Observations of Interacting Binaries
Presenter : Stephen
Suggested Starting Points
Taam & Sanquist, Sect. 5.4
Kahabka & van den Heuvel
Computational Studies
John Blondin's simulations of interacting binary stars
Colliding winds in binary systems by Rolf Walder and Doris Follini, ETHZ
Nice movie from the simulation series above
Assigned Reading
Discussion
What are the characteristics of Super-Soft X-ray Sources (SSS)? They are white dwarfs, with energies range from .09 to 2.5 KeV.
How common are SS X-ray Sources? ~1000 in galaxies like our own.
What type of secondary star will be present in binary systems containing SSS's?
What does Figure 5 (p. 79) tell us? What are some problems brought up by it? The problem is the very narrow range of accretion rates that can lead to steady accretion as opposed to cataclysmic variables. This limits the number of binary pairs that might lead to SSS and SN1As.
How do SSS's fit in as SN 1A progenitors? They end their stellar evolution by either becoming a neutron star or becoming a SN 1A. There's a good chance they may end up accounting for a significant amount of SN 1As in both spiral and irregular galaxies.