Beta Canis Minoris
Epoch J2000 Equinox J2000
|Right ascension||07h 27m 09.04174s|
|Declination||+08° 17′ 21.5368″|
|Apparent magnitude (V)||2.89|
|Spectral type||B8 Ve|
|U−B color index||–0.28|
|B−V color index||–0.09|
|Radial velocity (Rv)||+22 km/s|
|Proper motion (μ)||RA: -51.76 mas/yr
Dec.: -38.29 mas/yr
|Parallax (π)||20.17 ± 0.20 mas|
|Distance||162 ± 2 ly
(49.6 ± 0.5 pc)
|Surface gravity (log g)||3.51 cgs|
|Rotational velocity (v sin i)||210 km/s|
Beta Canis Minoris (β CMi, β Canis Minoris) is a star in the constellation of Canis Minor. In the night sky it is notable for its proximity to the prominent star Procyon. It has the traditional name Gomeisa, which comes from the Arabic al-ghumaisa’ "the bleary-eyed (woman)", short for مرزم الغميصاء mirzam al-ghumaisa’ "girdle of the bleary-eyed one". In Arabic, the short form would be identical with the name of Procyon.
In Chinese, 南河 (Nán Hé), meaning South River, refers to an asterism consisting of β Canis Minoris, Procyon and ε Canis Minoris. Consequently, β Canis Minoris itself is known as 南河二 (Nán Hé èr, English: the Second Star of South River.)
From parallax measurements, the distance to this star is about 162 light-years (50 parsecs). It has an apparent visual magnitude of 2.89, making it easily visible to the naked eye. Beta Canis Minoris has about 3.5 times the Sun's mass and is rotating rapidly with a projected rotational velocity of 210 km s–1, which gives a lower bound on the azimuthal rotational velocity along the star's equator. The actual rotation rate may be about once per day.
The stellar classification of this star is B8 Ve. A luminosity class V star belongs on the main sequence, which means it is presently generating energy through the thermonuclear fusion of hydrogen at its core. The star is radiating this energy from its outer envelope at an effective temperature of 12,050 K, giving it a blue-white hue typical of B-type stars. An 'e' classification indicates that the spectrum contains emission lines, which means this is a Be star that is surrounded by a thin, circumstellar disk made of gaseous material ejected from the star. This hot, gaseous disk is about three times the radius of the star.
Beta Canis Minoris shows little variation in brightness, but it does display changes in the hydrogen emission coming from the gaseous disk. Examination with the Canadian MOST space telescope reveals low amplitude changes in luminosity from the star. This variation has a cyclic pattern formed from multiple overlapping frequencies, with the dominant frequencies being 3.257 and 3.282 cycles per day. As such, it belongs to a class called slowly pulsating Be stars, or SPBe.
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