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Star in the constellation Pavo From Wikipedia, the free encyclopedia
λ Pavonis, Latinized as Lambda Pavonis, is a single,[13] variable star in the southern constellation of Pavo. It is a blue-white hued star that is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.22.[2] This object is located approximately 1,400 light years from the Sun, based upon parallax. It is a member of the Scorpius–Centaurus association.[14]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Pavo |
Right ascension | 18h 52m 13.03427s[1] |
Declination | −62° 11′ 15.3324″[1] |
Apparent magnitude (V) | 4.22[2] (4.00 - 4.26)[3] |
Characteristics | |
Spectral type | B2Ve[4] or B2II–IIIe[5] |
U−B color index | −0.88[6] |
B−V color index | −0.15[2] |
Variable type | γ Cas[3] |
Astrometry | |
Radial velocity (Rv) | +9.0±4.1[7] km/s |
Proper motion (μ) | RA: −1.86[1] mas/yr Dec.: −13.02[1] mas/yr |
Parallax (π) | 2.28 ± 0.18 mas[1] |
Distance | 1,400 ± 100 ly (440 ± 30 pc) |
Absolute magnitude (MV) | −3.97[2] |
Details | |
Mass | 12.5[8] M☉ |
Radius | 9±1[9] (polar) R☉ |
Luminosity | 8,450[2] L☉ |
Temperature | 20,300[10] K |
Rotational velocity (v sin i) | 190[11] km/s |
Other designations | |
Database references | |
SIMBAD | data |
This is a massive Be star, a rapidly rotating hot blue star which has developed a gas disk around it. It is a γ Cassiopeiae variable or shell star which has occasionally brightened to magnitude 4.0.[3] The stellar classification of B2Ve[4] suggests it is a B-type main-sequence star that is generating energy through core hydrogen fusion. This star is spinning rapidly with a projected rotational velocity of 190 km/s.[11] This is giving the star an oblate shape with an equatorial bulge that is an estimated 10% larger than the polar radius.[16] Lambda Pavonis has 12.5[8] times the mass of the Sun and nine times the Sun's polar radius.[9] It is radiating 8,450[2] times the luminosity of the Sun from its photosphere at an effective temperature of 20,300 K.[10]
Variations in signals coming from Lambda Pavonis have led to a debate on whether it is a binary, single or pulsating variable star.[14]
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