Applying the Jet Feedback Mechanism to Core-Collapse Supernova Explosions

Abstract

I examine a mechanism by which two fast narrow jets launched by a newly formed neutron star (NS), or a black hole (BH), at the center of a core collapse supernovae (CCSN), form two slow massive wide (SMW) jets. Such SMW jets are assumed as initial conditions in some numerical simulations that demonstrate that SMW jets can expel the rest of the collapsing star. The original fast narrow jets must deposit their energy inside the star via shock waves, and form two hot bubbles that accelerate a much larger mass to form SMW jets. To prevent the jets from penetrating through the still infalling gas and escape instead of forming the hot bubbles, the jets should encounter fresh infalling gas. This condition is met if the jets' axis changes its direction. The exact condition is derived. In addition, to maintain a small neutrino cooling the fast narrow jets must be shocked at a distance r>1000 km from the core, such that most of the post-shock energy is in radiation, and temperature is not too high. The scenario proposed here was shown to be able to suppress star formation in newly formed galaxies, and in forming SMW jets in cooling flow clusters of galaxies and in planetary nebulae. Namely, I suggest that NSs (or BHs) at the center of CCSNs shut off their own growth and expel the rest of the mass available for accretion by the same mechanism that super-massive BHs shut off their own growth, as well as that of their host bulge, in young galaxies.

Accepted by MNRAS

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