Astronomy:Nu Orionis
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Orion |
| Right ascension | 06h 07m 34.32588s[1] |
| Declination | +14° 46′ 06.5061″[1] |
| Apparent magnitude (V) | 4.42[2] |
| Characteristics | |
| Spectral type | B3 V[3] or B3 IV[4] |
| U−B color index | −0.67[2] |
| B−V color index | −0.18[2] |
| Astrometry | |
| Radial velocity (Rv) | +24.1[5] km/s |
| Proper motion (μ) | RA: +6.78[1] mas/yr Dec.: −20.23[1] mas/yr |
| Parallax (π) | 6.32 ± 0.33[1] mas |
| Distance | 520 ± 30 ly (158 ± 8 pc) |
| Orbit[6] | |
| 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[4] M☉ |
| Radius | 4.3[7] R☉ |
| Luminosity | 1,965[3] L☉ |
| Surface gravity (log g) | 4.06[8] cgs |
| Temperature | 17,880[8] K |
| Metallicity [Fe/H] | −0.05[8] dex |
| Rotational velocity (v sin i) | 30[9] km/s |
| Age | 26.3±5.3[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nu Orionis (ν Orionis) is a binary star[11] system in the northeastern part of the constellation Orion. It should not be confused with the variable star NU Orionis.[12] Nu Orionis has an apparent visual magnitude of 4.42,[2] which is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 0.00632 arcseconds,[1] the distance to this system is roughly 520 light years.
This is a single-lined spectroscopic binary system,[9] 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.[6] Depending on the source, the primary is either a B-type main sequence star with a stellar classification of B3 V,[3] or a more evolved B-type subgiant star of class B3 IV.[4] It has an angular diameter of 0.251 mas,[13] which, at the estimated distance of this system, yields a physical size of about 4.3 times the radius of the Sun.[7] The mass is 6.7[4] times that of the Sun and it shines with 1,965[3] times the solar luminosity from its outer atmosphere at an effective temperature of 17,880 K.[8]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 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, doi:10.1086/111220, Bibcode: 1971AJ.....76.1058C.
- ↑ 3.0 3.1 3.2 3.3 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, doi:10.1002/asna.200911355, Bibcode: 2010AN....331..349H.
- ↑ 4.0 4.1 4.2 4.3 4.4 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, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T.
- ↑ Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick, Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30, 30, University of Toronto: International Astronomical Union, p. 57, Bibcode: 1967IAUS...30...57E.
- ↑ 6.0 6.1 Pourbaix, D. et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics 424 (2): 727–732, doi:10.1051/0004-6361:20041213, Bibcode: 2004A&A...424..727P.
- ↑ 7.0 7.1 Lang, Kenneth R. (2006), Astrophysical formulae, Astronomy and astrophysics library, 1 (3rd ed.), Birkhäuser, ISBN 3-540-29692-1, https://books.google.com/books?id=OvTjLcQ4MCQC&pg=PA41.. The radius (R*) is given by:
- [math]\displaystyle{ \begin{align} 2\cdot R_* & = \frac{(158.2\cdot 0.251\cdot 10^{-3})\ \text{AU}}{0.0046491\ \text{AU}/R_{\bigodot}} \\ & \approx 8.5\cdot R_{\bigodot} \end{align} }[/math]
- ↑ 8.0 8.1 8.2 8.3 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, doi:10.1086/171116, Bibcode: 1992ApJ...387..673G.
- ↑ 9.0 9.1 Abt, Helmut A. et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A.
- ↑ "nu. Ori". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=nu.+Ori.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 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, https://books.google.com/books?id=0KRSphlvsqgC&pg=PA93.
- ↑ 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, doi:10.1051/0004-6361/200811147, Bibcode: 2009A&A...501..297Z.
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