Gamma Canis Majoris
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 07h 03m 45.49305s[1] |
| Declination | −15° 37′ 59.8300″[1] |
| Apparent magnitude (V) | +4.10[2] |
| Characteristics | |
| Spectral type | B8II[3] |
| U−B color index | −0.45[2] |
| B−V color index | −0.13[2] |
| Astrometry | |
| Radial velocity (Rv) | +32.0[4] km/s |
| Proper motion (μ) | RA: −0.14[1] mas/yr Dec.: –11.36[1] mas/yr |
| Parallax (π) | 7.38 ± 0.21 mas[1] |
| Distance | 440 ± 10 ly (136 ± 4 pc) |
| Details | |
| Radius | 5.6[5] R☉ |
| Surface gravity (log g) | 3.5[5] cgs |
| Temperature | 13,596[5] K |
| Metallicity [Fe/H] | −0.24[6] dex |
| Rotation | 6.16 d[7] |
| Rotational velocity (v sin i) | 30[8] km/s |
| Other designations | |
Gamma Canis Majoris (γ CMa, γ Canis Majoris) is a star in the constellation Canis Major. It has the traditional name Muliphein,[10] not to be confused with Muhlifain, which is Gamma Centauri; both names derive from the same Arabic root, محلفين muħlifayn. It is unclear exactly why this relatively faint star was given the "gamma" designation, but it is possibly because it is in the same part of the constellation as Sirius (alpha) and Murzim (beta).
γ Canis Majoris is a blue-white B-type bright giant with a stellar classification of B8II[3] and an apparent magnitude of +4.11. It is approximately 440 light years from Earth. It is a chemically peculiar Hg-Mg star displaying abnormal lines of mercury and magnesium.[7] This star has 5.6 times the radius of the Sun and the outer atmosphere has an effective temperature of 13,596 K.[5]
This star is suspected of being a spectroscopic binary system, and there is a candidate companion at an angular separation of 0.332″ along a position angle of 114.8°.[7] It is a member of the Collander 121 open cluster.[11]
Modern legacy
Muliphein appears on the flag of Brazil, symbolizing the state of Rondônia.[12]
References
- ^ a b c d e 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.
- ^ a b c 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.
- ^ a b Buscombe, W. (1962), "Spectral classification of Southern fundamental stars", Mount Stromlo Observatory Mimeogram, 4, Bibcode:1962MtSOM...4....1B.
- ^ Kharchenko, N. V.; et al. (2007), "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ∼55000 stars and mean radial velocities of 516 Galactic open clusters and associations", Astronomische Nachrichten, 328 (9): 889, doi:10.1002/asna.200710776.
- ^ a b c d Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189: 601–605, Bibcode:1979MNRAS.189..601U, doi:10.1093/mnras/189.3.601.
{{citation}}: CS1 maint: unflagged free DOI (link) - ^ Searle, Leonard; et al. (July 1966), "Studies of the Peculiar a Stars.IV. The Relative Abundances of Four Iron-Peak Elements", Astrophysical Journal, 145: 141, Bibcode:1966ApJ...145..141S, doi:10.1086/148750.
- ^ a b c Hubrig, S.; et al. (November 2012), "Magnetic fields of HgMn stars*", Astronomy & Astrophysics, 547: 24, arXiv:1208.2910, Bibcode:2012A&A...547A..90H, doi:10.1051/0004-6361/201219778, A90.
- ^ Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590.
- ^ "gam CMa -- Star in Cluster", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-03-07.
- ^ Star Name - R.H.Allen p.130
- ^ Maza, N. L.; et al. (October 2010), "Atomic species in the spectrum of the Hg-Mn star HD 53244", Revista Mexicana de Astronomía y Astrofísica, 46: 339−348, Bibcode:2010RMxAA..46..339M.
- ^ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website.
