John M. Blondin

TL;DR: In this article, the stability of standing, spherical accretion shocks is examined in core-collapse supernovae, star formation, and accreting white dwarfs and neutron stars.

TL;DR: In this article, a 2D hydrodynamics code was proposed to model the dynamics of the wind and shock structure formed by the collision in early-type binary systems, which self-consistently accounts for radiative cooling and represents a significant improvement over previous attempts to model these systems.

TL;DR: In this paper, the authors have carried out one and two-dimensional, two-fluid simulations of the crushing and reexpansion phases of a pulsar wind nebula (PWN) and showed that these phases are subject to Rayleigh-Taylor instabilities that result in the mixing of thermal and nonthermal fluids, and asymmetries in the surrounding interstellar medium give rise to asymmetric in the position of the PWN relative to the pulsar and explosion site.

TL;DR: In this paper, the evolution of a supernova remnant through the transition from an adiabatic Sedov-Taylor blast wave to a radiative pressure-driven snowplow phase is studied using one-and two-dimensional hydrodynamic simulations.

TL;DR: In this paper, the authors performed ab initio neutrino radiation hydrodynamics simulations in three and two spatial dimensions (3D and 2D) of core-collapse supernovae from the same 15 M⊙ progenitor through 440 ms after core bounce.