Kappa Cassiopeiae
 Location of κ Cassiopeiae (circled) |
|
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Cassiopeia |
| Right ascension | 00h 32m 59.991s[1] |
| Declination | +62° 55′ 54.42″[1] |
| Apparent magnitude (V) | 4.16[2] |
| Characteristics | |
| Spectral type | BC0.7 Ia[2] |
| Apparent magnitude (U) | 3.50[3] |
| Apparent magnitude (B) | 4.276[3] |
| Apparent magnitude (J) | 4.141[3] |
| Apparent magnitude (H) | 4.148[3] |
| Apparent magnitude (K) | 4.013[3] |
| U−B color index | -0.776[3] |
| B−V color index | +0.0869[3] |
| J−H color index | -0.0069[3] |
| J−K color index | +0.128[3] |
| Variable type | α Cyg[4] |
| Astrometry | |
| Radial velocity (Rv) | 0.30[5] km/s |
| Proper motion (μ) | RA: 3.65 ± 0.17[1] mas/yr Dec.: –2.07 ± 0.16[1] mas/yr |
| Parallax (π) | 0.73 ± 0.17[1] mas |
| Distance | approx. 4,000 ly (approx. 1,400 pc) |
| Absolute magnitude (MV) | −7.00[6] |
| Details[6] | |
| Mass | 33 M☉ |
| Radius | 33.0 R☉ |
| Luminosity | 302,000 L☉ |
| Surface gravity (log g) | 2.75 cgs |
| Temperature | 23,500 K |
| Rotational velocity (v sin i) | 66[7] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Kappa Cassiopeiae (κ Cas, κ Cassiopeiae) is a star in the constellation Cassiopeia.
κ Cassiopeiae has an unusual spectrum that has anomalously weak nitrogen lines, taken as an actual nitrogen deficiency in the atmosphere. This is indicated by the modified letter C. It is also interpolated to BC0.7, being slightly hotter than a standard B1 star.[8][9] It is assumed to be a mamber of the Cas OB14 stellar association at about 1,100 parsecs, while its distance found from the Hipparcos parallax is 1,369 parsecs.[9]
It is classified as an Alpha Cygni type variable star and its brightness varies by a few hundredths of a magnitude. Periods of two hours,[10] nine days,[11] and 2.65 days[12] have been reported from observations at different times.
It is a runaway star, moving at around 2.5 million mph relative to its neighbors (1,100 kilometers per second). Its magnetic field and wind of particles creates a visible bow shock 4 light-years ahead of it, colliding with the diffuse, and usually invisible, interstellar gas and dust. This is about the same distance that we are from Proxima Centauri, the nearest star to the sun.[13]
References
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