Xi Orionis

Today, Xi Orionis is an issue that is present in all spheres of society. From politics to pop culture, Xi Orionis has become a constant talking point. This trend has led to an increase in attention and interest in Xi Orionis, both from experts and laypeople. In this article, we will explore the various aspects of Xi Orionis, from its historical origins to its impact on the world today. We will analyze how Xi Orionis has evolved over time and examine its influence in different areas. Additionally, we will discuss the future implications of Xi Orionis and how it can affect our lives in the future.

ξ Orionis
Location of ξ Orionis (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Orion
Right ascension 06h 11m 56.39693s[1]
Declination +14° 12′ 31.5555″[1]
Apparent magnitude (V) 4.47[2]
Characteristics
Spectral type B3 IV[3]
U−B color index −0.65[2]
B−V color index −0.19[2]
Astrometry
Radial velocity (Rv)+19.30[4] km/s
Proper motion (μ) RA: +0.29[1] mas/yr
Dec.: −20.12[1] mas/yr
Parallax (π)5.37±0.23 mas[1]
Distance610 ± 30 ly
(186 ± 8 pc)
Orbit[5]
Period (P)45.1 d
Eccentricity (e)0.26
Periastron epoch (T)2,441,962.3 JD
Argument of periastron (ω)
(secondary)		205°
Semi-amplitude (K1)
(primary)		22.4 km/s
Details
ξ Ori A
Mass6.7±0.1[3] M☉
Luminosity1,390[6] L☉
Temperature15,476[6] K
Rotational velocity (v sin i)160[7] km/s
Age32.1±4.3[3] Myr
Other designations
ξ Ori, 70 Orionis, BD+14° 1187, HD 42560, HIP 29426, HR 2199, SAO 95362[8]
Database references
SIMBADdata

Xi Orionis (ξ Orionis) is a binary star system in the northeastern part of the constellation of Orion, well above the red giant star Betelgeuse in the sky. It lies next to another blue main-sequence star, Nu Orionis, which is somewhat closer at 520 light-years' distance. The apparent visual magnitude of Xi Orionis is 4.47,[2] which is bright enough to be seen with the naked eye. The distance to this star, as determined using the parallax method, is roughly 610 light-years.[1]

This is a spectroscopic binary star system with an orbital period of 45.1 days and an eccentricity of 0.26.[5] The primary component is a B-type subgiant star with a stellar classification of B3 IV.[3] With an estimated age of just 32 million years,[3] it has a relatively high rate of spin, showing a projected rotational velocity of 160 km/s.[7] Xi Orionis has about 6.7 times the mass of the Sun,[3] and shines with 1,390 times the solar luminosity from its outer atmosphere at an effective temperature of 15,476 K.[6]

References

  1. ^ a b c d e f 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 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.
  3. ^ a b c d e f Tetzlaff, N.; et al. (January 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.
  4. ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ a b Pourbaix, D.; et al. (2004), "SB9: 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.
  6. ^ a b c McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  7. ^ a b Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590.
  8. ^ "ksi Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-11-08.