Star map of the Bayers Stars in Orion. Chi1 Orionis is indicated.
Epoch J2000 Equinox J2000
|Right ascension||05h 54m 22.98s|
|Declination||+20° 16′ 34.2″|
|Apparent magnitude (V)||4.39|
|Spectral type||G0 V|
|U−B color index||0.07|
|B−V color index||0.59|
|Radial velocity (Rv)||−13.4 km/s|
|Proper motion (μ)||RA: −162.54 ± 0.28 mas/yr
Dec.: −99.51 ± 0.16 mas/yr
|Parallax (π)||115.43 ± 0.27 mas|
|Distance||28.26 ± 0.07 ly
(8.66 ± 0.02 pc)
|Absolute magnitude (MV)||4.67|
|Radius||0.979 ± 0.009 R☉|
|Luminosity||1.081 ± 0.018 L☉|
|Temperature||5,955 ± 6.1 K|
|Metallicity [Fe/H]||−0.01 dex|
χ1 Ori is a G0V star. It has a faint companion with a mass estimated at about 15% of the mass of the Sun, an orbital period of 14.1 years, and an estimated stellar class of M6. The companion orbits an average distance of 6.1 AU from the primary, but has a fairly high orbital eccentricity, ranging from 3.3 AU out to 8.9 AU from the primary. Because of this red dwarf companion, the likelihood of habitable planets in this system is low.
A necessary condition for the existence of a planet in this system are stable zones where the object can remain in orbit for long intervals. For hypothetical planets in a circular orbit around the individual members of this star system, this maximum orbital radius is computed to be 1.01 AU for the primary and 0.41 AU for the secondary. (Note that the orbit of the Earth is 1 AU from the Sun.) A planet orbiting outside of both stars would need to be at least 18.4 AU distant.
- van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- Boyajian, Tabetha S.; et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal, 746 (1): 101, arXiv:, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101. See Table 10.
- Kovtyukh; et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics, 411 (3): 559–564, arXiv:, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378
- Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948
- Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785
- Jim Kaler, Chi-1 Orionis.
- König, B.; Fuhrmann, K.; Neuhäuser, R.; Charbonneau, D.;Jayawardhana, R., Direct detection of the companion of chi1 Orionis Astronomy and Astrophysics, vol. 394, L43, 2002.
- Jaime, Luisa G.; et al. (December 2012), "Regions of dynamical stability for discs and planets in binary stars of the solar neighbourhood", Monthly Notices of the Royal Astronomical Society, 427 (4): 2723–2733, arXiv:, Bibcode:2012MNRAS.427.2723J, doi:10.1111/j.1365-2966.2012.21839.x.
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