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Xi Boötis

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Xi Boötis A/B
Diagram showing star positions and boundaries of the Boötes constellation and its surroundings
Diagram showing star positions and boundaries of the Boötes constellation and its surroundings

Location of ξ Boötis (circled)
Observation data
EpochJ2000EquinoxJ2000
Constellation Boötes
Right ascension 14h51m23.37993s[1]
Declination +19° 06′ 01.6994″[1]
Apparent magnitude(V) 4.70/6.97
Characteristics
Spectral type G8 Ve + K4 Ve
U−Bcolor index 0.24/1.15
B−Vcolor index 0.73/1.15
R−Icolor index 0.43 / 0.28
Variable type BY Draconis/None
flare star
Astrometry
ξ Boo A
Radial velocity(Rv)+3.0[2]km/s
Proper motion(μ)RA:127.468±0.126[3]mas/yr
Dec.:−40.569±0.129[3]mas/yr
Parallax(π)148.0695 ± 0.1317mas[3]
Distance22.03 ± 0.02ly
(6.754 ± 0.006pc)
Absolute magnitude(MV)5.54±0.007[4]
ξ Boo B
Proper motion(μ)RA:133.376±0.041[5]mas/yr
Dec.:−182.059±0.045[5]mas/yr
Parallax(π)148.1793 ± 0.0546mas[5]
Distance22.011 ± 0.008ly
(6.749 ± 0.002pc)
Orbit[6]
CompanionXi Boötis B
Period(P)151.505±0.170yr
Semi-major axis(a)4.9044±0.0027″
Eccentricity(e)0.5117±0.0006
Inclination(i)140.037±0.095°
Longitude of the node(Ω)168.100±0.164°
Periastronepoch(T)1,909.361±0.024
Argument of periastron(ω)
(secondary)		23.917±0.214°
Details
ξ Boo A
Mass0.88±0.03[7]M☉
Radius0.817±0.007[7]R☉
Luminosity0.562±0.036[7]L☉
Surface gravity(logg)4.561±0.017[7]cgs
Temperature5,545±92[7]K
Metallicity[Fe/H]−0.10±0.04[7]dex
Rotation6.2[8]d
Age200[9]Myr
ξ Boo B
Mass0.66±0.07[10]M☉
Radius0.61[8]R☉
Luminosity (visual, LV)0.061L☉
Temperature4,350±150[10]K
Rotation11.5[8]d
Other designations
ξ Boo,37 Boötis,BD+19°2870,HD131156,HIP72659,HR5544,SAO101250
Database references
SIMBADdata
ARICNSdata

Xi Boötis,Latinisedfrom ξ Boötis, is abinary star[10]system located at a distance of 22light-yearsaway fromEarth.It is the nearest visible star in theconstellationBoötes.The brighter, primary component of the pair has avisual magnitudeof 4.70, making it visible to the naked eye.

Properties

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A light curve for Xi Bootis, showing the average of theb and ymagnitudes as a function of time. Adapted from Lockwoodet al.(2007)[11]

The primary star in this system is aBY Draconis variablewith anapparent magnitudethat varies from +4.52 to +4.67 with a period just over 10 days long, and is classified as aG-type main-sequence star.Themagnetic activityin the star'schromospherevaries with time, but no activity cycle has yet been found.[12]It has 88% ofthe massand 82% ofthe radiusof the Sun, but shines with just 56% theSun's luminosity.[7]The secondary component is aK-type starwith just 66% of the Sun's mass and 61% of the Sun's radius. As of 2019, it is located at anangular separationof5.20″from the primary, along aposition angleof 298°.[13]

The pair follow a wide, highly elliptical orbit around their commonbarycenter,completing an orbit every 151.5 years.Radial velocitiestaken of the primary as part of anextrasolar planetsearch show a linear trend in the velocities which is likely due to the secondary star.[14]The pair can be resolved even through smaller telescopes. The binary system contains some of the closest young solar-type stars to the Sun, with a system age of about 200 million years old.[9]

The primary star (A) has been identified as a candidate for possessing aKuiper-like belt,[15]based oninfraredobservations. The estimated minimum mass of this dust disk is 2.4 times the mass of the Earth'sMoon.(Compare to the value of 8.2 lunar masses for the Kuiper belt.)[16]

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 be3.8AUfor the primary and 3.5 AU for the secondary. A planet orbiting outside of both stars would need to be at least 108 AU distant.[17]

References

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  1. ^abvan Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction",Astronomy and Astrophysics,474(2): 653–664,arXiv:0708.1752v1,Bibcode:2007A&A...474..653V,doi:10.1051/0004-6361:20078357,S2CID18759600Note:see VizieR catalogueI/311.
  2. ^Evans, D. S. (June 20–24, 1966), "The Revision of the General Catalogue of Radial Velocities", in Batten, Alan Henry; Heard, John Frederick (eds.),Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30,vol. 30, University of Toronto:International Astronomical Union,p. 57,Bibcode:1967IAUS...30...57E
  3. ^abcBrown, A. G. A.;et al. (Gaia collaboration) (2021)."GaiaEarly 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.S2CID227254300.(Erratum:doi:10.1051/0004-6361/202039657e).Gaia EDR3 record for this sourceatVizieR.
  4. ^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,S2CID119187733.
  5. ^abcBrown, A. G. A.;et al. (Gaia collaboration) (2021)."GaiaEarly 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.S2CID227254300.(Erratum:doi:10.1051/0004-6361/202039657e).Gaia EDR3 record for this sourceatVizieR.
  6. ^Wielen, R. (November 1962), "Automatic orbit computation for visual binaries",Astronomical Journal,67:599–607,Bibcode:1962AJ.....67..599W,doi:10.1086/108791The data is from Orbit #3; the solution used by the 6th Washington Double Star catalogue forWDS 14514+1906Archived2012-02-03 at theWayback Machine.
  7. ^abcdefgKarovicova, I.; White, T. R.; Nordlander, T.; Casagrande, L.; Ireland, M.; Huber, D. (2022). "Fundamental stellar parameters of benchmark stars from CHARA interferometry -- II. Dwarf stars".Astronomy & Astrophysics.658:A47.arXiv:2109.06203.Bibcode:2022A&A...658A..47K.doi:10.1051/0004-6361/202141833.S2CID219558406.
  8. ^abcWood, Brian E.; Linsky, Jeffrey L. (July 2010), "Resolving the ξ Boo Binary with Chandra, and Revealing the Spectral Type Dependence of the Coronal" FIP Effect "",The Astrophysical Journal,717(2): 1279–1290,arXiv:1005.3281,Bibcode:2010ApJ...717.1279W,doi:10.1088/0004-637X/717/2/1279,S2CID53394680
  9. ^abMamajek, 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,S2CID27151456
  10. ^abcFernandes, J.; et al. (October 1998), "Fundamental stellar parameters for nearby visual binary stars: eta Cas, XI Boo, 70 OPH and 85 Peg. Helium abundance, age and mixing length parameter for low mass stars",Astronomy and Astrophysics,338:455–464,Bibcode:1998A&A...338..455F
  11. ^Lockwood, G. W.; Skiff, B. A.; Henry, Gregory W.; Henry, Stephen; Radick, R. R.; Baliunas, S. L.; Donahue, R. A.; Soon, W. (July 2007)."Patterns of Photometric and Chromospheric Variation among Sun-like Stars: A 20 Year Perspective".The Astrophysical Journal Supplement Series.171(1): 260–303.arXiv:astro-ph/0703408.Bibcode:2007ApJS..171..260L.doi:10.1086/516752.S2CID18775739.Retrieved1 July2022.
  12. ^Finley, Adam J.; et al. (May 2019)."The Effect of Magnetic Variability on Stellar Angular Momentum Loss. II. The Sun, 61 Cygni A, ɛ Eridani, ξ Bootis A, and τ Bootis A".The Astrophysical Journal.876(1): 14.arXiv:1903.09871.Bibcode:2019ApJ...876...44F.doi:10.3847/1538-4357/ab12d2.S2CID85500195.44.
  13. ^Mason, B. D.; et al. (2014)."The Washington Visual Double Star Catalog".The Astronomical Journal.122(6): 3466.Bibcode:2001AJ....122.3466M.doi:10.1086/323920.Retrieved2015-07-22.
  14. ^Howard, Andrew W.; Fulton, Benjamin J. (2016). "Limits on Planetary Companions from Doppler Surveys of Nearby Stars".Publications of the Astronomical Society of the Pacific.128(969). 114401.arXiv:1606.03134.Bibcode:2016PASP..128k4401H.doi:10.1088/1538-3873/128/969/114401.S2CID118503912.
  15. ^Hinshaw, Gary (February 3, 1997),Science Requirements Document(PDF),NASA JPL, archived fromthe original(PDF)on 2006-05-29,retrieved2006-08-10
  16. ^Holmes, E. K.; et al. (2003), "A Survey of Nearby Main-Sequence Stars for Submillimeter Emission",The Astronomical Journal,125(6): 3334–3343,Bibcode:2003AJ....125.3334H,doi:10.1086/375202
  17. ^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,S2CID118570249.
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