Outflows and inflows in astrophysical systems

Details Outflows and inflows in astrophysical systems Outflows and inflows in astrophysical systems

2004-10-03

arxiv.org/abs/astro-ph/0410051v1

Chin.J.Astron.Astrophys. S5 (2005) 241-246

Astronomy and Astrophysics

Astrophysics

ChJAA accepted; contribution to the proceedings of the 5th microquasar workshop

Scientific paper

We seek for self-similar solutions describing the time-dependent evolution of self-gravity systems with either spherical symmetry or axisymmetric disk geometry. By assuming self-similar variable $x\equiv r/at$ where $a$ is isothermal sound speed we find self-similar solutions extending from the initial instant $t=0$ to the final stage $t\to \infty$ using standard semi-analytical methods. Different types of solutions are constructed, which describe overall expansion or collapse, envelope expansion with core collapse (EECC), the formation of central rotationally supported quasi-equilibrium disk as well as shocks. Though infinitely many, these self-similarity solutions have similar asymptotic behaviors which may impose diagnosis on the velocity and density structures in astrophysical systems.

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