Location of ν Orionis (circled) | |
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
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Constellation | Orion |
Right ascension | 06 07 34.32588 |
Declination | +14° 46′ 06.5061″ |
Apparent magnitude (V) | 4.42 |
Characteristics | |
Spectral type | B3 V or B3 IV |
U−B color index | −0.67 |
B−V color index | −0.18 |
Astrometry | |
Radial velocity (Rv) | +24.1 km/s |
Proper motion (μ) | RA: +6.78 mas/yr Dec.: −20.23 mas/yr |
Parallax (π) | 6.32 ± 0.33 mas |
Distance | 520 ± 30 ly (158 ± 8 pc) |
Orbit | |
Period (P) | 131.211 d |
Eccentricity (e) | 0.64 |
Periastron epoch (T) | 2436475.852 JD |
Argument of periastron (ω) (secondary) | 6.6° |
Semi-amplitude (K1) (primary) | 33.3 km/s |
Details | |
ν Ori A | |
Mass | 6.7±0.1 M☉ |
Radius | 4.3 R☉ |
Luminosity | 1,965 L☉ |
Surface gravity (log g) | 4.06 cgs |
Temperature | 17,880 K |
Metallicity | −0.05 dex |
Rotational velocity (v sin i) | 30 km/s |
Age | 26.3±5.3 Myr |
Other designations | |
ν Ori, 67 Orionis, BD+14° 1152, FK5 232, HD 41753, HIP 29038, HR 2159, SAO 95259. | |
Database references | |
SIMBAD | data |
Nu Orionis (ν Orionis) is a binary star system in the northeastern part of the constellation Orion. It should not be confused with the variable star NU Orionis. Nu Orionis has an apparent visual magnitude of 4.42, which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 0.00632 arcseconds, the distance to this system is roughly 520 light years.
This is a single-lined spectroscopic binary system, which means that only the absorption line features of one of the components can be distinguished. The components orbit each other with a period of 131.2 days and an eccentricity of 0.64. Depending on the source, the primary is either a B-type main sequence star with a stellar classification of B3 V, or a more evolved B-type subgiant star of class B3 IV. It has an angular diameter of 0.251 mas, which, at the estimated distance of this system, yields a physical size of about 4.3 times the radius of the Sun. The mass is 6.7 times that of the Sun and it shines with 1,965 times the solar luminosity from its outer atmosphere at an effective temperature of 17,880 K.
References
- ^ 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.
- ^ Crawford, D. L.; et al. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220.
- ^ Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349–360, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
- ^ Tetzlaff, N.; et al. (2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
- Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.), Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, vol. 30, University of Toronto: International Astronomical Union, p. 57, Bibcode:1967IAUS...30...57E.
- ^ Pourbaix, D.; et al. (2004), "SB: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424 (2): 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
- ^ Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1.. The radius (R*) is given by:
- ^ Gies, Douglas R.; Lambert, David L. (March 1992), "Carbon, nitrogen, and oxygen abundances in early B-type stars", Astrophysical Journal, Part 1, 387: 673–700, Bibcode:1992ApJ...387..673G, doi:10.1086/171116.
- ^ 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.
- "nu. Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-11-03.
- 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.
- Marett-Crosby, Michael (2013), Twenty-Five Astronomical Observations That Changed the World: And How To Make Them Yourself, The Patrick Moore Practical Astronomy Series, Springer Science & Business Media, p. 93, ISBN 978-1461468004.
- Zorec, J.; et al. (July 2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff", Astronomy and Astrophysics, 501 (1): 297–320, arXiv:0903.5134, Bibcode:2009A&A...501..297Z, doi:10.1051/0004-6361/200811147, S2CID 14969137.
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