11 Camelopardalis

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11 Camelopardalis
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Camelopardalis
Right ascension  05h 06m 08.45236s[1]
Declination +58° 58′ 20.5486″[1]
Apparent magnitude (V) 5.22[2]
Characteristics
Spectral type B3 Ve[3]
B−V color index −0.080[2]
Variable type Be[4]
Astrometry
Proper motion (μ) RA: −6.078[1] mas/yr
Dec.: −7.490[1] mas/yr
Parallax (π)4.6189 ± 0.1620[1] mas
Distance710 ± 20 ly
(217 ± 8 pc)
Absolute magnitude (MV)−1.38[2]
Details
Mass6.0±1.2[5] M
Luminosity1,766+131
−122
[5] L
Surface gravity (log g)4.00±0.35[5] cgs
Temperature17,240±560[5] K
Rotational velocity (v sin i)95±6[5] km/s
Age25±3[6] Myr
Other designations
11 Cam, BV Cam, BD+58°804, GC 6193, HD 32343, HIP 23734, HR 1622, SAO 25001, CCDM 05062+5900, WDS J05061+5858A[7]
Database references
SIMBADdata
11 Camelopardalis and its reddish companion 12 Camelopardalis

11 Camelopardalis is a single[8] star in the northern circumpolar constellation of Camelopardalis, located around 710 light years away from the Sun as determined by parallax. It has the variable star designation BV Camelopardalis; 11 Camelopardalis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of +5.22.[2] It forms a double star with 12 Camelopardalis, which is only 3 arcminutes away.

This is a main sequence Be star with a stellar classification of B3 Ve.[3] Samus et al. (2017) classify it as a Be variable, rather than a Gamma Cassiopeiae type, and it ranges in magnitude from a peak of 5.10 down to 5.22.[4] The star is spinning with a projected rotational velocity of 95 km/s,[5] but is being viewed from an extreme pole-on position. Hence it is spinning much more rapidly than indicated. Outbursts of hydrogen emission lines have been observed, as well as rapid changes in hydrogen line profiles.[9] It is 25[6] million years old with around six[5] times the mass of the Sun.

References[edit]

  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  3. ^ a b Slettebak, A. (1982), "Spectral types and rotational velocities of the brighter Be stars and A-F type shell stars", Astrophysical Journal Supplement Series, 50: 55, Bibcode:1982ApJS...50...55S, doi:10.1086/190820.
  4. ^ a b Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S.
  5. ^ a b c d e f g Zorec, J.; et al. (November 2016), "Critical study of the distribution of rotational velocities of Be stars. I. Deconvolution methods, effects due to gravity darkening, macroturbulence, and binarity", Astronomy & Astrophysics, 595: 26, Bibcode:2016A&A...595A.132Z.
  6. ^ a b Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x.
  7. ^ "11 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-15.
  8. ^ Eggleton, P. P.; et al. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x.
  9. ^ Ballereau, D.; et al. (May 1987), "Hα echelle spectroscopy of Be stars: an atlas.", Revista Mexicana de Astronomia y Astrofisica, 15 (1): 29–52, Bibcode:1987RMxAA..15...29B.