HD 21389

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HD 21389
Camelopardalis constellation map.svg
Red circle.svg

Location of CE Camelopardalis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Camelopardalis
Right ascension 03h 29m 54.74413s[1]
Declination +58° 52′ 43.4995″[1]
Apparent magnitude (V) 4.54[2]
Characteristics
Spectral type A0 Iae[2]
U−B color index −0.11[3]
B−V color index +0.56[3]
Variable type α Cyg[4]
Astrometry
Radial velocity (Rv) −6.20[5] km/s
Proper motion (μ) RA: 1.79[1] mas/yr
Dec.: −1.09[1] mas/yr
Parallax (π) 1.30 ± 0.56[1] mas
Distance 975[3] pc
Absolute magnitude (MV) −7.20[3]
Details[2]
Mass 19.3 M
Radius 97 R
Luminosity 55,000 L
Surface gravity (log g) 1.75 cgs
Temperature 9,730 K
Rotation 25
Age 11[3] Myr
Other designations
CE Camelopardalis, BD+58°607, HIP 16281, HR 1040, HD 21389, SAO 24061
Database references
SIMBAD data
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)
CE Cam and the surrounding nebulosity at infrared wavelengths (Credit: NASA/JPL-Caltech/UCLA)

HD 21389 is a supergiant variable star in reflection nebula VDB 15, in the constellation Camelopardalis. It is part of the Camelopardalis OB1 association. The near-identical member CS Camelopardalis lies half a degree to the north.

Since 1943, the spectrum of CE Cam has served as one of the stable anchor points by which other stars are classified.[6]

CE Camelopardalis is some 19 times as massive as the Sun and 55,000 timers as luminous. Hohle and colleagues, using the parallax, extinction and analysis of spectrum, came up with a mass 14.95 ± 0.41 times that and luminosity 62,679 times that of the Sun.[7]

CE Cam is embedded in a large dusty molecular cloud, part of which it illuminates as a reflection nebula (vdB15 or BFS 29). This is a region of ongoing star formation with stars aged from one to a hundred million years old. CE Cam itself is thought to be around 11 million years old, long enough to have exhausted its core hydrogen and evolved away from the main sequence into a supergiant.[3]

References[edit]

  1. ^ a b c d e Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c Shultz, M.; Wade, G. A.; Petit, V.; Grunhut, J.; Neiner, C.; Hanes, D.; MiMeS Collaboration (2014). "An observational evaluation of magnetic confinement in the winds of BA supergiants". Monthly Notices of the Royal Astronomical Society 438 (2): 1114. arXiv:1311.5116. Bibcode:2014MNRAS.438.1114S. doi:10.1093/mnras/stt2260. 
  3. ^ a b c d e f Lyder, David A. (2001). "The Stars in Camelopardalis OB1: Their Distance and Evolutionary History". The Astronomical Journal 122 (5): 2634. Bibcode:2001AJ....122.2634L. doi:10.1086/323705. 
  4. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S 1. Bibcode:2009yCat....102025S. 
  5. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. 
  6. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society 25: 1319, Bibcode:1993AAS...183.1710G, retrieved 2012-02-04 
  7. ^ Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355 

External links[edit]