The observational study of the stellar magnetic activity is always the hot topic in Stellar physics field. Stellar prominence activity is an important part of the stellar magnetic activity. The observational study of stellar prominence activity, not only enriches our knowledge about the stellar magnetic activity, but also has great significance to the study of stellar coronal structure and coronal magnetic field topology. Consequently we purpose to detect the stellar prominences by means of high-resolution spectroscopy, and study the basic characteristics of the stellar prominence activity. We have made observational study for the eclipsing binary AR Lac、SZ Psc and the rapidly rotating single star LQ Hya with the 2.16 m telescope at the Xinglong station of the National Astronomical Observatories. The results are obtained as follows: For eclipsing binary AR Lac, we obtained two observing night spectra in Oct. 2009. Using the spectral subtraction technique, we analyzed H-alpha lines in out of eclipsing and total eclipsing. We found the absorption features in some residual H-alpha profiles, and calculated the distance from the rotation axis of the cooler component. The absorption is not likely caused by prominences because of the short distance. In addition, for the purpose of detecting the prominences, we also removed the effect of chromospheric activity in some residual spectra by Gaussian fitting, but we did not find the prominences. For rapidly rotating single star LQ Hya, we also obtained a batch of spectra. We firstly analyzed the H-alpha lines of the observed spectra using the spectral subtraction technique, and then detected the stellar prominences in residual spectra with two methods. However，there is no evidence of prominence activity. In Dec. 2010, we made high-resolution spectroscopic observation for the active eclipsing binary SZ Psc, and obtained many high-resolution echelle spectra. We performed the analysis for the spectra using the spectral subtraction technique, and found that the cooler component of the system has stronger chromospheric activity. Also, the subtracted spectra of the cooler component showed broad wings that can arise from microflaring. Some absorption features were detected in the subtracted H-alpha lines, and one of them probably results from the prominence-like material seen on the cooler component. According to the simple model, we calculated the distance of the prominence from the rotation axis of cooler component. Moreover, we made a comparison between the prominences seen in SZ Psc and in other binary systems. Finally, We have made a summary to our work, and made a prospect to the research works of this field in future. Considering our present research status, a long-term project is proposed according to our instruments.
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