scholarly journals LARGE LYOT-CORONOGRAPH OF NIKOLSKY-SAZANOV DESIGN AT THE CRIMEAN ASTROPHYSICAL OBSERVATORY

2019 ◽  
Author(s):  
A.N. Babin ◽  
◽  
A.N. Koval ◽  
Keyword(s):  
Crimean Astrophysical Observatory

On the Inhomogeneity of Chemical Composition over the Surface of 21 Per

1976 ◽  
Vol 32 ◽  
pp. 343-349
Author(s):  
Yu.V. Glagolevsky ◽  
K.I. Kozlova ◽  
V.S. Lebedev ◽  
N.S. Polosukhina
Keyword(s):  
Chemical Composition ◽  
Spectral Line ◽  
Variable Star ◽  
Radial Velocities ◽  
Crimean Astrophysical Observatory ◽  
Line Intensities ◽  
Magnetic Variable

SummaryThe magnetic variable star 21 Per has been studied from 4 and 8 Å/mm spectra obtained with the 2.6 - meter reflector of the Crimean Astrophysical Observatory. Spectral line intensities (Wλ) and radial velocities (Vr) have been measured.

scholarly journals V 1500 Cyg: Slow Variability in Post-nova Stage

1990 ◽  
Vol 122 ◽  
pp. 68-70
Author(s):  
E. Pavlenko
Keyword(s):  
Ussr Academy ◽  
Crimean Astrophysical Observatory ◽  
Photometric Observations ◽  
The Mean ◽  
Academy Of Sciences

Regular photometric observations of V1500 Gyg (Nova Cygni 1975) have been carried out at the Crimean Astrophysical Observatory of the USSR Academy of Sciences from 1975 till now. The 0.5 m telescope equipped with a TV system is used to estimate the star brightness in V.The decline of the mean brightness is presented in Figure 1. The solid lines (1) and (2) show the changes of the V brightness according to Patterson (1979) and Arkhipova and Zaitseva (1978), respectively. The dotted line is drawn according to our data (Pavlenko 1988). The arrows indicate the amplitudes of the light and colour variations.

Very high energy y-rays from Cygnus X-3

1981 ◽  
Vol 301 (1462) ◽  
pp. 633-634 ◽  
Keyword(s):  
Light Curve ◽  
High Energy ◽  
Crimean Astrophysical Observatory ◽  
Sharp Peak ◽  
X Rays ◽  
Very High Energy ◽  
Time Variations ◽  
Comparison Of The Results ◽  
Very High

Very high energy y-rays (above 10 12 eV) from Cyg X-3 have been observed for 7 years at the Crimean Astrophysical Observatory by means of the Cherenkov technique. These observations enable us to find the derivative with time of the 4.8 hour periodicity. As is well known, the observations of X -rays have revealed time variations of the Cyg X-3 period (see, for instance, Eisner et al. 1979). The ‘light’ curve for very high energy y-rays has a sharp peak lasting 15 minutes and differs significantly from the ‘light’ curve for X-rays. For this reason the comparison of the results in these two regions is important.

scholarly journals The Nova-Likes AC Cnc, RW Tri, UX UMa and the Nova DQ Her: Common and Different Properties

1996 ◽  
Vol 158 ◽  
pp. 13-14
Author(s):  
E. S. Dmitrienko
Keyword(s):  
High Speed ◽  
Crimean Astrophysical Observatory ◽  
The Other ◽  
Orbital Cycles

AbstractAn analysis of the main photometric properties of the nova-like variables AC Cnc, RW Tri and UX UMa, and Nova Her 1934 (DQ Her) is presented. The analysis is based on simultaneous high-speed UBVRI photometry, covering several dozens of orbital cycles evenly distributed over 14 years (1982 ... 1995) for DQ Her, and over 11 years (1985 ... 1995) for the other three stars. All data have been obtained with the 1.25 m telescope at the Crimean Astrophysical Observatory.

scholarly journals Precision of Ephemerides for Space Missions

1971 ◽  
Vol 12 ◽  
pp. 639-642 ◽  
Author(s):  
B.G. Marsden
Keyword(s):  
Space Missions ◽  
Crimean Astrophysical Observatory ◽  
Minor Planet ◽  
Minor Planets ◽  
Synodic Period

One of the most extensive programs of systematic observations of minor planets currently being conducted is that at the Crimean Astrophysical Observatory. The observed positions, together with the residuals from the predictions in the annual Ephemeris volumes, have been listed in the Minor Planet Circulars for several years now; and inspection of the residuals yields information about the accuracy of minor planet ephemerides as a whole.The observations are made using a 40 cmf/4 double astrograph, the limiting magnitude being about 18. Between June 1968 and October 1969, corresponding to one synodic period of an average minor planet, about 40 percent of all the numbered objects were observed. These observations may be regarded as reasonably representative of all the planets. Observations were made of 60 of the objects with numbers in the 100’s and only 29 of those in the 1100’s, but in general the distribution was surprisingly uniform.

scholarly journals Spectral Analysis of a White Light Flare

1989 ◽  
Vol 104 (2) ◽  
pp. 247-250
Author(s):  
Boyer R. ◽  
Sotirovski P.
Keyword(s):  
Spectral Analysis ◽  
Solar Flare ◽  
Electron Density ◽  
White Light ◽  
Time Profile ◽  
Crimean Astrophysical Observatory ◽  
Stark Broadening ◽  
Emission Mechanism ◽  
Measured Time ◽  
The Continuum

AbstractWe discuss observations of a solar flare located close to the limb (N15, W75) at 07 00 UT on 26 September 1963 from the Crimean Astrophysical observatory.Stark broadening and hence electron density have been obtained from measured time profile and half-width of the Baliner series lines from Hα to H M.The emission mechanism has been deduced from a study of the continuum intensity as a function of wavelength.

scholarly journals On possible mass loss from the supergiant RHO Cassiopeia

1981 ◽  
Vol 59 ◽  
pp. 117-118
Author(s):  
M. Boyarchuk
Keyword(s):  
Mass Loss ◽  
Crimean Astrophysical Observatory ◽  
High Luminosity ◽  
Very High

The supergiant Rho Cas F8Ia has a very high luminosity. Astronomers have payed attention to this star in August 1946, when its by its brightness had dropped from 4.2 to 6.2. The systematic spectrographic observations of Rho Cas are beeing carried out at the Crimean Astrophysical Observatory since 1965. No large light variations were observed during that time.

scholarly journals Kharkiv study of near-Earth asteroids

2006 ◽  
Vol 2 (S236) ◽  
pp. 385-390 ◽  
Author(s):  
Yu. N. Krugly ◽  
N. M. Gaftonyuk ◽  
I. N. Belskaya ◽  
V. G. Chiorny ◽  
V. G. Shevchenko ◽  
...  
Keyword(s):  
Surface Properties ◽  
Crimean Astrophysical Observatory ◽  
Photometric System ◽  
Rotation Periods ◽  
Photometric Observations ◽  
National University ◽  
Ccd Observations ◽  
Asteroid Hazard ◽  
Near Earth Asteroids

AbstractThe regular CCD observations of near-Earth asteroids (NEAs) in the Institute of Astronomy of Kharkiv National University were initiated in 1995 within the framework of asteroid hazard problem in collaboration with the DLR, Institute of Planetary Research (Berlin). The main aim of the study is a determination of rotation periods and shapes of NEAs as well as astrometry of newly discovered objects. We also carry out the absolute photometry of NEAs in BVRI bands in order to put constraints on surface properties and to estimate their diameters. The observations are carried out with 0.7-m telescope of the Institute of Astronomy (Kharkiv) and with 1-m telescope of the Crimean Astrophysical Observatory (Simeiz) in the standard Johnson-Cousins photometric system. Some observations were made as an optical support of radar observation of NEAs. We present the results of photometric observations of 21 NEAs obtained in 2004-2006 which include asteroid rotation properties, diameters and shapes.

scholarly journals The Hβ line shape of Akn 120

2000 ◽  
pp. 7-33 ◽  
Author(s):  
N. Stanic ◽  
L.C. Popovic ◽  
A. Kubicela ◽  
E. Bon
Keyword(s):  
Line Shape ◽  
Crimean Astrophysical Observatory ◽  
Broad Line ◽  
Line Profiles ◽  
Shape Variation

We present here the Akn 120 H? line profiles from 97 spectra observed from 1977 till 1990 at Crimean Astrophysical Observatory (Appendix 1). The H? line has been fitted with three broad and one narrow Gaussian throughout the whole considered period. The central broad components of the H? and a shelf cause the H? line shape variation. Three broad Gaussians may suggest the existence of three broad line regions in the central part of the Akn 120. Long-term H? line shape variations in spectra of this galaxy are discussed.

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