Nu3 Canis Majoris
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 06h 37m 53.42144s[1] |
| Declination | −18° 14′ 14.9218″[1] |
| Apparent magnitude (V) | 4.41[2] (4.63 + 8.56)[3] |
| Characteristics | |
| Spectral type | K0 II-III[4] |
| U−B color index | +1.04[2] |
| B−V color index | +1.16[2] |
| Astrometry | |
| Radial velocity (Rv) | −1.50±0.70[5] km/s |
| Proper motion (μ) | RA: −7.32[1] mas/yr Dec.: −8.72[1] mas/yr |
| Parallax (π) | 7.74 ± 0.43[1] mas |
| Distance | 420 ± 20 ly (129 ± 7 pc) |
| Absolute magnitude (MV) | −1.13[6] |
| Details[4] | |
| ν3 CMa A | |
| Mass | 3.38±0.37[7] M☉ |
| Radius | 32.7 R☉ |
| Luminosity | 398 L☉ |
| Surface gravity (log g) | 2.34 cgs |
| Temperature | 4,510 K |
| Metallicity [Fe/H] | −0.24 dex |
| Rotation | 183 d |
| Rotational velocity (v sin i) | 8[8] km/s |
| Age | 380±20[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nu3 Canis Majoris, Latinized from ν3 Canis Majoris, is a binary star[3] system in the southern constellation of Canis Major. It is visible to the naked eye with a combined apparent visual magnitude of 4.41.[2] Based upon an annual parallax shift of 7.74 mas as seen from Earth,[1] this system is located about 420 light years from the Sun.
The primary member, component A, is an evolved, orange-hued giant/bright giant hybrid with an apparent magnitude of +4.63[3] and a stellar classification of K0 II-III.[4] It is most likely (96% chance) on the horizontal branch.[7] The star has a moderate level of surface activity with a magnetic field strength of 2.2±0.4 G and is a source of X-ray emission with a luminosity of 624×1027 erg s−1.[4]
This giant has an estimated 3.4[7] times the mass of the Sun and has expanded to 33[4] times the Sun's radius. It is radiating 398 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,510 K.[4] The star is spinning with the leisurely period of 183 days.[4] Its companion, component B, is 1.040 arcseconds distant and has an apparent magnitude of +8.56.[3]
References
- 1 2 3 4 5 6 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.
- 1 2 3 4 Fernie, J. D. (May 1983), "New UBVRI photometry for 900 supergiants", Astrophysical Journal Supplement Series, 52: 7–22, Bibcode:1983ApJS...52....7F, doi:10.1086/190856.
- 1 2 3 4 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.
- 1 2 3 4 5 6 7 Aurière, M.; et al. (2015), "The magnetic fields at the surface of active single G-K giants", Astronomy & Astrophysics, 574, arXiv:1411.6230, Bibcode:2015A&A...574A..90A, doi:10.1051/0004-6361/201424579, A90.
- ↑ 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, A61.
- ↑ 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.
- 1 2 3 4 Reffert, Sabine; et al. (2015), "Precise radial velocities of giant stars. VII. Occurrence rate of giant extrasolar planets as a function of mass and metallicity", Astronomy & Astrophysics, 574: A116, arXiv:1412.4634, Bibcode:2015A&A...574A.116R, doi:10.1051/0004-6361/201322360.
- ↑ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1), Bibcode:1970CoAsi.239....1B.
- ↑ "nu03 CMa". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-05.