Optical CCD photometry and Rosat X-ray spectral analysis of the shortest period CV EI Psc (1RXS J232953.9 + 062814)

We present here the optical observations of EI Psc (1RXS J232953.9 + 062814) through Turkish National Observatory (TUG) with RTT150 cm Russian–Turkish joint telescope and its X-ray observation using the ROSAT archival data. Our optical observations reveal a period of 0.0408 days (58.75 min) which is rather different from its early value of 0.046 days (66.24 min) as reported by [Schmeer, P., 2001. vsnet-alert6830, ]. Also possible periodicities as well as any QPOs are studied without having any clear indication of it. Archival ROSAT RASS data are also analyzed for its X-ray spectra.The raw data were fitted with various spectral models and the best fit models are found to be that of Blackbody and Raymond–Smith with best fit temperatures of kT=(0.07±0.02)keV for blackbody model and kT=(0.13±0.04)keV for Raymond–Smith model while the column density fixed at 0.54×10-21cm-2. The estimated 0.1–2.4 keV flux is found to be in the range of between logF=-13logF=-13 and logF=-14ergcm-2s-1. The model dependent luminosity values were in the range of log L=29ergs-1 for Raymond–Smith model and logL=31ergs-1 for blackbody model. Using the well fitted temperature values, the mass of the primary value that is obtained by [Uemura, M., Kato, T., Ishioka, R., Yamaoka, H., Scgmeer, P., Starkey, D.R., Torii, K., Kawai, N., Urata, Y., Kohama, M., Yoshida, A., Ayani, K., Kawabata, T., Tanabe, K., Matsumoto, K., Kiyota, S., Pietz, J., Vanmunster, T., Krajci, T., Oksanen, A., Giambersio, A., 2002b. Superhump Evolution in the Ultrashort Period Dwarf Nova 1RXS J232953.9 + 062814. PASJ 54, 599–607] and the equations taken from literature, the mass accretion rate in the boundary layer is obtained to be (1.58±0.14)×1021gs-1 for the blackbody model and (2.2±0.052)×1019gs-1 for Raymond–Smith model.As a result of our study it seems that the system EI Psc has a very high mass accretion rate; and because of the observed soft X-ray photons and high mass accretion rates it has an optically thick boundary layer and M-type secondary star which can be a Brown Dwarf.