53 Camelopardalis is a binary star system in the northern circumpolar constellation of Camelopardalis,[1] 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.[1] 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[4] system with an orbital period of 6.63 years and a high eccentricity of about 0.7.[5] 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.[5]

The visible component is a well-studied magnetic Ap star[5] with a stellar classification of A3VpSrSiCrEu[6] and a visual magnitude of 6.3.[7] 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.[5]

Tadeusz Jarzębowski discovered that 53 Camelopardalis is a variable star, in 1960.[8] 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.[9]

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.[5]

References

  1. ^ "53 Cam". Retrieved 2019-04-22.
  2. ^
  3. ^ 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. ^ Kochukhov, O.; Bagnulo, S.; Wade, G. A.; Sangalli, L.; Piskunov, N.; Landstreet, J. D.; Petit, P.; Sigut, T. A. A. (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
  5. ^ Carrier, F.; North, P.; Udry, S.; Babel, J. (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
  6. ^ 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
  7. ^ Malkov, O. Yu.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (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
  8. ^ Jarzębowski, T. (1960). "Relation between Light-variation and Magnetic Variation in Magnetic Alpha Variables". Acta Astronomica. 10: 31–52. Bibcode:1960AcA....10...31J
  9. ^ Samus, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General Catalogue of Variable Stars", Astronomy Reports. 61 (1): 80–88, 5.1, Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869