Categories
  • Henry Draper Catalogue objects
  • Hipparcos objects
  • Objects with variable star designations
    •   Encyclosphere.org ENCYCLOREADER
      supported by EncyclosphereKSF

    HO Telescopii

    Topic: Astronomy

     From Handwiki - Reading time: 3 min
    Short description: Star in the constellation Telescopium
    HO Telescopii
    HOTelLightCurve.png
    A visual band light curve for HO Telescopii, adapted from Sürgit et al. (2017)[1]
    Observation data
    Equinox J2000.0]] (ICRS)
    Constellation Telescopium
    Right ascension  19h 51m 58.93159s[2]
    Declination −46° 51′ 42.4354″[2]
    Apparent magnitude (V) 8.22[3] (Max)
    Characteristics
    Spectral type A7III(m)[4]
    Variable type Algol[5]
    Astrometry
    Radial velocity (Rv)−5.91±0.09[6] km/s
    Proper motion (μ) RA: +1.814[2] mas/yr
    Dec.: −33.369[2] mas/yr
    Parallax (π)3.5831 ± 0.0796[2] mas
    Distance910 ± 20 ly
    (279 ± 6 pc)
    Orbit[6]
    Period (P)1.613097 d
    Semi-major axis (a)≥0.019±0.0001 astronomical unit|AU
    Eccentricity (e)0.00[7]
    Inclination (i)82.7±0.5[8]°
    Periastron epoch (T)2,451,875.06581±0.00027 HJD
    Semi-amplitude (K1)
    (primary)    		131.11±0.18 km/s
    Semi-amplitude (K2)
    (secondary)    		142.35±0.18 km/s
    Details
    A
    Mass1.88±0.04[1] M☉
    Radius2.28±0.15[1] R☉
    Age1.1[1] Gyr
    B
    Mass1.73±0.04[1] M☉
    Radius2.08±0.16[1] R☉
    Other designations
    HO Tel, CD−47°13121, HD 187418, HIP 97756, SAO 229902[9]
    Database references
    SIMBADdata

    HO Telescopii is an eclipsing binary star system located in the southern constellation of Telescopium. The maximum apparent visual magnitude of 8.22[3] is too faint to be visible to the naked eye. The system is located at a distance of approximately 910 light years based on parallax.[2] The combined stellar classification of the system is A7III(m),[4] matching an evolved A-type star[10] that is possibly metallic-lined. The system is around 1.1[1] billion years old and consists of two stars of similar mass and size.[1]

    The variability of this system was discovered by W. Strohmeier, R. Knigge, and H. Ott in 1965.[11][12] It is a detached binary system with both components filling three-fourths of their respective Roche lobes.[1] Their orbital period is 1.613097[6] days with a circularized orbit,[7] and the orbital plane is inclined by 83° to the line of sight from the Earth; close to edge-on.[8] As a consequence, they form an Algol-like eclipsing binary with a magnitude decrease of 0.51 during the primary eclipse and 0.45 during the secondary eclipse.[3]

    References

    1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 Sürgit, D. et al. (July 2017). "Absolute parameters of detached binaries in the southern sky - III: HO Tel". New Astronomy 54: 109–114. doi:10.1016/j.newast.2017.01.013. Bibcode: 2017NewA...54..109S. 
    2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
    3. ↑ 3.0 3.1 3.2 Avvakumova, E. A. et al. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten 334 (8): 860. doi:10.1002/asna.201311942. Bibcode: 2013AN....334..860A. 
    4. ↑ 4.0 4.1 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode: 1978mcts.book.....H. 
    5. ↑ Samus, N. N. 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. 
    6. ↑ 6.0 6.1 6.2 Sürgit, D. et al. (July 2015). Rucinski, Slavek M.; Torres, Guillermo; Zejda, Miloslav. eds. "First Spectroscopic Solutions of Two Southern Eclipsing Binaries: HO Tel and QY Tel". Living Together: Planets, Host Stars and Binaries, Proceedings of a conference held 8-12 September 2014 in Litomyšl, Czech Republic. ASP Conference Series (San Francisco: Astronomical Society of the Pacific) 496: 258. Bibcode: 2015ASPC..496..258S. 
    7. ↑ 7.0 7.1 Khaliullin, Kh. F.; Khaliullina, A. I. (January 2010). "Synchronization and circularization in early-type binaries on main sequence". Monthly Notices of the Royal Astronomical Society 401 (1): 257–274. doi:10.1111/j.1365-2966.2009.15630.x. Bibcode: 2010MNRAS.401..257K. 
    8. ↑ 8.0 8.1 Grygar, J.; Horak, T. B. (1980). "Orbital Elements of the Eclipsing Binaries RW CrA and HO Tel from Multicolour Light Curves". Bulletin of the Astronomical Institute of Czechoslovakia 31: 297. Bibcode: 1980BAICz..31..297G. 
    9. ↑ "HO Tel". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HO+Tel. 
    10. ↑ Spoelstra, T. A. Th.; Van Houten, C. J. (1972). "Five-colour photometry of the eclipsing binary HO Telescopii". Astronomy and Astrophysics Supplement 7: 83. Bibcode: 1972A&AS....7...83S. 
    11. ↑ Sistero, R. F.; Candellero, B. A. (August 1979). "HO Telescopii: Light Elements". Information Bulletin on Variable Stars 1666: 1. Bibcode: 1979IBVS.1666....1S. 
    12. ↑ Strohmeier, W. et al. (February 1965). "Bright Southern BV-Stars". Information Bulletin on Variable Stars 81: 1. Bibcode: 1965IBVS...81....1S. 



    Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:HO_Telescopii&oldid=2995070"
    This article is licensed under CC BY-SA 3.0.
    Original source: https://handwiki.org/wiki/HO Telescopii
    Status: article is cached
    Encyclosphere.org EncycloReader is supported by the EncyclosphereKSF