Numerical simulations of jet launching and breakout from collapsars

TL;DR

This study uses self-consistent 2.5-D GRMHD simulations to model jet formation and breakout in collapsars, revealing how magnetic fields and progenitor structure influence jet dynamics and gamma-ray burst properties.

Contribution

It presents the first self-consistent simulations from black hole horizon to stellar surface, incorporating accretion dynamics and magnetic field effects in collapsar jet formation.

Findings

Jets are launched by strong dipolar magnetic fields from magnetically arrested disks.

Breakout times range from 1.8 to 3.5 seconds, with luminosities up to 7×10^{52} erg/s.

Initial magnetic field strength and progenitor density distribution critically affect jet structure and evolution.

Abstract

Long Gamma-Ray Bursts (LGRBs) are often associated with the collapse of stripped-envelope massive stars. Powerful relativistic jets drill through the stellar envelope before the gamma emission. Previous hydrodynamical studies imposed jets artificially, neglecting accretion dynamics, while the central engine simulations have reproduced jet launching via the Blandford-Znajek mechanism focusing on the inner core regions. However, both the central engine and the progenitor structure are crucial to determining the jet's evolution. In this study, we present axisymmetric (2.5-D) GRMHD simulations that self-consistently follow jet formation from the black-hole horizon to breakout at the stellar surface ($R_\star \sim 10^{10}$~cm). The setup assumes a Kerr black hole with spin $a \sim 0.9$ in the centre of three progenitor models, varying the magnetic-field strength and geometry. Relativistic jets are successfully launched by a strong dipolar magnetic field ($B_0 \gtrsim 10^{12}$-$10^{14}$~G) from magnetically arrested disks. These jets, initially magnetically dominated, convert energy into thermal and kinetic during their propagation. We found breakout times within $1.8 \lesssim t_{\rm bo} \lesssim 3.5$~s and luminosities $L_j \sim 5\times10^{49}-7\times10^{52}$~erg\,s$^{-1}$. Our results highlight the role of the initial magnetic field strength and its geometry, emphasizing the progenitor's density distribution as a key factor impacting the final structure and dynamics of LGRB jets.