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This is a main sequenceBe star with a stellar classification of B3 Ve. Samus et al. (2017) classify it as a Be variable, rather than a Gamma Cassiopeiae type, and it ranges from a peak Hipparcos magnitude of 5.10 down to 5.22. The star is spinning with a projected rotational velocity of 95 km/s, but is being viewed from an extreme pole-on position. Hence it is spinning much more rapidly than indicated. Outbursts of hydrogen emission lines have been observed, as well as rapid changes in hydrogen line profiles. It is 25 million years old with around six times the mass of the Sun.
"BV Cam", International Variable Star Index, AAVSO, retrieved 2022-07-26.
^ Slettebak, A. (1982), "Spectral types and rotational velocities of the brighter Be stars and A-F type shell stars", Astrophysical Journal Supplement Series, 50: 55, Bibcode:1982ApJS...50...55S, doi:10.1086/190820.
^ Zorec, J.; et al. (November 2016), "Critical study of the distribution of rotational velocities of Be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity", Astronomy & Astrophysics, 595: 26, Bibcode:2016A&A...595A.132Z, doi:10.1051/0004-6361/201628760, hdl:11336/37946.
Ballereau, D.; et al. (May 1987), "Hα echelle spectroscopy of Be stars: an atlas.", Revista Mexicana de Astronomía y Astrofísica, 15 (1): 29–52, Bibcode:1987RMxAA..15...29B.