Observation dataEpoch J2000.0      Equinox J2000.0 Constellation Location of ρ Orionis (circled) Orion 05h 13m 17.48015s[1] +02° 51′ 40.5479″[1] +4.44[2] K0 III[3] +1.13[2] +1.19[2] Radial velocity (Rv) +40.5[4] km/s Proper motion (μ) RA: +0.83[1] mas/yr Dec.: +3.91[1] mas/yr Parallax (π) 9.32 ± 0.94 mas[1] Distance approx. 350 ly (approx. 110 pc) Absolute magnitude (MV) −0.65[5] Mass 2.67 M☉ Radius 25[7] R☉ Luminosity 251 L☉ Surface gravity (log g) 2.4[8] cgs Temperature 4,533 K Metallicity [Fe/H] 0.06[8] dex Age 650 Myr Period (P) 1031.4 days Semi-major axis (a) 6.9 mas[note 1] Eccentricity (e) 0.1 Inclination (i) 122.8° Longitude of the node (Ω) 242.6° Periastron epoch (T) 2426182.46 Argument of periastron (ω)(secondary) 17.9° Semi-amplitude (K1)(primary) 8.70 km/s ρ Ori, 17 Orionis, BD+02° 888, HD 33856, HIP 24331, HR 1698, SAO 112528 SIMBAD data

Rho Orionis, Latinised from ρ Orionis, is the Bayer designation for an orange-hued binary star system in the equatorial constellation of Orion. It is visible to the naked eye with an apparent visual magnitude of +4.44.[2] The star shows an annual parallax shift of 9.32 mas due to the orbital motion of the Earth, which provides a distance estimate of roughly 350 light-years from the Sun. It is moving away from the Sun with a radial velocity of +40.5 km/s.[4] About 2.6 million years ago, Rho Orionis made its perihelion passage at a distance of around 10 light-years (3.1 parsecs).[10]

This is a single-lined spectroscopic binary system with an orbital period of 2.8 years and an eccentricity of 0.1.[9] The visible component is an evolved giant star of type K with a stellar classification of K0 III.[3] Its measured angular diameter is 2.19±0.02 mas,[11] which, at its estimated distance yields a physical size of about 25 times the radius of the Sun.[7] It has 2.67 times the mass of the Sun and is about 650 million years old. The star is radiating 251 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,533 K.[6]

Notes

1. ^ This is the photocentric semi-major axis, from the motion shown by the observed "star" relative to distant objects, and in practice relative to the barycentre. This is always smaller than the orbital semi-major axis, dramatically smaller when the primary star is much more massive than the secondary or when it is not much brighter.

References

1. 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.
2. ^ a b c d Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
3. ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars, Vol. 5". Michigan Spectral Survey. 05: 0. Bibcode:1999MSS...C05....0H.
4. ^ a b Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
5. ^ Smith, Graeme H.; Shetrone, Matthew D. (2000). "CaII K Emission-Line Asymmetry among Red Giants Detected by the ROSAT Satellite". The Publications of the Astronomical Society of the Pacific. 112 (776): 1320. Bibcode:2000PASP..112.1320S. doi:10.1086/316634.
6. ^ a b Luck, R. Earle (2015). "Abundances in the Local Region. I. G and K Giants". The Astronomical Journal. 150 (3): 88. arXiv:1507.01466. Bibcode:2015AJ....150...88L. doi:10.1088/0004-6256/150/3/88. S2CID 118505114.
7. ^ a b 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:
{\displaystyle {\begin{aligned}2\cdot R_{*}&={\frac {(107\cdot 2.19\cdot 10^{-3})\ {\text{AU))}{0.0046491\ {\text{AU))/R_{\bigodot ))}\\&\approx 50.4\cdot R_{\bigodot }\end{aligned))}
8. ^ a b Soubiran, C.; Le Campion, J.-F.; Cayrel de Strobel, G.; Caillo, A. (June 2010), "The PASTEL catalogue of stellar parameters", Astronomy and Astrophysics, 515: A111, arXiv:1004.1069, Bibcode:2010A&A...515A.111S, doi:10.1051/0004-6361/201014247, S2CID 118362423.
9. ^ a b Ren, S. (2013), "Hipparcos Photocentric Orbits of 72 Single-lined Spectroscopic Binaries", The Astronomical Journal, 145 (3): 81, Bibcode:2013AJ....145...81R, doi:10.1088/0004-6256/145/3/81
10. ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
11. ^ Richichi, A.; Percheron, I.; Khristoforova, M. (February 2005), "CHARM2: An updated Catalog of High Angular Resolution Measurements", Astronomy and Astrophysics, 431 (2): 773–777, Bibcode:2005A&A...431..773R, doi:10.1051/0004-6361:20042039