Astronomy:2 Camelopardalis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 04h 39m 58.06187s[1] |
| Declination | +53° 28′ 22.4654″[1] |
| Apparent magnitude (V) | 5.36[2] |
| Characteristics | |
| A | |
| Spectral type | A8V[3] |
| U−B color index | +0.05[2] |
| B−V color index | +0.34[2] |
| Astrometry | |
| Radial velocity (Rv) | +20.1±3.2[4] km/s |
| Proper motion (μ) | RA: +44.269[1] mas/yr Dec.: −77.004[1] mas/yr |
| Parallax (π) | 15.3220 ± 0.3790[1] mas |
| Distance | 213 ± 5 ly (65 ± 2 pc) |
| Orbit[5] | |
| Primary | 2 Cam A |
| Companion | 2 Cam B |
| Period (P) | 26.34 ± 0.05 yr |
| Semi-major axis (a) | 0.1727 ± 0.0023″ |
| Eccentricity (e) | 0.846 ± 0.005 |
| Inclination (i) | 113.3 ± 3.4° |
| Longitude of the node (Ω) | 12.6 ± 2.5° |
| Periastron epoch (T) | B 1988.98 ± 0.03 |
| Argument of periastron (ω) (secondary) | 42.9 ± 2.6° |
| Orbit[5] | |
| Primary | 2 Cam AB |
| Companion | 2 Cam C |
| Period (P) | 660 yr |
| Semi-major axis (a) | 1.666 ± 0.019″ |
| Eccentricity (e) | 0.405 ± 0.015 |
| Inclination (i) | 132.5 ± 1.9° |
| Longitude of the node (Ω) | 286.2 ± 1.8° |
| Periastron epoch (T) | B 2011.7 ± 2.7 |
| Argument of periastron (ω) (secondary) | 105.1 ± 5.4° |
| Details[5] | |
| A | |
| Mass | 1.94 M☉ |
| B | |
| Mass | 1.45 M☉ |
| C | |
| Mass | 1.5 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | 2 Cam |
| 2 Cam AB | |
| 2 Cam C | |
2 Camelopardalis is a triple star[6] system in the northern circumpolar constellation of Camelopardalis, next to the southern constellation border with Perseus. It is dimly visible to the naked eye with a combined apparent visual magnitude of 5.36.[2] The system is located at a distance of about 213 light-years (65 parsecs) from the Sun, based on its parallax.[1] It is drifting further away with a radial velocity of +20 km/s.[4]
The primary member of 2 Camelopardalis, designated component A, is an A-type main-sequence star with a spectral type of A8V. It has an apparent magnitude of 5.86, and has a secondary with an apparent magnitude of 7.35, designated component B.[7] The two orbit each other on a very eccentric orbit with a period of 26.34 years.[5] Further out, there is an eight-magnitude companion (designated component C), orbiting once every few hundred years.[5] As the third star was previously thought to be relatively massive for its luminosity, it was suspected of being a binary star itself,[8] but the current estimate of component C's magnitude as a single star matches its absolute magnitude.[5]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M. http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?1986EgUBV........0M&db_key=AST&nosetcookie=1.
- ↑ Appenzeller, Immo (1967). "MK Spectral Types for 185 Bright Stars". Publications of the Astronomical Society of the Pacific 79 (467): 102. doi:10.1086/128449. Bibcode: 1967PASP...79..102A.
- ↑ 4.0 4.1 Holmberg, J.; Nordström, B.; Andersen, J. (2007). "The Geneva-Copenhagen survey of the Solar neighbourhood II". Astronomy and Astrophysics 475 (2): 519. doi:10.1051/0004-6361:20077221. Bibcode: 2007A&A...475..519H.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Tokovinin, A. (2021). "Inner and Outer Orbits in 13 Resolved Hierarchical Stellar Systems". The Astronomical Journal 161 (3): 144. doi:10.3847/1538-3881/abda42. Bibcode: 2021AJ....161..144T.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (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.
- ↑ "Sixth Catalog of Orbits of Visual Binary Stars". United States Naval Observatory. http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/orb6. Retrieved 4 April 2017.
- ↑ Heintz, W. D. (1996). "A Study of Multiple-Star Systems". The Astronomical Journal 111: 408. doi:10.1086/117792. Bibcode: 1996AJ....111..408H.
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