Magnetically-dominated jets inside collapsing stars as a model for gamma-ray bursts and supernova explosions

TL;DR

This paper models magnetar-driven, magnetically-dominated jets inside collapsing stars, proposing a mechanism for gamma-ray bursts and supernova explosions through magnetic pressure overcoming infalling matter, leading to collimated jets.

Contribution

It introduces the 'Pulsar-in-a-Cavity' paradigm for magnetar interactions within collapsing stars and outlines a plasma physics framework for jet formation in GRB scenarios.

Findings

Magnetic pressure can dominate over ram pressure, driving explosions.

Jets are collimated into narrow, magnetic-tower structures.

Delayed jet formation explains Nickel-56 production in supernovae.

Abstract

It has been suggested that magnetic fields play a dynamically-important role in core-collapse explosions of massive stars. In particular, they may be important in the collapsar scenario for gamma-ray bursts (GRB), where the central engine is a hyper-accreting black hole or a millisecond magnetar. The present paper is focussed on the magnetar scenario, with a specific emphasis on the interaction of the magnetar magnetosphere with the infalling stellar envelope. First, the ``Pulsar-in-a-Cavity'' problem is introduced as a paradigm for a magnetar inside a collapsing star. The basic set-up of this fundamental plasma-physics problem is described, outlining its main features, and simple estimates are derived for the evolution of the magnetic field. In the context of a collapsing star, it is proposed that, at first, the ram pressure of the infalling plasma acts to confine the magnetosphere, enabling a gradual build-up of the magnetic pressure. At some point, the growing magnetic pressure overtakes the (decreasing) ram pressure of the gas, resulting in a magnetically-driven explosion. The explosion should be highly anisotropic, as the hoop-stress of the toroidal field, confined by the surrounding stellar matter, collimates the magnetically-dominated outflow into two beamed magnetic-tower jets. This creates a clean narrow channel for the escape of energy from the central engine through the star, as required for GRBs. In addition, the delayed onset of the collimated-explosion phase can explain the production of large quantities of Nickel-56, as suggested by the GRB-Supernova connection. Finally, the prospects for numerical simulations of this scenario are discussed.