Lambda Cassiopeiae

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λ Cassiopeiae
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
Right ascension 00h 31m 46.35935s[1]
Declination +54° 31′ 20.2257″[1]
Apparent magnitude (V) 4.772[2]
(5.33 / 5.62)[3]
Characteristics
Spectral type B8 Vnn[4]
U−B color index −0.35[5]
B−V color index −0.10[5]
Astrometry
Radial velocity (Rv) −12.20±1.3[6] km/s
Proper motion (μ) RA: +41.20±0.29[1] mas/yr
Dec.: −16.54±0.35[1] mas/yr
Parallax (π) 8.64 ± 0.43[1] mas
Distance 380 ± 20 ly
(116 ± 6 pc)
Absolute magnitude (MV) −0.57[4]
Orbit[3]
Period (P) 245.70±35.96 yr
Semi-major axis (a) 0.448±0.028
Eccentricity (e) 0.689±0.119
Inclination (i) 53.6±5.2°
Longitude of the node (Ω) 17.6±9.6°
Periastron epoch (T) 2025.54±4.56
Argument of periastron (ω)
(secondary)
301.0±2.6°
Details
λ Cas A
Mass 2.9+0.45
−0.40
[7] M
Radius 3.50[8] R
Luminosity 255[4] L
Surface gravity (log g) 4.0±0.25[7] cgs
Temperature 12,000±1,000[7] K
Rotational velocity (v sin i) 253[9] km/s
Age 58+104
−48
[7] Myr
Other designations
λ Cas, 14 Cassiopeiae, BD+53° 82, HD 2772, HIP 2505, HR 123, SAO 21489, ADS 434, CCDM J00318+5431
Database references
SIMBAD λ Cas
λ Cas A
λ Cas B

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,[1] 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.[3] The primary displays an infrared excess, possibly due to a debris disk or other orbiting material.[8]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752Freely accessible. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. ^ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. 
  3. ^ a b c "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 16 May 2017. 
  4. ^ a b c Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971Freely accessible, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. 
  5. ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Bibcode:1986EgUBV........0M. 
  6. ^ a b Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv:0705.0878Freely accessible. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. 
  7. ^ a b c d Gullikson, Kevin; et al. (August 2016). "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars". The Astronomical Journal. 152 (2): 13. arXiv:1604.06456Freely accessible. Bibcode:2016AJ....152...40G. doi:10.3847/0004-6256/152/2/40. 40. 
  8. ^ a b Cotten, Tara H.; Song, Inseok (July 2016), "A Comprehensive Census of Nearby Infrared Excess Stars", The Astrophysical Journal Supplement Series, 225 (1): 24, arXiv:1606.01134Freely accessible, Bibcode:2016ApJS..225...15C, doi:10.3847/0067-0049/225/1/15, 15 
  9. ^ Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052Freely accessible, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691.