We have detected several candidates for Cepheid variables in eclipsing binary systems in the Large Magellanic Cloud 10 (LMC). Using high-resolution spectra, we confirmed the discovery of a classical ...

Stars have been observed and recorded since ancient times. Practices of documenting brightness led to observations of variability. Optical CCD observations of eclipsing binary stars were made with ...

Abstract: To increase maximum radar range, determined with effective radiated energy, pulse duration has to be expanded. However, a larger pulse increases the blind zone, i.e. the eclipsing effect is ...

Abstract: A multisite photometric campaign for the β Cephei and eclipsing variable 16 Lacertae is reported. 749 h of high-quality differential photoelectric Strömgren, Johnson and Geneva time series ...

A variable star is, quite simply, a star that changes brightness. A star is considered variable if its apparent magnitude (brightness) is altered in any way from our perspective on Earth. These ...

New UBV photometry of DN Cas indicates eclipse depths in V of 0ṃ4 and 0ṃ3 and an ephemeris for the primary of JD 2441388.571 + 2ḑ310955 E. Since our new period is twice that of Hoffmeister, DN Cas is ...

We introduce a special class of functions for mathematical modeling of periodic signals of special shape with irregularly spaced arguments. This method was developed for determination of ...

The emission lines found in the majority of cataclysmic variables are generally used as tracers of accretion flows which dominate the light at optical wavelengths. It has been suggested from previous ...

A new eclipsing variable with period 0ḍ959 or 1ḍ918 has been found near the cluster NGC 1783 in the Large Magellanic Cloud. Journal Information Publications of the Astronomical Society of the Pacific, ...

A 2D histogram is generated of the lightcurve along time and flux directions the shift of the mode of the flux in time is compared to a limit value. If the number of peaks is between nlim and plim the ...

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