42 Camelopardalis
Star in the constellation Camelopardalis From Wikipedia, the free encyclopedia
Star in the constellation Camelopardalis From Wikipedia, the free encyclopedia
42 Camelopardalis is a single[11] star in the constellation Camelopardalis,[10] located roughly 770 light years away from the Sun.[1] It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.14.[2] The visual magnitude of the star is diminished by an extinction of 0.22 due to interstellar dust.[12] It is moving further from the Earth with a heliocentric radial velocity of 3 km/s.[4] 42 Camelopardalis has a peculiar velocity of 24.4+1.9
−2.1 km/s and may be a runaway star.[6]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Camelopardalis |
Right ascension | 06h 50m 57.08877s[1] |
Declination | +67° 34′ 18.9814″[1] |
Apparent magnitude (V) | 5.14[2] |
Characteristics | |
Spectral type | B4 IV[3] or B5 V[2] |
B−V color index | −0.152±0.002[2] |
Astrometry | |
Radial velocity (Rv) | 3.2±1.2[4] km/s |
Proper motion (μ) | RA: +0.55[5] mas/yr Dec.: +5.02[5] mas/yr |
Parallax (π) | 4.2456 ± 0.2405 mas[1] |
Distance | 770 ± 40 ly (240 ± 10 pc) |
Absolute magnitude (MV) | −2.10[2] |
Details | |
Mass | 6.5±0.2[6] M☉ |
Radius | 5.6[7] R☉ |
Luminosity (bolometric) | 2,460[8] L☉ |
Temperature | 16,550[8] K |
Rotational velocity (v sin i) | 105[9] km/s |
Age | 50.1±11.7[6] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Observations made in 1933 appeared to suggest this could be a Beta Cephei variable,[13] but this was not confirmed by follow-up measurements.[14] The star has a stellar classification of B4 IV,[3] matching a B-type subgiant star. It has 6.5[6] times the mass of the Sun and about 5.6[7] times the Sun's radius. 42 Camelopardalis is 50[6] million years old with a high rotation rate, showing a projected rotational velocity of 105 km/s.[9] It is radiating 2,460[8] times the luminosity of the Sun from its photosphere at an effective temperature of 16,550 K.[8] This star is notable as demonstrating similarities between the short-period B-type variables and the Cepheid variables.[citation needed]
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