Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Camelopardalis |
Right ascension | 05h 12m 22.43769s [2] |
Declination | +73° 56′ 48.03820″ [2] |
Apparent magnitude (V) | 5.49 [3] (5.34 to 5.58) [4] |
Characteristics | |
Spectral type | B9.5VpSi [5] |
B−V color index | −0.108±0.003 [3] |
Variable type | α2 CVn [4] |
Astrometry | |
Radial velocity (Rv) | +9.3±2.8 [3] km/s |
Proper motion (μ) |
RA: +6.033
[2]
mas/
yr Dec.: –27.088 [2] mas/ yr |
Parallax (π) | 10.5286 ± 0.2275 mas [2] |
Distance | 310 ± 7
ly (95 ± 2 pc) |
Absolute magnitude (MV) | +0.13 [3] |
Details | |
Mass | 3.05±0.13 [6] M☉ |
Radius | 2.9±0.4 [7] R☉ |
Luminosity | 110 [6] L☉ |
Surface gravity (log g) | 4.15±0.11 [7] cgs |
Temperature | 11,561 [6] K |
Rotation | 2.73332 days [7] |
Rotational velocity (v sin i) | 23 [8] km/s |
Other designations | |
Database references | |
SIMBAD | data |
BN Camelopardalis is a suspected astrometric binary [10] in the northern circumpolar constellation of Camelopardalis. It appears as a variable star that is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude that fluctuates around 5.49. [3] The system is located at a distance of around 310 light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +9 km/s. [3]
The visible component is a weakly magnetic [11] chemically peculiar star [12] [13] with a stellar classification of B9.5VpSi, [5] matching a B-type main-sequence star with an anomalous abundance of silicon. It is a variable star [14] that ranges in brightness from 5.34 down to 5.58. [4] Samus et al. (2017) have it categorized as an α2 Canum Venaticorum variable with a period of 2.7347 days, [4] while Adelman and Sutton (2007) found a period of 2.73501 days. [12] The star has three times the mass and radius of the Sun and is radiating 110 times the Sun's luminosity from its photosphere at an effective temperature of 11,561 K. [7] [6]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Camelopardalis |
Right ascension | 05h 12m 22.43769s [2] |
Declination | +73° 56′ 48.03820″ [2] |
Apparent magnitude (V) | 5.49 [3] (5.34 to 5.58) [4] |
Characteristics | |
Spectral type | B9.5VpSi [5] |
B−V color index | −0.108±0.003 [3] |
Variable type | α2 CVn [4] |
Astrometry | |
Radial velocity (Rv) | +9.3±2.8 [3] km/s |
Proper motion (μ) |
RA: +6.033
[2]
mas/
yr Dec.: –27.088 [2] mas/ yr |
Parallax (π) | 10.5286 ± 0.2275 mas [2] |
Distance | 310 ± 7
ly (95 ± 2 pc) |
Absolute magnitude (MV) | +0.13 [3] |
Details | |
Mass | 3.05±0.13 [6] M☉ |
Radius | 2.9±0.4 [7] R☉ |
Luminosity | 110 [6] L☉ |
Surface gravity (log g) | 4.15±0.11 [7] cgs |
Temperature | 11,561 [6] K |
Rotation | 2.73332 days [7] |
Rotational velocity (v sin i) | 23 [8] km/s |
Other designations | |
Database references | |
SIMBAD | data |
BN Camelopardalis is a suspected astrometric binary [10] in the northern circumpolar constellation of Camelopardalis. It appears as a variable star that is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude that fluctuates around 5.49. [3] The system is located at a distance of around 310 light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +9 km/s. [3]
The visible component is a weakly magnetic [11] chemically peculiar star [12] [13] with a stellar classification of B9.5VpSi, [5] matching a B-type main-sequence star with an anomalous abundance of silicon. It is a variable star [14] that ranges in brightness from 5.34 down to 5.58. [4] Samus et al. (2017) have it categorized as an α2 Canum Venaticorum variable with a period of 2.7347 days, [4] while Adelman and Sutton (2007) found a period of 2.73501 days. [12] The star has three times the mass and radius of the Sun and is radiating 110 times the Sun's luminosity from its photosphere at an effective temperature of 11,561 K. [7] [6]