Abstract
The seasonal behavior of the light curve for selected star SS UMI and EXDRA during outburst cycle is studied. This behavior describes maximum temperature of outburst in dwarf nova. The raw data has been mathematically modeled by fitting Gaussian function based on the full width of the half maximum and the maximum value of the Gaussian. The results of this modeling describe the value of temperature of the dwarf novae star system leading to identify the type of elements that each dwarf nova consisted of.
Highlights
Cataclysmic variables are binary stars in which a relatively normal star is transferring mass to its compact by orbiting so close to each other's [1]
There are two models describe the outburst in dwarf nova systems; A. mass transfer burst a sudden increase in the transfer of material from the companion star to the accretion disk causes the disk to collapse
Disk instability model (DIM): the cause of outburst are strongly depend on the instability that taking place in the accretion disk
Summary
Cataclysmic variables are binary stars in which a relatively normal star is transferring mass to its compact by orbiting so close to each other's [1]. The gas from secondary stars flows following magnetic field and or gravity field and falls on the white dwarf [2] This material flow creates an accretion disk around the white dwarf star and from times to times, nuclear reaction starts and the system show an increase in brightness, this phenomenon called an outburst. There are two models describe the outburst in dwarf nova systems; A. mass transfer burst a sudden increase in the transfer of material from the companion star to the accretion disk causes the disk to collapse. Disk instability model (DIM): the cause of outburst are strongly depend on the instability that taking place in the accretion disk This because the material is transferred from the secondary star at a constant rate. The system turned out to be a double-eclipsing dwarf nova of the UGem class with a quiescence magnitude of about 14m, relatively small outburst amplitude of 1m–2.3m and an orbital period of 5.04 h [6]
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