplitude of about half a magnitude.[2] In the mid-infraredL 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 OHmaser emission varied in intensity with a 1994 day period.[7] In 1990, Paolo Persi et al. showed that V669 Cassiopeiae varied in infrared brightness,[8] and for that reason it was given its variable star designation in 1993.[9]
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.[6]
^ abcdeCutri, 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.
^ abcDe 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. S2CID16131273.