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A precise analytic expression is obtained for calculation of the spotted stars light variations in the case of arbitrary radius of the spot and arbitrary inclination of the rotation axis of the star with reference to the line of sight by adopting a linear law for limb darkening of both the star and the spot but with different coefficients of darkening. The results obtained can be used for the calculation of the light curves of the spotted stars with an arbitrary number of spots on the surface of the star. more...

On the basis of the analytical solution of the direct photometric problem for spotted stars is obtained solution of the corresponding inverse problem. It is given expressions for determining of the location, size, and temperature of the spot and of the inclination of the rotational axis of the spotted star with regard to the line-of-sight. more...

In the framework of the direct photometric problem we obtained an analytical representation of the light variations of binary systems of stars one of which with spots on its surface. The photometric effect is due to the mutual eclipses and to the rotation of the spotted component. These expressions can be used for the solution of the inverse problem for spotted stars. more...

Multicolour photometry of the polar AM Her was obtained during 3 observational seasons (1994/95/96). The star was in its high state for most of the observations. It was in its low state in '96 April. It was established that these two states differ not only in the average light level but in the larger amplitudes of variations at low state than at high state. Moreover the energy distributions of the two states differ in the stronger dependence of the flux on ν at high state than at low state. The Fourier analysis of the photometric data shows variability with the spectroscopic (orbital) period. The amplitudes of this variability in all colours are about two times bigger at low state than at high state. An attempt to explain the photometric behaviour of AM Her by a model of dominant emission of two hot spots at the magnetic poles of the white dwarf was made and the spot parameters were determined. more...

BVRI photometry of SS Cyg from the end of 1996 and the beginning of 1997 is presented. The star underwent an eruption around December 11. The amplitude of which was slightly bigger than those of observed earlier eruptions. We saw some indication of the future outburst in the decreasing of brightness in all colours by about 0.4 mag during the last two weeks before the event. The emission of the system moved strongly to the shorter wavelengths at outburst. Our multicolour data confirm the existence of a light variability with the orbital (spectroscopic) period at quiescence. Moreover we found for the first time that this variability exists also at outburst but its amplitude is 3–5 times smaller. Whereas the amplitudes of the orbital variability at quiescence decrease to the longer wavelengths, they increase at outburst to the longer wavelengths. The orbital folded curve at quiescence has two-wave shape and was fitted well by the different visibility of two diametrical opposite hot spots (210000 K) with angular size 100on the magnetic poles of the white dwarf. An analogy between the two basic states of the U Gem-star SS Cyg, the polar AM Her and Z Cam-star RX And was found. more...

In the framework of the direct photometric problem we obtained an analytical representation of the light variations of spotted stars adopting quadratic limb-darkening law. The btained results can be a basis for the solution of the inverse photometric problem for spotted late FK Com-type giants. more...

In the framework of the direct photometric problem for spotted stars we obtained an analytic solution adopting gradually changing of the spot temperature from the center to the outskirts of the spots. The results are intended for the solution of the corresponding inverse problem that could give information for the mechanisms leading to spot creating. more...

The results from the simultaneous observations in B and R colours of AM Her are presented. Analysis of these data shows the following: (a) There are always two clear minima in the R light curves, while the secondary minimum in B light curves sometimes is not well defined; (b) The times of the minima in R and B colour nearly coincide; (c) The photometric period changes remarkably from cycle to cycle but its mean value remains constant; (d) Short stillstands on the increasing branches of the two minima are seen similar to those visible in UX UMa-type cataclysmic stars; (e) Besides the irregular flickering with time scale of a few minutes, a variability with a period 20.28 min in the two colours is established. more...

This paper presents an extension of the method of the characteristic points by Kjurkchieva (1987, 1989). This method for the analysis of light curves of spotted stars is further developed by including spectral information. Expressions describing the variation of the rotation broadening of spectral features arising from a star spot are derived for a known spot configuration. The results are used in the solution of the inverse problem by the method of the characteristic points. It is shown that the rotation broadening of spectral features from star spots can be used to easily determine the angular size and the polar distance of a circular spot. It turns out that the equatorial velocity and radius of the spotted star can be obtained in some cases by the combined analysis of the photometric and spectral data. more...

In the framework of the direct photometric problem we obtained analytic expressions describing the light variations of spotted stars in case of arbitrary limb-darkening law. These could be used as a basis for solution of the inverse photometric problem for arbitrary types of rotating stars characterized by surface spots. more...

The solution of the inverse photometric problem for spotted stars obtained on the basis of the analytical solution of the direct problem is applied to II Peg 1977 light curve. The geometric parameters of the spot configuration so obtained are unambigously determined in contrast to the cases when analysis of the light curve is done on the basis of numerical modelling. A comparison between both methods has been carried out. more...

The cataclysmic star RX And was observed in the states standstill and quiescence. They differed not only in the light level but in the type of variations around this level. The standstill observed by us turned out quite near to the maximum light and its duration was unusually long. The energy distribution of RX And at the standstill seemed similar to the spectrum of an accretion disk. Two variabilities with periods 3 h 43 min and 1 h 26 min were found at the standstill but only the second of them was present at quiescence too. The star did not show light variability with the spectroscopic period. We tried to interpret some of the results by the supposition that the Z Cam-stars are an intermediate subtype of the cataclysmic stars evolving from UX UMa-subtype to U Gem-subtype and that probably RX And presents a pattern of Z Cam-star that is very near to the U Gem-subtype. more...