53 Camelopardalis
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 08h 01m 42.44039s[2] |
| Declination | +60° 19′ 27.8068″[2] |
| Apparent magnitude (V) | 6.02[3] (6.3 + 7.5)[4] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | A3VpSrSiCrEu[5] |
| B−V color index | 0.158±0.005[3] |
| Variable type | α2 CVn[6] |
| Astrometry | |
| Radial velocity (Rv) | −2.2[3] km/s |
| Proper motion (μ) | RA: −25.627[2] mas/yr Dec.: −26.731[2] mas/yr |
| Parallax (π) | 11.2405±0.2219 mas[2] |
| Distance | 290 ± 6 ly (89 ± 2 pc) |
| Absolute magnitude (MV) | 1.05[3] |
| Orbit[7] | |
| Period (P) | 6.6504±0.0089 |
| Semi-major axis (a) | 0.055±0.018″ |
| Eccentricity (e) | 0.706±0.024 |
| Inclination (i) | 55.4±2.9° |
| Longitude of the node (Ω) | 118.3±20.1° |
| Periastron epoch (T) | 2001.2281±0.025 |
| Argument of periastron (ω) (secondary) | 8.3±1.8° |
| Semi-amplitude (K1) (primary) | 12.08±0.45[8] km/s |
| Details[8] | |
| 53 Cam A | |
| Mass | 2.074±0.012 M☉ |
| Radius | 2.36±0.10 R☉ |
| Luminosity | 24.9±1.15 L☉ |
| Surface gravity (log g) | 3.70±0.10 cgs |
| Temperature | 8,400±150 K |
| Rotation | 8.02681±0.00004 d |
| Rotational velocity (v sin i) | 12.5±0.5 km/s |
| Age | 615+56 −51 Myr |
| Other designations | |
| 53 Cam, AX Cam, BD+60°1105, FK5 302, GC 10822, HD 65339, HIP 39261, HR 3109, SAO 14402, CCDM 08017+6019, WDS J08017+6019[9] | |
| Database references | |
| SIMBAD | data |
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
[edit]- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 3 4 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.
- 1 2 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
- 1 2 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
- 1 2 Samus, N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 2025-02-08.
- 1 2 3 4 5 6 7 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.
- 1 2 3 "53 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-22.
- ↑ 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
- ↑ Jarzębowski, T. (1960). "Relation between Light-variation and Magnetic Variation in Magnetic Alpha Variables". Acta Astronomica. 10: 31–52. Bibcode:1960AcA....10...31J.
