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11 Camelopardalis is a single[11] star in the northern circumpolar constellation of Camelopardalis, located around 690 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.[5] It forms a double star with 12 Camelopardalis, which is only 3 arcminutes away.

11 Camelopardalis

A light curve for BV Camelopardalis, plotted from Hipparcos data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Camelopardalis
Right ascension 05h 06m 08.45273s[2]
Declination +58° 58′ 20.5432″[2]
Apparent magnitude (V) 5.08[3]
Characteristics
Spectral type B3 Ve[4]
B−V color index −0.080[5]
Variable type Be[6]
Astrometry
Proper motion (μ) RA: −6.264[2] mas/yr
Dec.: −7.118[2] mas/yr
Parallax (π)4.7543 ± 0.1224 mas[2]
Distance690 ± 20 ly
(210 ± 5 pc)
Absolute magnitude (MV)−1.38[5]
Details
Mass6.0±1.2[7] M☉
Radius7.87[8] R☉
Luminosity1,766+131
−122[7] L☉
Surface gravity (log g)4.00±0.35[7] cgs
Temperature17,240±560[7] K
Rotational velocity (v sin i)95±6[7] km/s
Age25±3[9] 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[10]
Database references
SIMBADdata
11 Camelopardalis and its reddish companion 12 Camelopardalis
11 Camelopardalis and its reddish companion 12 Camelopardalis

This is a main sequence Be star with a stellar classification of B3 Ve.[4] Samus et al. (2017) classify it as a Be variable, rather than a Gamma Cassiopeiae type, and it ranges from a peak Hipparcos magnitude of 5.10 down to 5.22.[6] The star is spinning with a projected rotational velocity of 95 km/s,[7] 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.[12] It is 25[9] million years old with around six[7] times the mass of the Sun.


References


  1. "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  2. Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  3. "BV Cam", International Variable Star Index, AAVSO, retrieved 2022-07-26.
  4. 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.
  5. 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, S2CID 119257644.
  6. Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/s1063772917010085, S2CID 125853869.
  7. 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, doi:10.1051/0004-6361/201628760.
  8. Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: 657. arXiv:2109.10912. Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. S2CID 237605138.
  9. 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, S2CID 118629873.
  10. "11 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-15.
  11. 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, S2CID 14878976.
  12. Ballereau, D.; et al. (May 1987), "Hα echelle spectroscopy of Be stars: an atlas.", Revista Mexicana de Astronomía y Astrofísica, 15 (1): 29–52, Bibcode:1987RMxAA..15...29B.

На других языках

- [en] 11 Camelopardalis

[es] 11 Camelopardalis

11 Camelopardalis (11 Cam / HD 32343 / HR 1622)[1] es una estrella en la constelación de Camelopardalis, la jirafa, de magnitud aparente +5,03. Constituye una estrella doble con 12 Camelopardalis, de la que está separada 3 minutos de arco. Se encuentra aproximadamente a 670 años luz del Sistema Solar.

[ru] 11 Жирафа

11 Жирафа, 11 Camelopardalis, сокращ. 11 Cam — одиночная звезда[9] в циркумполярном созвездии Жирафа. Звезда имеет видимую звёздную величину +5.22m[2], и, согласно шкале Бортля, видна невооружённым глазом даже на засвеченном пригородном небе (англ. Bright suburban sky).


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