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HR 3082
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Camelopardalis[1] |
| Right ascension | 08h 04m 47.0589s[2] |
| Declination | +79° 28′ 46.610″[2] |
| Apparent magnitude (V) | 5.39[1] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | A0p Si[3] or B9.5 IVs[4] |
| B−V color index | −0.040±0.002[1] |
| Astrometry | |
| Radial velocity (Rv) | +2.7±0.8[5] km/s |
| Proper motion (μ) | RA: −28.922(74) mas/yr[2] Dec.: −50.085(101) mas/yr[2] |
| Parallax (π) | 9.5700±0.0876 mas[2] |
| Distance | 341 ± 3 ly (104.5 ± 1.0 pc) |
| Absolute magnitude (MV) | 0.32±0.12[6] |
| Details | |
| Mass | 2.65±0.06[6] M☉ |
| Radius | 2.89[7] R☉ |
| Luminosity | 74+9 −8[6] L☉ |
| Surface gravity (log g) | 3.94±0.14[8] cgs |
| Temperature | 10,795±367[8] K |
| Rotational velocity (v sin i) | 30[8] km/s |
| Age | 36[8] Myr |
| Other designations | |
| BD+79°265, FK5 2617, HD 64486, HIP 39538, HR 2527, SAO 6392, WDS J08048+7929AB[9] | |
| Database references | |
| SIMBAD | data |
HR 3082 is a double star in the northern circumpolar constellation of Camelopardalis. It is faintly visible to the naked eye with an apparent visual magnitude of 5.39.[1] The system is moving closer to the Sun with a heliocentric radial velocity of +2.7 km/s.[5] It is currently at a distance of around 341 light years, based upon an annual parallax shift of 9.57 mas.[2]
The brighter component is a magnetic,[7] mild Ap star that displays an overabundance of silicon in its spectrum.[10] Cowley et al. (1969) listed a stellar classification of A0p Si,[3] while Abt and Morrell (1995) have it pegged as a subgiant star with a class of B9.5 IVs.[4] It has an estimated 2.65[6] times the mass of the Sun and 2.89[7] times the Sun's radius. The star is radiating 74[6] times the Sun's luminosity from its photosphere at an effective temperature of 10,795 K.[8]
The fainter component is a magnitude 9.6 star at an angular separation of 0.4″ along a position angle (PA) of 84°, as of 2009.[11] This is most likely a visual companion located along the same line of sight.[12] There is a magnitude 13.6 visual companion at a separation of 6.4″ along a PA of 169°, as of 2016.[11]
References
[edit]- ^ a b c d 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. XHIP record for this object at VizieR.
- ^ a b c d e f 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.
- ^ a b 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 Abt, Helmut A.; Morrell, Nidia I. (July 1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
- ^ a b 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 c d e Kochukhov, O.; Bagnulo, S. (2006), "Evolutionary state of magnetic chemically peculiar stars", Astronomy and Astrophysics, 450 (2): 763, arXiv:astro-ph/0601461, Bibcode:2006A&A...450..763K, doi:10.1051/0004-6361:20054596, S2CID 18596834.
- ^ a b c Shulyak, D.; et al. (September 2014), "Interferometry of chemically peculiar stars: theoretical predictions versus modern observing facilities", Monthly Notices of the Royal Astronomical Society, 443 (2): 1629–1642, arXiv:1406.6093, Bibcode:2014MNRAS.443.1629S, doi:10.1093/mnras/stu1259.
- ^ a b c d e David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ "HD 49878". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-06-06.
- ^ Adelman, S. J. (September 1982), "Spectrophotometry of peculiar B and A stars. XII - HD 10783, 56 Tauri, HD 43819, 53 Aurigae, 49 Camelopardalis, HD 64486, HD 147550, HD 184905 and HD 192913", Astronomy and Astrophysics Supplement Series, 49: 663–672, Bibcode:1982A&AS...49..663A.
- ^ a b Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
