53 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis,[9] located 290 light years away from the Sun as determined by parallax measurements.[2] It has the variable star designation AX Camelopardalis; 53 Camelopardalis is the Flamsteed designation.[9] This object is dimly visible to the naked eye as a white hued star with a baseline apparent visual magnitude of +6.02.[3] It is a single-lined spectroscopic binary[10] system with an orbital period of 6.63 years and a high eccentricity of about 0.7.[8] The "a sin i" value of the primary is 280 Gm (1.9 AU), where a is the semimajor axis and i is the orbital inclination.[8]

The visible component is a well-studied magnetic Ap star[8] with a stellar classification of A3VpSrSiCrEu[5] and a visual magnitude of 6.3.[4] The magnetic field topology of 53 Camelopardalis is complex, and is accompanied by abundance variations across the surface of elements like silicon, calcium, titanium, iron, and neodymium.[8]

Tadeusz Jarzębowski discovered that 53 Camelopardalis is a variable star, in 1960.[11] It is classified as an Alpha2 Canum Venaticorum type variable star and the combined brightness of the system varies from magnitude +6.00 down to +6.05 with a rotationally-modulated period of 8.0278 days.[6]

The primary has 2.1 times the mass of the Sun and 2.4 times the Sun's radius. It is spinning with a projected rotational velocity of 12.5 km/s and a rotation period of 8.0268 days. The inclination angle of the pole is estimated to be 57°±5°. The star is about 615 million years old and is radiating 25 times the luminosity of the Sun from its photosphere at an effective temperature of 8,400 K.[8]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e f 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.
  3. ^ a b c d e 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.
  4. ^ a b Malkov, O. Yu.; et al. (2012), "Dynamical Masses of a Selected Sample of Orbital Binaries", Astronomy & Astrophysics, 546: 5, Bibcode:2012A&A...546A..69M, doi:10.1051/0004-6361/201219774, A69
  5. ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement Series, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182
  6. ^ 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, doi:10.1134/S1063772917010085, S2CID 125853869.
  7. ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 2025-02-08.
  8. ^ a b c d e f g Carrier, F.; et al. (October 2002), "Multiplicity among chemically peculiar stars. II. Cool magnetic Ap stars", Astronomy and Astrophysics, 394: 151–169, arXiv:astro-ph/0208082, Bibcode:2002A&A...394..151C, doi:10.1051/0004-6361:20021122, S2CID 14223227.
  9. ^ a b c "53 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-22.
  10. ^ Kochukhov, O.; et al. (February 2004), "Magnetic Doppler imaging of 53 Camelopardalis in all four Stokes parameters", Astronomy and Astrophysics, 414 (2): 613–632, Bibcode:2004A&A...414..613K, doi:10.1051/0004-6361:20031595
  11. ^ Jarzębowski, T. (1960). "Relation between Light-variation and Magnetic Variation in Magnetic Alpha Variables". Acta Astronomica. 10: 31–52. Bibcode:1960AcA....10...31J. Retrieved 29 December 2024.
Allikas: Https://en.wikipedia.org/wiki/53_Camelopardalis
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