Envelope Expansion with Core Collapse II. Quasi-Spherical Self-Similar Solutions for an Isothermal Magnetofluid

Abstract

We investigate self-similar magnetohydrodynamic (MHD) processes in an isothermal self-gravitating fluid with a quasi-spherical symmetry and extend the envelope expansion with core collapse (EECC) solutions of Lou & Shen by incorporating a random magnetic field. Stagnation surfaces of EECC solutions that seperate core collapse and envelope expansion propagate at constant speeds either sub-magnetosonically or super-magnetosonically. Crossing the magnetosonic line twice analytically, there exists an infinite number of discrete magnetized EECC and ECCC solutions. In addition to the EECC shock solution which could change the central accretion rate, the magnetic field can also affect the core accretion rate. As the magnetic parameter $\lambda$ increases, the core accretion rate appropriate for the MHD EWCS becomes larger. Under the frozen-in approximation, magnetic fields in the envelope expansion portion would scale as $B\propto r^{-1}$, while in the core collapse portion they would scale as $B\propto r^{-1/2}$. We discuss several astrophysical applications of EECC similarity solutions to the formation process of proto-planetary nebulae connecting the AGB phase and the planetary nebula, to supernova remnants, collapse of magnetized molecular cloud, to $\text{H}\text{II}$ clouds surrounding massive OB stars and to a certain evolution phase of galaxy clusters.

19 pages, 18 figures. accepted for publication in MNRAS

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• Self-Similar Dynamics of a Magnetized Polytropic Gas
• Self-Similar Dynamics of a Relativistically Hot Gas
• Self-Similar Shocks in Polytropic Gas Flows around Star-Forming Regions
• Magnetized massive stars as magnetar progenitors
• Global Collapses and Expansions in Star-Forming Clouds
• An Imaging and Spectral Study of Ten X-Ray Filaments around the Galactic Center
• Dispersal of Gaseous Circumstellar Discs around High-Mass Stars
• General Polytropic Magnetofluid under Self-Gravity: Voids and Shocks
• Collisional interaction limits between dark matters and baryons in `cooling flow' clusters
• Self-Similar Shocks and Winds in Galaxy Clusters
• A Three-Dimensional Magnetohydrodynamic Model of Planetary Nebula Jets, Knots, and Filaments
• Magnetohydrodynamic Model of Equatorial Plasma Torus in Planetary Nebulae
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