Lambda Cassiopeiae

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λ Cassiopeiae
File:Lambda cassiopeiae diagram.jpg
Map of the Bayer-designated stars in Cassiopeia. Lambda Cassiopeiae is circled.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cassiopeia[1]
Right ascension Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 4.772[3]
(5.33 / 5.62)[4]
Characteristics
Spectral type B8 Vnn[1]
U−B Template:Engvar −0.35[5]
B−V Template:Engvar −0.10[5]
Astrometry
Radial velocity (Rv)Template:Val[6] km/s
Proper motion (μ) RA: Template:Val[2] mas/yr
Dec.: Template:Val[2] mas/yr
Parallax (π)8.64±0.43 mas[2]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)−0.57[1]
Orbit[4]
Period (P)Template:Val yr
Semi-major axis (a)Template:Val
Eccentricity (e)Template:Val
Inclination (i)Template:Val°
Longitude of the node (Ω)Template:Val°
Periastron epoch (T)Template:Val
Argument of periastron (ω)
(secondary)
Template:Val°
Details
λ Cas A
MassTemplate:Val[7] Template:Solar mass
Radius3.50[8] Template:Solar radius
Luminosity255[1] Template:Solar luminosity
Surface gravity (log g)Template:Val[7] cgs
TemperatureTemplate:Val[7] K
Rotational velocity (v sin i)253[9] km/s
AgeTemplate:Val[7] Myr
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
Template:Odlist
Database references
SIMBADλ Cas
λ Cas A
λ Cas B

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File:Lambda Cassiopeiae.jpg
λ Cassiopeiae in optical light

Lambda Cassiopeiae, Latinized from λ Cassiopeiae, is a binary star system, in the northern constellation of Cassiopeia. The system has a combined apparent magnitude of +4.74, making it faintly visible to the naked eye. With an annual parallax shift of 8.64 mass,[2] it is approximately 380 light years from Earth. The system is moving closer to the Sun with a radial velocity of −12 km/s.[6]

Both components are blue-white B-type main-sequence stars. The brighter member, component A, has an apparent magnitude of +5.5, while its companion, component B, has an apparent magnitude of +5.8. The two stars are separated by 0.6 arcseconds and complete one orbit around their common centre of mass about once every 250 years.[4] The primary displays an infrared excess, possibly due to a debris disk or other orbiting material.[8]

References

Template:Reflist

Template:Stars of Cassiopeia

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