53 Camelopardalis
In today's world, 53 Camelopardalis has become a topic of great importance and relevance. Its impact covers different areas and sectors, from economics to politics, through technology and society in general. Interest in 53 Camelopardalis has been increasing in recent years, awakening the curiosity and attention of a wide spectrum of people. It is important to understand and analyze in depth everything related to 53 Camelopardalis, its origin, evolution, implications and possible future challenges. In this article, we will exhaustively explore this fascinating topic, with the aim of offering a complete and up-to-date overview of 53 Camelopardalis, so that readers can expand their knowledge and better understand the importance of this phenomenon today.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 08h 01m 42.43137s[2] |
| Declination | +60° 19′ 27.8016″[2] |
| Apparent magnitude (V) | 6.02[3] (6.3 + 7.5)[4] |
| Characteristics | |
| Evolutionary stage | main sequence |
| 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: −21.367[2] mas/yr Dec.: −26.386[2] mas/yr |
| Parallax (π) | 11.2327±0.1547 mas[2] |
| Distance | 290 ± 4 ly (89 ± 1 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
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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.
- ^ 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.
- ^ 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
- ^ 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
- ^ 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.
- ^ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. Retrieved 2025-02-08.
- ^ 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.
- ^ a b c "53 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-22.
- ^ 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
- ^ 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.
