Langbahn Team – Weltmeisterschaft

HO Telescopii

HO Telescopii

A visual band light curve for HO Telescopii, adapted from Sürgit et al. (2017)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
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 mas[2]
Distance910 ± 20 ly
(279 ± 6 pc)
Orbit[6]
Period (P)1.613097 d
Semi-major axis (a)≥0.019±0.0001 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. ^ a b c d e f g h i Sürgit, D.; et al. (July 2017). "Absolute parameters of detached binaries in the southern sky - III: HO Tel". New Astronomy. 54: 109–114. Bibcode:2017NewA...54..109S. doi:10.1016/j.newast.2017.01.013.
  2. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data 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 source at VizieR.
  3. ^ a b c Avvakumova, E. A.; et al. (October 2013). "Eclipsing variables: Catalogue and classification". Astronomische Nachrichten. 334 (8): 860. Bibcode:2013AN....334..860A. doi:10.1002/asna.201311942. hdl:10995/27061.
  4. ^ a b Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
  5. ^ 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.
  6. ^ a b c 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. 496. San Francisco: Astronomical Society of the Pacific: 258. Bibcode:2015ASPC..496..258S.
  7. ^ a b 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. Bibcode:2010MNRAS.401..257K. doi:10.1111/j.1365-2966.2009.15630.x.
  8. ^ a b 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. Retrieved 2020-12-12.
  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.
Quelle: https://en.wikipedia.org/wiki/HO_Telescopii