Epsilon Cassiopeiae
 Segin is the leftmost star in the "W" |
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| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 01h 54m 23.72567s |
| Declination | +63° 40′ 12.3628″ |
| Apparent magnitude (V) | 3.37 |
| Characteristics | |
| Spectral type | B3 V |
| U−B color index | -0.62 |
| B−V color index | -0.15 |
| Variable type | Periodic |
| Astrometry | |
| Radial velocity (Rv) | −8.1 km/s |
| Proper motion (μ) |
RA: +32.09 mas/yr Dec.: −18.94 mas/yr |
| Parallax (π) | 7.92 ± 0.43mas |
| Distance | 410 ± 20 ly (126 ± 7 pc) |
| Details | |
| Mass | 9.2 ± 0.2 M☉ |
| Radius | 6 R☉ |
| Luminosity | 2,500 L☉ |
| Surface gravity (log g) | 3.5 cgs |
| Temperature | 15,174 K |
| Rotational velocity (v sin i) | 30 km/s |
| Age | 15.4 ± 3.0 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Epsilon Cassiopeiae (ε Cas, ε Cassiopeiae) is a star system in the constellation Cassiopeia. It has the traditional name Segin. With an apparent visual magnitude of 3.4, this is one of the brightest stars in the constellation. It is located at a distance of around 390–430 light-years (120–130 parsecs).
ε Cassiopeiae has a stellar classification of B3 V, indicating that it is a main sequence star fusing hydrogen in its core. Cote et al. (2003) indicate that it displays the spectral properties of a Be star, even though it is not categorized as such. The presence of emission lines in the spectrum indicates the presence of a circumstellar shell of gas that has been thrown off by the star. The outer atmosphere has an effective temperature of 15,174 K (14,901 °C; 26,854 °F), giving it the blue-white hue of a B-type star.
The distance to this star has been determined directly using parallax measurements, yielding a value of around 390–430 light-years (120–130 parsecs). The interferometer-measured angular diameter is 0.43 milliarcseconds. At the estimated distance of this star, this yields a physical size of roughly 6 times the radius of the Sun.
Observation during the Hipparcos mission suggest that the star may undergo weak periodic variability. The amplitude of this variation is 0.0025 in magnitude with a frequency of 11.17797 times per day, or one cycle every 2.15 hours. The signal-to-noise ratio for this measured variation is 4.978. Hipparcos measurements of the space velocity components for this star suggest that it is a member of the Cas-Tau group of co-moving stars, with a 93% likelihood. This group may be kinematically associated with the alpha Persei cluster, indicating that the Cas-Tau group, including Epsilon Cassiopeiae, may have been separated from the cluster through tidal interactions.
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