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This paper presents new CCD BVRI light curves of the newly discovered RS CVneclipsing binary V1034 Her in 2009 and 2010, which shapes are different fromthe previous published results. They show asymmetric outside eclipse and we tryto use a spot model to explain the phenomena. Using the Wilson-Devinney programwith one-spot or two-spots model, photometric solutions of the system andstarspot parameters were derived. Comparing the two results, it shows that thecase of two spots is better successful in reproducing the light-curvedistortions. For all the spot longitudes, it suggests that the trend towardsactive longitude belts and each active longitude belts might be switch.Comparing the light curves of 2009 and 2010, it indicates that the light curvechanges on a long time scale of one year, especially in phase 0.25. Inaddition, we also collected the values of the maximum amplitudes of photometricdistortion of the short-period RS CVn binary. We found for the first time thatthere is a trend of increasing activity with decreasing the orbital period.Finally, fitting all available light minimum times including our newly obtainedones with polynomial function confirmed that the orbital period of V1034underwent up increase.

research in astronomy and astrophysics/research in astronomy and astrophysics

The New RS CVn Binary V1034 Her Revisited and the orbital period -  Activity relation of Short-period RS CVn binaries using photometric  distortion amplitude