Astronomy:3 Camelopardalis
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 04h 39m 54.682s[2] |
| Declination | +53° 04′ 46.33″[2] |
| Apparent magnitude (V) | 5.073[3] |
| Characteristics | |
| Spectral type | K0III[4] |
| U−B color index | 0.89[5] |
| B−V color index | 1.07[5] |
| Variable type | suspected RS CVn[6] |
| Astrometry | |
| Radial velocity (Rv) | −40.50[7] km/s |
| Proper motion (μ) | RA: −5.68±0.66[2] mas/yr Dec.: −15.00±0.60[2] mas/yr |
| Parallax (π) | 7.72 ± 0.70[2] mas |
| Distance | 420 ± 40 ly (130 ± 10 pc) |
| Absolute magnitude (MV) | −0.82[4] |
| Orbit[8] | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | 121 days |
| Eccentricity (e) | 0.02 |
| Semi-amplitude (K1) (primary) | 28.20 km/s |
| Details | |
| Aa | |
| Mass | 3.3[9] M☉ |
| Radius | 24.1[9] R☉ |
| Luminosity | 259[9] L☉ |
| Surface gravity (log g) | 2.49[10] cgs |
| Temperature | 4,715[9] K |
| Metallicity | −0.21[10] |
| Rotation | 121 days[9] |
| Rotational velocity (v sin i) | 6.7[4] km/s |
| Ab | |
| Mass | 2.37[11] M☉ |
| B | |
| Mass | 0.65[11] M☉ |
| Other designations | |
HR 1467, HD 29317, BD+52°865, HIP 21727, SAO 24743, GC 5658, ADS 3359, CCDM 04399+5305 | |
| Database references | |
| SIMBAD | data |
| Data sources: | |
| Hipparcos Catalogue, CCDM (2002), Bright Star Catalogue (5th rev. ed.) | |
3 Camelopardalis is a spectroscopic and visual binary in the constellation Camelopardalis. It is approximately 496 light years from Earth.
3 Camelopardalis is a visual binary with the two components separated by 3.7". The brighter of the pair is also a single-lined spectroscopic binary with an orbital period of 121 days.[11]
The primary component, 3 Camelopardalis Aa, is an orange K-type giant with a mean apparent magnitude of +5.07. It rotates once every 121 days, matching the orbital period with its close companion. It was thought to be a short period Cepheid variable[12] when it was first investigated, but has since been classified as a probable RS Canum Venaticorum variable. The total amplitude of its variations is less than 0.1 magnitudes.[6]
The spectroscopic companion has not been observed directly and its cannot be detected in the spectrum. It is inferred on the basis of radial velocity variations in its brighter companion. Assuming a circular orbit, it has a mass of 2.37 M☉.
The visual companion is a 12th magnitude star.
References
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ 2.0 2.1 2.2 2.3 2.4 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL. Vizier catalog entry
- ↑ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27. Bibcode: 2000A&A...355L..27H.
- ↑ 4.0 4.1 4.2 Eker, Z; Ak, N. Filiz; Bilir, S; Doğru, D; Tüysüz, M; Soydugan, E; Bakış, H; Uğraş, B et al. (2008). "A catalogue of chromospherically active binary stars (third edition)". Monthly Notices of the Royal Astronomical Society 389 (4): 1722. doi:10.1111/j.1365-2966.2008.13670.x. Bibcode: 2008MNRAS.389.1722E.
- ↑ 5.0 5.1 Hoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H 5050. Bibcode: 1995yCat.5050....0H.
- ↑ 6.0 6.1 NSV 1681
- ↑ Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R. et al. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society 349 (3): 1069–1092. doi:10.1111/j.1365-2966.2004.07588.x. Bibcode: 2004MNRAS.349.1069K.
- ↑ Pourbaix, D; Tokovinin, A. A; Batten, A. H; Fekel, F. C; Hartkopf, W. I; Levato, H; Morrell, N. I; Torres, G et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy & Astrophysics 424 (2): 727–732. doi:10.1051/0004-6361:20041213. Bibcode: 2004A&A...424..727P.
- ↑ 9.0 9.1 9.2 9.3 9.4 Gondoin, P (2007). "The rotation-activity correlation among G and K giants in binary systems". Astronomy & Astrophysics 464 (3): 1101–1106. doi:10.1051/0004-6361:20066751. Bibcode: 2007A&A...464.1101G.
- ↑ 10.0 10.1 Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics 591: A118. doi:10.1051/0004-6361/201628497. Bibcode: 2016A&A...591A.118S.
- ↑ 11.0 11.1 11.2 Tokovinin, A (2008). "Comparative statistics and origin of triple and quadruple stars". Monthly Notices of the Royal Astronomical Society 389 (2): 925–938. doi:10.1111/j.1365-2966.2008.13613.x. Bibcode: 2008MNRAS.389..925T.
- ↑ MacRae, D. A. (1975). "David Dunlap Observatory, University of Toronto, Richmond Hill, Ontario, Canada. Observatory report". Bulletin of the American Astronomical Society 7: 39. Bibcode: 1975BAAS....7...39M.
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