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Chi1 Orionis

January 27, 2023

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

Chi1 Orionis (χ1 Ori, χ1 Orionis) is a star about 28 light years away.[1] It is in the constellation Orion, where it can be seen in the tip of the hunter's upraised club.[13]

Chi1 Orionis A

Star map of the Bayers Stars in Orion. Chi1 Orionis is indicated.
Observation data
Epoch J2000      Equinox J2000
Constellation Orion
Right ascension 05h 54m 22.98s[1]
Declination +20° 16′ 34.2″[1]
Apparent magnitude (V) 4.38 - 4.41[2]
Characteristics
Spectral type G0 V[3]
U−B color index +0.07[4]
B−V color index +0.59[4]
Variable type RS CVn[2]
Astrometry
Radial velocity (Rv)−15.42[5] km/s
Proper motion (μ) RA: −162.54±0.28[1] mas/yr
Dec.: −99.51±0.16[1] mas/yr
Parallax (π)115.43 ± 0.27 mas[1]
Distance28.26 ± 0.07 ly
(8.66 ± 0.02 pc)
Absolute magnitude (MV)4.82±0.005[6]
Orbit[7]
Period (P)5156.291±2.508 d
Semi-major axis (a)89.662±0.880 Mas
Eccentricity (e)0.452±0.002
Inclination (i)95.937±0.790°
Longitude of the node (Ω)126.360±0.593°
Periastron epoch (T)2451468.2±3.083 JD
Argument of periastron (ω)
(secondary)		111.527±0.230°
Semi-amplitude (K1)
(primary)		1.876±0.003 km/s
Details
primary
Mass1.01[8] M☉
Radius0.979±0.009[9] R☉
Luminosity1.081±0.018[9] L☉
Surface gravity (log g)4.39[8] cgs
Temperature5,955±6.1[10] K
Metallicity [Fe/H]−0.01[11] dex
Rotation5.2 days[11]
Rotational velocity (v sin i)8.7[8] km/s
Age300–400[12] Myr
companion
Mass0.15[8] M☉
Age70-130[8] Myr
Other designations
54 Ori, Gl 222, HR 2047, BD+20°1162, HD 39587, LTT 11743, GCTP 1354.00, SAO 77705, HIP 27913
Database references
SIMBADdata
A light curve for Chi1 Orionis, plotted from TESS data.[14] The 5.5 day period derived by Stępień and Geyer is marked in red.

χ1 Ori is a G0V star.[8] It is listed in the General Catalog of Variable Stars as an RS Canum Venaticorum variable, varying between visual magnitude 4.38 and 4.41.[2] Stępień and Geyer measured its period to be 5.5 days.[15]

χ1 Ori has a faint companion with a mass estimated at about 15% of the mass of the Sun, and an orbital period of 14.1 years. 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. It is thought that the companion is a red dwarf still contracting towards the main sequence.[8]

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.[16]

χ1 Ori is a candidate stream star member of the Ursa Major Moving Group, although there is some evidence to the contrary.[11]

See also

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. Vizier catalog entry
  2. ^ a b c "khi 1 Ori". General Catalog of Variable Stars. Sternberg Astronomical Institute. Retrieved 29 December 2022.
  3. ^ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. ^ a b Hoffleit, Dorrit; Jaschek, Carlos (1991). "The Bright star catalogue". New Haven, Conn.: Yale University Observatory, 5th Rev.ed. Bibcode:1991bsc..book.....H.
  5. ^ Vallenari, A.; et al. (Gaia Collaboration) (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. arXiv:2208.00211. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
  6. ^ Park, Sunkyung; et al. (2013). "Wilson-Bappu Effect: Extended to Surface Gravity". The Astronomical Journal. 146 (4): 73. arXiv:1307.0592. Bibcode:2013AJ....146...73P. doi:10.1088/0004-6256/146/4/73. S2CID 119187733.
  7. ^ Han, Inwoo; Gatewood, George (2002). "A Precise Orbit Determination of χ1Orionis from Astrometric and Radial Velocity Data". Publications of the Astronomical Society of the Pacific. 114 (792): 224–228. Bibcode:2002PASP..114..224H. doi:10.1086/338367.
  8. ^ a b c d e f g König, B.; Fuhrmann, K.; Neuhäuser, R.; Charbonneau, D.; Jayawardhana, R. (2002). "Direct detection of the companion of chi 1 Orionis". Astronomy and Astrophysics. 394. arXiv:astro-ph/0209404. Bibcode:2002A&A...394L..43K. doi:10.1051/0004-6361:20021377. S2CID 10411048.
  9. ^ a b 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:1112.3316. Bibcode:2012ApJ...746..101B. doi:10.1088/0004-637X/746/1/101. S2CID 18993744.. See Table 10.
  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:astro-ph/0308429. Bibcode:2003A&A...411..559K. doi:10.1051/0004-6361:20031378. S2CID 18478960.
  11. ^ a b c 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:1007.1132. Bibcode:2010A&A...521A..12M. doi:10.1051/0004-6361/201014948. S2CID 119209183.
  12. ^ 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:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
  13. ^ Jim Kaler. "Chi-1 Orionis". Retrieved 2022-12-29.
  14. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 28 December 2022.
  15. ^ Stępień, K.; Geyer, E. (May 1996). "Rotation of solar-like main sequence stars". Astronomy and Astrophysics Supplement. 117: 83–91. Bibcode:1996A&AS..117...83S.
  16. ^ 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:1208.2051. Bibcode:2012MNRAS.427.2723J. doi:10.1111/j.1365-2966.2012.21839.x. S2CID 118570249.

External links

  • Chi-1 Orionis by Professor Jim Kaler.
  • Chi1 Orionis 2 at SolStation.

January 27, 2023
chi1, orionis, other, stars, with, this, bayer, designation, orionis, orionis, star, about, light, years, away, constellation, orion, where, seen, hunter, upraised, club, astar, bayers, stars, orion, indicated, observation, dataepoch, j2000, equinox, j2000cons. For other stars with this Bayer designation see x Orionis Chi1 Orionis x1 Ori x1 Orionis is a star about 28 light years away 1 It is in the constellation Orion where it can be seen in the tip of the hunter s upraised club 13 Chi1 Orionis AStar map of the Bayers Stars in Orion Chi1 Orionis is indicated Observation dataEpoch J2000 Equinox J2000Constellation OrionRight ascension 05h 54m 22 98s 1 Declination 20 16 34 2 1 Apparent magnitude V 4 38 4 41 2 CharacteristicsSpectral type G0 V 3 U B color index 0 07 4 B V color index 0 59 4 Variable type RS CVn 2 AstrometryRadial velocity Rv 15 42 5 km sProper motion m RA 162 54 0 28 1 mas yr Dec 99 51 0 16 1 mas yrParallax p 115 43 0 27 mas 1 Distance28 26 0 07 ly 8 66 0 02 pc Absolute magnitude MV 4 82 0 005 6 Orbit 7 Period P 5156 291 2 508 dSemi major axis a 89 662 0 880 MasEccentricity e 0 452 0 002Inclination i 95 937 0 790 Longitude of the node W 126 360 0 593 Periastron epoch T 2451 468 2 3 083 JDArgument of periastron w secondary 111 527 0 230 Semi amplitude K1 primary 1 876 0 003 km sDetailsprimaryMass1 01 8 M Radius0 979 0 009 9 R Luminosity1 081 0 018 9 L Surface gravity log g 4 39 8 cgsTemperature5 955 6 1 10 KMetallicity Fe H 0 01 11 dexRotation5 2 days 11 Rotational velocity v sin i 8 7 8 km sAge300 400 12 MyrcompanionMass0 15 8 M Age70 130 8 MyrOther designations54 Ori Gl 222 HR 2047 BD 20 1162 HD 39587 LTT 11743 GCTP 1354 00 SAO 77705 HIP 27913Database referencesSIMBADdata A light curve for Chi1 Orionis plotted from TESS data 14 The 5 5 day period derived by Stepien and Geyer is marked in red x1 Ori is a G0V star 8 It is listed in the General Catalog of Variable Stars as an RS Canum Venaticorum variable varying between visual magnitude 4 38 and 4 41 2 Stepien and Geyer measured its period to be 5 5 days 15 x1 Ori has a faint companion with a mass estimated at about 15 of the mass of the Sun and an orbital period of 14 1 years 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 It is thought that the companion is a red dwarf still contracting towards the main sequence 8 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 16 x1 Ori is a candidate stream star member of the Ursa Major Moving Group although there is some evidence to the contrary 11 See also EditList of star systems within 25 30 light yearsReferences Edit 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 amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 Vizier catalog entry a b c khi 1 Ori General Catalog of Variable Stars Sternberg Astronomical Institute Retrieved 29 December 2022 Keenan Philip C McNeil Raymond C 1989 The Perkins catalog of revised MK types for the cooler stars The Astrophysical Journal Supplement Series 71 245 Bibcode 1989ApJS 71 245K doi 10 1086 191373 a b Hoffleit Dorrit Jaschek Carlos 1991 The Bright star catalogue New Haven Conn Yale University Observatory 5th Rev ed Bibcode 1991bsc book H Vallenari A et al Gaia Collaboration 2022 Gaia Data Release 3 Summary of the content and survey properties Astronomy amp Astrophysics arXiv 2208 00211 doi 10 1051 0004 6361 202243940 Gaia DR3 record for this source at VizieR Park Sunkyung et al 2013 Wilson Bappu Effect Extended to Surface Gravity The Astronomical Journal 146 4 73 arXiv 1307 0592 Bibcode 2013AJ 146 73P doi 10 1088 0004 6256 146 4 73 S2CID 119187733 Han Inwoo Gatewood George 2002 A Precise Orbit Determination of x1Orionis from Astrometric and Radial Velocity Data Publications of the Astronomical Society of the Pacific 114 792 224 228 Bibcode 2002PASP 114 224H doi 10 1086 338367 a b c d e f g Konig B Fuhrmann K Neuhauser R Charbonneau D Jayawardhana R 2002 Direct detection of the companion of chi 1 Orionis Astronomy and Astrophysics 394 arXiv astro ph 0209404 Bibcode 2002A amp A 394L 43K doi 10 1051 0004 6361 20021377 S2CID 10411048 a b 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 1112 3316 Bibcode 2012ApJ 746 101B doi 10 1088 0004 637X 746 1 101 S2CID 18993744 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 astro ph 0308429 Bibcode 2003A amp A 411 559K doi 10 1051 0004 6361 20031378 S2CID 18478960 a b c 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 1007 1132 Bibcode 2010A amp A 521A 12M doi 10 1051 0004 6361 201014948 S2CID 119209183 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 0807 1686 Bibcode 2008ApJ 687 1264M doi 10 1086 591785 S2CID 27151456 Jim Kaler Chi 1 Orionis Retrieved 2022 12 29 MAST Barbara A Mikulski Archive for Space Telescopes Space Telescope Science Institute Retrieved 28 December 2022 Stepien K Geyer E May 1996 Rotation of solar like main sequence stars Astronomy and Astrophysics Supplement 117 83 91 Bibcode 1996A amp AS 117 83S 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 1208 2051 Bibcode 2012MNRAS 427 2723J doi 10 1111 j 1365 2966 2012 21839 x S2CID 118570249 External links EditChi 1 Orionis by Professor Jim Kaler Chi1 Orionis 2 at SolStation Retrieved from https en wikipedia org w index php title Chi1 Orionis amp oldid 1130306643, wikipedia, wiki, book, books, library,

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