| Radio radiation can be detected in various types of stars on the H-Rdiagram,and it is closely related to the physical parameters of the star,the activity of the star and the evolution of the star.A comprehensive grasp of the physical properties of stars requires the study of more bands like optical or radio bands.The optical and radio observations of stars are an important means to study physical parameters,magnetic activities,mass transfer and other physical processes of stars.This is not only of great significance to the study of the physical properties of radio eclipsing binaries,but also will lay a solid observation foundation for the theoretical study of radio stars.The main findings of our study are as follows:Wendker has collected stars with radio radiation for many years and there are at least 150 eclipsing binary systems in his work.From this catalog,it is shown that the spectral type of the primary components of these eclipsing binaries show a decreasing trend from type A to type M,and there is a weak linear correlation between radio flux at different frequencies.In this paper,the physical properties of five eclipsing binaries have been studied,of which three(V CRT,WY CNC and CG CYG)are from the radio catalogue collected by Wendker,and their new CCD data observed by the SARA 60 cm telescope and the NAOC 85 cm telescope in Chile.Using these data and the apparent velocity studied by previous studies,the orbital parameters of these eclipsing binaries are obtained by using the Wilson-Devinney program.We updated their epoch formula by analyzing their minimum moments,and calculated that the orbital period of V Crt increases at a rate of 2.7972(±2.1421)10-9days/year.The orbital period of WY Cnc decreases at a rate of 8.641(±0.004)10-8days/year.There is a third celestial body with a minimum mass of 0.14 solar masses with a period of about 59 years for CG Cyg and analyzed the second oscillation by the(O-C)II.The periodic variations of WY Cnc and CG Cyg are more likely by internal magnetic activity and stellar winds.For the other two eclipsing binaries,V582 Lyr and V1016Oph,we also obtained by the SARA 91.4cm telescope and the 60cm telescope to obtain the CCD.The apparent velocity was determined by LAMOST spectral measurement,and the V582 Lyr spectral type was identified as K5 type.The observed H?line was absorbed,and there was H?line emission after subtracting from the template star spectrum,and there was weak chromosphere activity on the surface.The spectral type of V1016 Oph is determined to be G8 by using the low dispersion spectrum taken by the 2.4-meter telescope in Lijiang,and the epochal formula is updated.The orbital periods of both V582 Lyr and V1016 Oph are decreasing.Finally,Wilson Devinney program was used to obtain the orbit parameters from the CCD data.Meanwhile,because they are eclipsing binary stars,the connection degrees of V582Lyr and V1016 Oph are 3.35(±0.08)%and 41.0(±0.1)%,respectively.With information on more than 900,000 targets from the FIRST Radio Sky Survey,LAMOST DR7 has released more than 20 million spectrum.More than20,000 dispersive spectra with low resolution and more than 1,000 dispersive spectra with medium resolution were obtained by cross-identification with LAMOST spectrum database of the FIRST radio sky survey.The equivalent widths of different chromosphere activity indexes were obtained by using HAMMER program.We found no significant correlation between the radio flux peak(Fpeak)and the equivalent widths(EW)of H?emission lines from the low resolution dispersion.The H?equivalent widths calculated from the medium resolution dispersion spectra show a positive linear correlation with the radio flow peak(Fpeak).At present,we still lack direct radio observation data.In the future,we can use the Five-hundred-meter Aperture Spherical Radio Telescope(FAST)built in Pingtang County,Guizhou Province to observe the radio band of the target. |
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