Outflows and inflows in astrophysical systems

Abstract

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.

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

References in corpus (4)

• Self-similar Collapse of Rotating Magnetic Molecular Cloud Cores
• Self-similar champagne flows in HII regions
• Envelope Expansion with Core Collapse. I. Spherical Isothermal Similarity Solutions
• Shocked similarity collapses and flows in star formation processes

Cited by in corpus (1)

• Spherical Isothermal Self-Similar Shock Flows