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Double and Multiple Star Speckle Observations at the 6-m Telescope

Published online by Cambridge University Press:  12 April 2016

I.I. Balega ,
Y.Y. Balega ,
V.A. Vasyuk  and
J.J. McManus
I.I. Balega
Affiliation:
Special Astrophysical Observatory of the Russian Academy, Zelenchuk region, Karachai–Cherkesia 357147, Russia
Y.Y. Balega
Affiliation:
Special Astrophysical Observatory of the Russian Academy, Zelenchuk region, Karachai–Cherkesia 357147, Russia
V.A. Vasyuk
Affiliation:
Special Astrophysical Observatory of the Russian Academy, Zelenchuk region, Karachai–Cherkesia 357147, Russia
J.J. McManus
Affiliation:
Florida Institute of Technology, 150 West University Blvd., Melbourne, FL, USA

Extract

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During the last 15 years more than 9,000 speckle interferometric measurements of binary stars have been collected using large optical telescopes (McAlister & Hartkopf 1988). Among them a significant contribution to the world speckle data has been made by the 6-m telscope near Zelenchuk. Up to now this instrument provides the maximal spatial resolution for single–aperture telescopes. First speckle images of the binary Capella were recorded at the telescope in 1977 (Balega & Tikhonov 1977), but we spent 5 more years to create special television techniques for photon counting and digital means for image processing before we started the regular interferometric program of binary observations in the wide range of stellar magnitudes. At first, the measurements were conducted in cooperation with French astronomers from the Centre d’Etudes et de Recherches Geodynamiques et Astronomiques using the optical camera and the television detector developed by Blazit et al. (1977). Since 1983 our equipment has been in use. The program of observations was oriented upon the traditional problems of multiple star speckle interferometry:

  1. 1. Determination of stellar distances and masses for different types of binaries whose orbital elements can be derived. This includes already known fast visual and astrometric pairs with undetermined orbits, spectroscopic binaries that can be resolved directly, and newly discovered interferometric pairs which show fast orbital motion. The main attention was devoted to the late–type dwarfs in the vicinity of the Sun.

  2. 2. Search for the secondary components whose existence could explain anomalies of stellar spectra or photometry (stars with composite spectra, occultation binaries, etc.)

  3. 3. Study of unusual binaries (symbiotic stars, binaries with relativistic components, such as SS 433, etc.)

Type
High Resolution At Visual Wavelengths
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 469 - 476
Copyright
Copyright © Astronomical Society of the Pacific 1992

References

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