11 Camelopardalis
Star in the constellation Camelopardalis
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11 Camelopardalis is a single[11] star in the northern circumpolar constellation of Camelopardalis, located around 690 light years away from the Sun as determined by parallax. It has the variable star designation BV Camelopardalis; 11 Camelopardalis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of +5.22.[5] It forms a double star with 12 Camelopardalis, which is only 3 arcminutes away.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 05h 06m 08.45273s[2] |
| Declination | +58° 58′ 20.5432″[2] |
| Apparent magnitude (V) | 5.08[3] |
| Characteristics | |
| Spectral type | B3 Ve[4] |
| B−V color index | −0.080[5] |
| Variable type | Be[6] |
| Astrometry | |
| Proper motion (μ) | RA: −6.264[2] mas/yr Dec.: −7.118[2] mas/yr |
| Parallax (π) | 4.7543±0.1224 mas[2] |
| Distance | 690 ± 20 ly (210 ± 5 pc) |
| Absolute magnitude (MV) | −1.38[5] |
| Details | |
| Mass | 6.0±1.2[7] M☉ |
| Radius | 7.87[8] R☉ |
| Luminosity | 1,766+131 −122[7] L☉ |
| Surface gravity (log g) | 4.00±0.35[7] cgs |
| Temperature | 17,240±560[7] K |
| Rotational velocity (v sin i) | 95±6[7] km/s |
| Age | 25±3[9] Myr |
| Other designations | |
| 11 Cam, BV Cam, BD+58°804, GC 6193, HD 32343, HIP 23734, HR 1622, SAO 25001, CCDM 05062+5900, WDS J05061+5858A[10] | |
| Database references | |
| SIMBAD | data |
This is a main sequence Be star with a stellar classification of B3 Ve.[4] John R. Percy et al. discovered that 11 Camelopardalis is a variable star in 1979, and published that finding in 1981.[12] It was given its variable star designation in 1987.[13] Samus et al. (2017) classify it as a Be variable, rather than a Gamma Cassiopeiae type, and it ranges from a peak Hipparcos magnitude of 5.10 down to 5.22.[6] The star is spinning with a projected rotational velocity of 95 km/s,[7] but is being viewed from an extreme pole-on position. Hence it is spinning much more rapidly than indicated. Outbursts of hydrogen emission lines have been observed, as well as rapid changes in hydrogen line profiles.[14] It is 25[9] million years old with around six[7] times the mass of the Sun.