Gomeisa
 Position of Beta Canis Minoris. |
|
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Canis Minor |
| Right ascension | 07h 27m 09.04174s |
| Declination | +08° 17′ 21.5368″ |
| Apparent magnitude (V) | 2.89 |
| Characteristics | |
| Spectral type | B8 Ve |
| U−B color index | –0.28 |
| B−V color index | –0.09 |
| Variable type | SPBe |
| Astrometry | |
| Radial velocity (Rv) | +22 km/s |
| Proper motion (μ) |
RA: -51.76 mas/yr Dec.: -38.29 mas/yr |
| Parallax (π) | 20.17 ± 0.20mas |
| Distance | 162 ± 2 ly (49.6 ± 0.5 pc) |
| Details | |
| Mass | 3.5 M☉ |
| Radius | 3.5 R☉ |
| Luminosity | 195 L☉ |
| Surface gravity (log g) | 3.51 cgs |
| Temperature | 11,772 K |
| Rotational velocity (v sin i) | 210 km/s |
| Age |
160+20 −60 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Beta Canis Minoris (β Canis Minoris, abbreviated Beta CMi, β CMi), also named Gomeisa, is a star in the constellation of Canis Minor. In the night sky it is notable for its proximity to the prominent star Procyon.
β Canis Minoris (Latinised to Beta Canis Minoris) is the star's Bayer designation.
The traditional name Gomeisa 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 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included Gomeisa for this star.
In Chinese, 南河 (Nán Hé), meaning South River, refers to an asterism consisting of β Canis Minoris, Procyon and Epsilon 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.
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