7 Camelopardalis
Location of 7 Camelopardalis (circled in red) | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | 4.43[2] (4.49 + ? + 7.90 + 11.30)[3] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | A1 V[4] |
| B−V color index | −0.017±0.003[2] |
| Astrometry | |
| Radial velocity (Rv) | −9.5±3.7[5] km/s |
| Proper motion (μ) | RA: −24.51[1] mas/yr Dec.: +7.71[1] mas/yr |
| Parallax (π) | 8.77±0.60 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | −0.84[2] |
| Orbit[6] | |
| Primary | 7 Cam Aa |
| Name | 7 Cam Ab |
| Period (P) | 3.884 d |
| Eccentricity (e) | 0 |
| Periastron epoch (T) | 2,457,726.05 JD |
| Argument of periastron (ω) (secondary) | 0° |
| Semi-amplitude (K1) (primary) | 34.9±0.2 km/s |
| Details | |
| 7 Cam Aa | |
| Mass | 3.16±0.10[7] M☉ |
| Luminosity | 221.6+36.8 −31.5[7] L☉ |
| Temperature | 9,226+236 −231[7] K |
| Rotational velocity (v sin i) | 40[7] km/s |
| Other designations | |
| Template:Odlist[8] | |
| Database references | |
| SIMBAD | data |
7 Camelopardalis is a multiple star system[9] in the northern circumpolar constellation of Camelopardalis. It is located approximately 370 light years from the Sun, as determined from its parallax.[1] This system is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 4.43.[2] It is moving closer to the Earth with a heliocentric radial velocity of −10 km/s.[5]
The primary member of the group, designated component A, is a single-lined spectroscopic binary system with a circular orbit and a period of 3.88 days.[6] The visible component of this pair is a magnitude 4.49[3] A-type main-sequence star with a stellar classification of A1 V.[4] It has 3.2 times the mass of the Sun and is spinning with a projected rotational velocity of 40 km/s. The star is radiating 222 times the Sun's luminosity from its photosphere at an effective temperature of 9,226 K.[7]
The magnitude 7.90[3] component B has an orbital solution with the Aa/Ab pair, which yields a period of 284 years and an eccentricity of 0.74. However, Drummond (2014) found the data to be discordant and instead determined that they are an optical pair with no physical association.[10] The fourth member, component C, is a magnitude 11.30 star at an angular separation of 25.50″ along a position angle of 242° from the primary, as of 2003.[3] It shares a common proper motion with the primary star.[11]
References
- ^ a b c d e f Page Module:Citation/CS1/styles.css has no content.van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
- ^ a b c d Page Module:Citation/CS1/styles.css has no content.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 c d Page Module:Citation/CS1/styles.css has no content.Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ a b Page Module:Citation/CS1/styles.css has no content.de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ a b Page Module:Citation/CS1/styles.css has no content.Heyne, T.; Mugrauer, M.; Bischoff, R.; Wagner, D.; Hoffmann, S.; Lux, O.; Munz, V.; Geymeier, M.; Neuhäuser, R. (2020). "Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533". Astronomische Nachrichten. 341 (1): 99–117. arXiv:1912.05343. Bibcode:2020AN....341...99H. doi:10.1002/asna.202013683. S2CID 209202812.
- ^ a b c d e Page Module:Citation/CS1/styles.css has no content.Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
- ^ Page Module:Citation/CS1/styles.css has no content."7 Cam". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-15.
{{cite web}}: Invalid|mode=Script error: No such module "Citation mode".(help) - ^ Page Module:Citation/CS1/styles.css has no content.Eggleton, P. P.; et al. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Page Module:Citation/CS1/styles.css has no content.Drummond, Jack D. (March 2014), "Binary Stars Observed with Adaptive Optics at the Starfire Optical Range", The Astronomical Journal, 147 (3): 10, Bibcode:2014AJ....147...65D, doi:10.1088/0004-6256/147/3/65, 65.
- ^ Template:Cite Gaia EDR3
