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Psi2 Orionis

October 15, 2023

For other stars with this Bayer designation, see Psi Orionis.

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

ψ2 Orionis

A light curve for Psi2 Orionis plotted from TESS data[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Orion
Right ascension 05h 26m 50.22932s[2]
Declination +03° 05′ 44.4222″[2]
Apparent magnitude (V) 4.55 (- 4.58) - 4.61[3]
Characteristics
Spectral type B2 IV[4] (B1 III + B2 V)[5]
U−B color index −0.94[6]
B−V color index −0.22[6]
Variable type Eclipsing[3]
Astrometry
Radial velocity (Rv)+19[7] km/s
Proper motion (μ) RA: +1.448[2] mas/yr
Dec.: −1.019[2] mas/yr
Parallax (π)2.9943 ± 0.1533 mas[2]
Distance1,090 ± 60 ly
(330 ± 20 pc)
Absolute magnitude (MV)−2.71[8]
Orbit[7]
Period (P)2.529 d
Eccentricity (e)0.053
Inclination (i)58±8°
Periastron epoch (T)2450774 JD
Argument of periastron (ω)
(secondary)		172°
Semi-amplitude (K1)
(primary)		145 km/s
Semi-amplitude (K2)
(secondary)		237 km/s
Details
primary
Mass9.6[9] M☉
Luminosity10,252[4] L☉
Surface gravity (log g)3.5[10] cgs
Temperature25,000[10] K
Rotational velocity (v sin i)95±5[10] km/s
Age11.4[7] Myr
secondary
Mass7.06[9] M☉
Surface gravity (log g)3.5[10] cgs
Temperature22,500[10] K
Rotational velocity (v sin i)75±5[10] km/s
Other designations
ψ2 Ori, 30 Orionis, BD+02°962, HD 35715, HIP 25473, HR 1811, SAO 112775.[11]
Database references
SIMBADdata

This is a double-lined spectroscopic binary,[5] which means that the individual absorption lines of both components can be discerned. The pair orbit each other with a period of 2.526 days and a low eccentricity of 0.04.[10] The close orbit is causing their mutual gravitational interaction to distort the shapes of the stars, turning this system into an ellipsoidal variable.[12] The inclination of orbital plane is sufficiently low that the two stars form a grazing eclipsing binary. During the eclipse of the primary component, the visual magnitude is reduced by 0.06, whereas the secondary eclipse reduces the magnitude by 0.03.[13] The brightness variability has led to the star being classified as a pulsating Beta Cephei variable, but no evidence has been found of pulsations superimposed on the variability due to ellipsoidal rotations and eclipses.[14][7]

The combined spectrum of Psi2 Orionis matches that of a B-type subgiant star with a stellar classification of B2 IV.[4] The primary component is an evolved giant star with a class of B1 III, while the secondary is a B-type main sequence star with a classification of B2 V.[5]

References Edit

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  3. ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
  4. ^ a b c Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  5. ^ a b c 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.
  6. ^ a b 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.
  7. ^ a b c d Telting, J. H.; Abbott, J. B.; Schrijvers, C. (2001). "Apsidal motion and non-radial pulsations in <ASTROBJ>psi 2 Ori</ASTROBJ>". Astronomy and Astrophysics. 377: 104. Bibcode:2001A&A...377..104T. doi:10.1051/0004-6361:20011026-1.
  8. ^ Melnik, A. M.; Dambis, A. K. (2020), "Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions", Astrophysics and Space Science, 365 (7): 112, arXiv:2006.14649, Bibcode:2020Ap&SS.365..112M, doi:10.1007/s10509-020-03827-0, S2CID 220128144.
  9. ^ a b Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series. 124: 75. Bibcode:1997A&AS..124...75T. doi:10.1051/aas:1997181.
  10. ^ a b c d e f g Lu, W. (1985), "The double-lined spectroscopic binary psi Orionis", Publications of the Astronomical Society of the Pacific, 97: 428, Bibcode:1985PASP...97..428L, doi:10.1086/131556, S2CID 121466372.
  11. ^ "psi02 Ori", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-12-01.
  12. ^ Beech, Martin (February 1989), "The ellipsoidal variables. IV - Light variations", Astrophysics and Space Science, 152 (2): 329–335, Bibcode:1989Ap&SS.152..329B, doi:10.1007/BF00636314, S2CID 119488926.
  13. ^ Lefèvre, L.; et al. (2009), "A systematic study of variability among OB-stars based on HIPPARCOS photometry", Astronomy and Astrophysics, 507 (2): 1141–1201, Bibcode:2009A&A...507.1141L, doi:10.1051/0004-6361/200912304, ISSN 0004-6361.
  14. ^ Waelkens, C.; Rufener, F. (May 1983), "An observational study of the influence of close companions on the pulsations of beta Cephei stars", Astronomy and Astrophysics, 121: 45–50, Bibcode:1983A&A...121...45W.

October 15, 2023
psi2, orionis, other, stars, with, this, bayer, designation, orionis, binary, star, system, equatorial, constellation, orion, apparent, visual, magnitude, indicating, that, visible, naked, based, upon, annual, parallax, shift, mass, roughly, light, years, dist. For other stars with this Bayer designation see Psi Orionis Psi2 Orionis a binary star system in the equatorial constellation of Orion It has an apparent visual magnitude of 4 6 indicating that it is visible to the naked eye Based upon an annual parallax shift of 2 87 mass it is roughly 1 100 light years distant from the Sun ps2 OrionisA light curve for Psi2 Orionis plotted from TESS data 1 Observation dataEpoch J2000 0 Equinox J2000 0 ICRS Constellation OrionRight ascension 05h 26m 50 22932s 2 Declination 03 05 44 4222 2 Apparent magnitude V 4 55 4 58 4 61 3 CharacteristicsSpectral type B2 IV 4 B1 III B2 V 5 U B color index 0 94 6 B V color index 0 22 6 Variable type Eclipsing 3 AstrometryRadial velocity Rv 19 7 km sProper motion m RA 1 448 2 mas yr Dec 1 019 2 mas yrParallax p 2 9943 0 1533 mas 2 Distance1 090 60 ly 330 20 pc Absolute magnitude MV 2 71 8 Orbit 7 Period P 2 529 dEccentricity e 0 053Inclination i 58 8 Periastron epoch T 2450774 JDArgument of periastron w secondary 172 Semi amplitude K1 primary 145 km sSemi amplitude K2 secondary 237 km sDetailsprimaryMass9 6 9 M Luminosity10 252 4 L Surface gravity log g 3 5 10 cgsTemperature25 000 10 KRotational velocity v sin i 95 5 10 km sAge11 4 7 MyrsecondaryMass7 06 9 M Surface gravity log g 3 5 10 cgsTemperature22 500 10 KRotational velocity v sin i 75 5 10 km sOther designationsps2 Ori 30 Orionis BD 02 962 HD 35715 HIP 25473 HR 1811 SAO 112775 11 Database referencesSIMBADdataThis is a double lined spectroscopic binary 5 which means that the individual absorption lines of both components can be discerned The pair orbit each other with a period of 2 526 days and a low eccentricity of 0 04 10 The close orbit is causing their mutual gravitational interaction to distort the shapes of the stars turning this system into an ellipsoidal variable 12 The inclination of orbital plane is sufficiently low that the two stars form a grazing eclipsing binary During the eclipse of the primary component the visual magnitude is reduced by 0 06 whereas the secondary eclipse reduces the magnitude by 0 03 13 The brightness variability has led to the star being classified as a pulsating Beta Cephei variable but no evidence has been found of pulsations superimposed on the variability due to ellipsoidal rotations and eclipses 14 7 The combined spectrum of Psi2 Orionis matches that of a B type subgiant star with a stellar classification of B2 IV 4 The primary component is an evolved giant star with a class of B1 III while the secondary is a B type main sequence star with a classification of B2 V 5 References Edit MAST Barbara A Mikulski Archive for Space Telescopes Space Telescope Science Institute Retrieved 8 December 2021 a b c d e Brown A G A et al Gaia collaboration 2021 Gaia Early Data Release 3 Summary of the contents and survey properties Astronomy amp Astrophysics 649 A1 arXiv 2012 01533 Bibcode 2021A amp A 649A 1G doi 10 1051 0004 6361 202039657 S2CID 227254300 Erratum doi 10 1051 0004 6361 202039657e Gaia EDR3 record for this source at VizieR a b Samus N N Durlevich O V et al 2009 VizieR Online Data Catalog General Catalogue of Variable Stars Samus 2007 2013 VizieR On line Data Catalog B GCVS Originally Published in 2009yCat 102025S 1 B gcvs Bibcode 2009yCat 102025S a b c Hohle M M et al April 2010 Masses and luminosities of O and B type stars and red supergiants Astronomische Nachrichten 331 4 349 arXiv 1003 2335 Bibcode 2010AN 331 349H doi 10 1002 asna 200911355 S2CID 111387483 a b c 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 a b 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 a b c d Telting J H Abbott J B Schrijvers C 2001 Apsidal motion and non radial pulsations in lt ASTROBJ gt psi 2 Ori lt ASTROBJ gt Astronomy and Astrophysics 377 104 Bibcode 2001A amp A 377 104T doi 10 1051 0004 6361 20011026 1 Melnik A M Dambis A K 2020 Distance scale for high luminosity stars in OB associations and in field with Gaia DR2 Spurious systematic motions Astrophysics and Space Science 365 7 112 arXiv 2006 14649 Bibcode 2020Ap amp SS 365 112M doi 10 1007 s10509 020 03827 0 S2CID 220128144 a b Tokovinin A A 1997 MSC a catalogue of physical multiple stars Astronomy and Astrophysics Supplement Series 124 75 Bibcode 1997A amp AS 124 75T doi 10 1051 aas 1997181 a b c d e f g Lu W 1985 The double lined spectroscopic binary psi Orionis Publications of the Astronomical Society of the Pacific 97 428 Bibcode 1985PASP 97 428L doi 10 1086 131556 S2CID 121466372 psi02 Ori SIMBAD Centre de donnees astronomiques de Strasbourg retrieved 2016 12 01 Beech Martin February 1989 The ellipsoidal variables IV Light variations Astrophysics and Space Science 152 2 329 335 Bibcode 1989Ap amp SS 152 329B doi 10 1007 BF00636314 S2CID 119488926 Lefevre L et al 2009 A systematic study of variability among OB stars based on HIPPARCOS photometry Astronomy and Astrophysics 507 2 1141 1201 Bibcode 2009A amp A 507 1141L doi 10 1051 0004 6361 200912304 ISSN 0004 6361 Waelkens C Rufener F May 1983 An observational study of the influence of close companions on the pulsations of beta Cephei stars Astronomy and Astrophysics 121 45 50 Bibcode 1983A amp A 121 45W Retrieved from https en wikipedia org w index php title Psi2 Orionis amp oldid 1170215823, wikipedia, wiki, book, books, library,

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