Astronomy:11 Camelopardalis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[2] mas |
| Distance | 690 ± 20 ly (210 ± 5 pc) |
| Absolute magnitude (MV) | −1.38[5] |
| Details | |
| Mass | 6.0±1.2[7] M☉ |
| Radius | 7.87[8] R☉ |
| Luminosity | 1,766+131 −122[7] L☉ |
| Surface gravity (log g) | 4.00±0.35[7] cgs |
| Temperature | 17,240±560[7] K |
| Rotational velocity (v sin i) | 95±6[7] km/s |
| Age | 25±3[9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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.
This is a main sequence Be star with a stellar classification of B3 Ve.[4] John R. Percy et al. discovered that 11 Camelopardalis is a variable star in 1979, and published that finding in 1981.[12] It was given its variable star designation in 1987.[13] 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.[14] It is 25[9] million years old with around six[7] times the mass of the Sun.
References
- ↑ "Hipparcos Tools Interactive Data Access". ESA. https://www.cosmos.esa.int/web/hipparcos/interactive-data-access.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ BV Cam, AAVSO, https://www.aavso.org/vsx/index.php?view=detail.top&oid=4632, retrieved 2022-07-26.
- ↑ 4.0 4.1 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, doi:10.1086/190820, Bibcode: 1982ApJS...50...55S.
- ↑ 5.0 5.1 5.2 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 6.0 6.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/s1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 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, doi:10.1051/0004-6361/201628760, Bibcode: 2016A&A...595A.132Z.
- ↑ 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. doi:10.1051/0004-6361/202142146. Bibcode: 2022A&A...657A...7K.
- ↑ 9.0 9.1 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, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T.
- ↑ "11 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=11+Cam.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Percy, J. R.; Jakate, S. M.; Matthews, J. M. (January 1981). "Short-period light variations in Be stars". Astronomical Journal 86: 53–61. doi:10.1086/112855. Bibcode: 1981AJ.....86...53P. https://articles.adsabs.harvard.edu/pdf/1981AJ.....86...53P. Retrieved 29 December 2024.
- ↑ Kholopov, P. N.; Samus, N. N.; Kazarovets, E. V.; Kireeva, N. N. (August 1987). "The 68th Name-List of Variable Stars". Information Bulletin on Variable Stars 3058: 1. Bibcode: 1987IBVS.3058....1K. https://ibvs.konkoly.hu/pub/ibvs/3001/3058.pdf. Retrieved 29 December 2024.
- ↑ 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.
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