Philipp Podsiadlowski

Abstract:

Irradiation of the secondaries in close binary systems affects their appearance and can drastically change their internal structure and hence long-term evolution. We have developed a three-dimensional fluid dynamics code for modelling these effects. We give particular emphasis to the role of circulation driven by the external heating and the radiative surface stress. We present results of self-consistent calculations for the circulation in irradiated systems and show how the inclusion of these is vital to the understanding and interpretation of any system where external irradiation of the secondary is significant.

Abstract:

Ultraluminous X-ray sources (ULXs) with L-x > 10(39) ergs s(-1) have been discovered in great numbers in external galaxies with ROSAT, Chandra, and XMM-Newton. The central question regarding this important class of sources is whether they represent an extension in the luminosity function of binary X-ray sources containing neutron stars and stellar-mass black holes (BHs), or a new class of objects, e.g., systems containing intermediate-mass black holes (100-1000 M-circle dot), We have carried out a theoretical study to test whether a large fraction of the ULXs, especially those in galaxies with recent star formation activity, can be explained with binary systems containing stellar-mass black holes. To this end, we have applied a unique set of binary evolution models for black-hole X-ray binaries, coupled to a binary population synthesis code, to model the ULXs observed in external galaxies. We find that for donor stars with initial masses > 10 Me the mass transfer driven by the normal nuclear evolution of the donor star is sufficient to potentially power most ULXs. This is the case during core hydrogen burning and, to an even more pronounced degree, while the donor star ascends the giant branch, though the latter phases last only 5% of the main sequence phase. We show that with only a modest violation of the Eddington limit, e,g., a factor of similar to 10, both the numbers and properties of the majority of the ULXs can be reproduced.

Abstract:

We derive a two-streams formalism for convective motions that guarantees self-consistency for chemistry and energy budget. We apply this formalism to convective Urca cores in massive white dwarfs. We stress that in degenerate matter, nuclear reactions that change the number of electrons strongly influence the convective velocities. We point out the sensitivity of the energy budget on the mixing. We illustrate our model by computing stationary convective cores with Urca nuclei. We show that even a very small mass fraction of Urca nuclei (namely 10(-8)) strongly influences the convective velocities. Finally, we present preliminary computations of the late evolution of a close to Chandrasekhar mass C+O white dwarf including the convective Urca process.