Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987jass....4...11n&link_type=abstract
Journal of Astronomy and Space Science, vol. 4, no. 1, p. 11-23.
Astronomy and Astrophysics
Astronomy
Scientific paper
In dward nova we assume the primary star as a white dwarf and the secondary as the late type star which filled Roche lobe. Mass flow from the secondary star leads to the formation of thin accretion disk around the white dwarf. We use the ¥á parameter as viscosity to maintain the disk form and propose that the outburst in dwarf nova cause the steep increase of source term. With these assumptions we solve the basic equations of stellar structure using Newton-Raphson method. We show the physical parameters like temperature, density, pressure, opacity, surface density, height and flux to the radius of disk. Changing the value of ¥á, we compare several parameters when mass flow rate is constant with those of when luminosity of disk is brightest. At the same time, we obtain time-dependent variations of luminosity and mass of disk. We propose the suitable range of ¥á is 0.15-0.18 to the difference of luminosity. We compare several parameters of disk with those of the normal late type stars which have the same molecular weight of disk is lower. Maybe the outburst in dwarf nova is due to the variation of the ¥á value instead of increment of mass flow from the secondary star.
Choi Kyu-Hong
Kim Kyung-Mee
Na Hye-Weon
No associations
LandOfFree
Time-Dependent Variations of Accretion Disk does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Time-Dependent Variations of Accretion Disk, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Time-Dependent Variations of Accretion Disk will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1818055