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VII SMALL ASTRONOMICAL TELESCOPE FACILITIES

The Role of Public Observatories in Astronomical Observations: T. Kogure

 
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Construction of telescopes for non-academic use in public observatories in Japan (Kuroda 1993).
 
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Bisei Astronomical Observatory which is located in one of the best sites for astronomical observations in Japan and equipped with a telescope of 101-cm aperture, constructed with many new technical ideas for observing stars. The dome is separated from the main building to avoid every possible heat source which may distort air flows in and around the dome. The open space under the dome was left for the same reason to keep the steady flow of winds (Courtesy of T. Kogure).
 

Small Telescopes in Research and Education: R.K. Kochhar

 

Networking of Small Astronomical Telescope Facilities in Education and Research Programmes on Subjects Such as Variable Stars and Near-Earth Objects: S. Frandsen

 

Single-Site and Multi-Site Photometric Research Programmes for Small Telescopes: P. Martinez

 
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The Johnson B light curve (top) and amplitude spectrum (bottom) of the rapid oscillations in the Ap star HD 84041, discovered using the 0.5-m telescope at Sutherland. The period of pulsation in this star is 15.0 minutes and the pulsation amplitude in this light curve is about 3.6 mag. The peak labelled "n1" in the Fourier spectrum is the pulsation frequency of the star. The other prominent peak at very low frequency is a gradual sky transparency variation.
 
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The long-term behaviour of the pulsation phase of HR 3831. In this diagram a constant pulsation frequency should be a horizontal straight line with (O-C) = 0.0. Sloping straight lines indicate changing frequency and abrupt vertical jumps indicate abrupt phase changes. The smooth, continuous variation in the data suggests a cycle frequency variation.
 
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The rotation light curve of the Ap star HD 84041; the rotation period is 3.69 d. The double wave suggests that one of the magnetic poles is seen at more favourable aspect than the other. Notice the changing amplitudes and the phase shift with filter from U to I.
 
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The extreme ultraviolet (top), X-ray (middle) and optical (bottom) light curves of the K star AB Dor. The optical light curve was acquired at Mount Stromlo, Sutherland and Las Campanas. The Sutherland portion of the light curve runs from ~ UT 7.85 to ~ UT 8.08 November 1993. Taken from Smith, S.M. et al. (1995 preprint).
 
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Light and colour curves of AI Vel for 1991 (filled circles), 1991-1992 (crosses), and 1992-1993 (open circles) (Kilkenny et al. 1995)).
 

Hands-On Astrophysics - and Beyond: J.R. Percy, J.A. Mattei