Photometric Observation of Dwarf Nova IP Pegasii Using CAT-ITB Telescope N. F. Nurindra, C. Kunjaya, H. L. Malasan, M. Putra, M. Z. Aprianizar
Institut Teknologi Bandung
Abstract
Cataclysmic binaries are a type of star system in which mass transfer from one star to its companion occurs. One type of cataclysmic binary is dwarf nova. Photometric observations of the dwarf nova IP Pegasii were done to determine the characteristics of the dwarf nova light curve using a small telescope in a city with light pollution. Observations were made using the CAT-ITB telescope at the ITB Astronomy Study Program. The light curve obtained through image processing has a shape and trend similar to the light curve in previous observations but does not clearly show the egress profile of the white dwarf and hotspot. Through comparison of the time of minima between two nights of observation, a period of 3.79200 hours was obtained. There is a difference of \(\sim 4.5\) seconds with the period taken from previous studies. From the calculation of the accretion disk radius, it was found that the accretion disk radius on September 28th 2024 was \( R_{D}/R_1 = 0.76915 \) and on September 30th 2024 was \( R_{D}/R_1 = 0.83609 \). Both values are in the range of \( R_{D}/R_1 \) IP Pegasii taken from previous studies.
