Variable star in the constellation Canis Major
 ;/td ;
! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000.0
       Equinox J2000.0
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Spectral type
! style="text-align:left" | Variable type
 ;/th ; ;/tr ;
 ;/th ; ;/tr ;
FY Canis Majoris (FY CMa), also known as HD 58978, is a star about 1,800 light years from the Earth, in the constellation Canis Major ("very" near the border of Puppis). It is usually a 5th magnitude star, so it will be visible to the naked eye of an observer far from city lights. It is a Gamma Cassiopeiae variable star, whose brightness varies from magnitude 4.8 to 6.25.
In 1967, Alejandro Feinstein detected low amplitude (0.14 magnitude) variability in HD 58978's brightness, from photoelectric observations at La Plata Observatory. The star was given the variable star designation FY Canis Majoris in 1973. During an outburst in 2009, the star brightened to magnitude 4.8, its historical peak brightness. "TESS" data show that FY CMa pulsates at many different frequencies, with periods ranging from 1.07 hours to 5.8 days.
In 1905, Edward King noted that FY CMa has a peculiar spectrum with an unusually bright Hβ (and other) emission lines. Paul Merrill "et al." listed it as a Be star in 1925. Spectra taken by various observers over several decades of the 20th century showed that the strength and relative intensities of the star's emission line are variable, and could change on a timescale of just a few days.
In 2008, Geraldine Peters "et al." obtained high resolution spectra from the " IUE" and found that the Be star has hot, far less massive subdwarf companion star, with which it forms a spectroscopic binary.
Hui-Lau Cao calculated that FY CMa is losing mass at a rate of about 6 × 10−8 M☉/year via a stellar wind with a terminal velocity of about 750 km/sec.
References.
 ;templatestyles src="Reflist/styles.css" / ;