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HR 6384

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HR 6384

Thevisual bandlight curveof HR 6384, adapted from Walkeret al.(1985)[1]
Observation data
EpochJ2000EquinoxJ2000
Constellation Ara
Right ascension 17h14m13.40536s[2]
Declination –56° 53′ 18.6897″[2]
Apparent magnitude(V) 6.153[1]
Characteristics
Spectral type M1/M2II/III + A[3]
U−Bcolor index +1.340[1]
B−Vcolor index +1.787[1]
Variable type ellipsoidal variable[4]
Astrometry
Radial velocity(Rv)−34.0±4.0[5]km/s
Proper motion(μ)RA:2.760[2]mas/yr
Dec.:–7.033[2]mas/yr
Parallax(π)2.2407 ± 0.1939mas[2]
Distance1,500 ± 100ly
(450 ± 40pc)
Absolute magnitude(MV)−2.20[5]
Details
Radius160.39+9.31
−23.02[2]R☉
Luminosity3,732±368[2]L☉
Temperature3,562+287
−99[2]K
Other designations
V829 Ara,CD–56°6744,HD155341,HIP84311,HR6384,SAO244539[6]
Database references
SIMBADdata

HR 6384is abinary starsystem in the southernconstellationofAra,the Altar. The system is faintly visible to the naked eye with a combinedapparent visual magnitudethat fluctuates around 6.153,[1]and it is located at a distance of approximately 1,300light-years(400parsecs) from theSun.[2]It is drifting closer with aradial velocityof around −34 km/s.[5]

The system appears to be a close, interacting binary with a hot secondary component of class A or hotter.[7]It forms a suspectedellipsoidal variable[4]with a period of 80 days and an amplitude variation of 0.08 in magnitude.[8]The primary component is an agingred giant/bright giantwith astellar classificationof M1/M2II/III,[3]currently on theasymptotic giant branch.[9]With the supply ofhydrogenat itscoreexhausted, it has expanded to 160 times thegirth of the Sun.It is radiating 3,562 times theluminosity of the Sunfrom its enlargedphotosphereat aneffective temperatureof 3,562 K.[2]

References

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  1. ^abcdeWalker, W. S. G.; Marino, B. F.; Herdman, G. (August 1985), "Photometry of HR 6384 - an 80 Day Ellipsoidal Binary?",Information Bulletin on Variable Stars,2775:1,Bibcode:1985IBVS.2775....1W.
  2. ^abcdefghijBrown, A. G. A.;et al. (Gaia collaboration) (August 2018)."GaiaData Release 2: Summary of the contents and survey properties ".Astronomy & Astrophysics.616.A1.arXiv:1804.09365.Bibcode:2018A&A...616A...1G.doi:10.1051/0004-6361/201833051.Gaia DR2 record for this sourceatVizieR.
  3. ^abHouk, Nancy (1979),Michigan catalogue of two-dimensional spectral types for the HD stars,vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan,Bibcode:1978mcts.book.....H.
  4. ^abSamus, N. N.; et al. (2017), "General Catalogue of Variable Stars",Astronomy Reports,5.1,61(1): 80–88,Bibcode:2017ARep...61...80S,doi:10.1134/S1063772917010085,S2CID125853869.
  5. ^abcAnderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation",Astronomy Letters,38(5): 331,arXiv:1108.4971,Bibcode:2012AstL...38..331A,doi:10.1134/S1063773712050015,S2CID119257644.
  6. ^"V829 Ara".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2019-12-07.
  7. ^Ake, T. B.; Parsons, S. B. (March 1985), "HR 6384: a Probable Interacting Binary",Information Bulletin on Variable Stars,2686:1,Bibcode:1985IBVS.2686....1A.
  8. ^Hoffleit, Dorrit (1996), "A Catalogue of Correlations Between Eclipsing Binaries and Other Categories of Double Stars",The Journal of the American Association of Variable Star Observers,24(2): 105–116,Bibcode:1996JAVSO..24..105H.
  9. ^Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun",Astronomical Journal,104(1): 275–313,Bibcode:1992AJ....104..275E,doi:10.1086/116239.
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