High-Resolution Simulations of the Interaction Between the Nova/Supernova Ejecta and the Accretion Disk

TL;DR

This study uses high-resolution simulations to explore how nova and supernova ejecta interact with accretion disks, revealing disk destruction, altered ejecta geometry, and instabilities that influence subsequent explosions and contamination levels.

Contribution

It provides the first detailed simulations of ejecta-disk interactions, showing disk destruction and effects on nova cycles and ejecta structure.

Findings

Disks are often destroyed or partially destroyed depending on initial conditions.

Ejecta geometry is altered, reducing contamination of the companion star.

Formation of a cavity in ejecta and development of hydrodynamic instabilities.

Abstract

Many nova and type Ia supernova explosion scenarios involve accretion disks. However, direct numerical simulations of these explosive phenomena have barely addressed the question of the impact of ejecta-disk collision on the midterm evolution of such explosions. This is particularly critical for a better understanding of classical and recurrent novae, where each nova cycle depends on the imprint left by the precedent explosion. In this work, we describe and analyze a set of high-resolution simulations of the ejecta-disk interaction. We show that, depending on the initial configuration of the binary system, the disk is partially or, more often, totally destroyed, which will impact the next nova-explosion cycle. In the case of type Ia supernovae, the much larger kinetic energy carried by the ejecta always provokes complete destruction of the accretion disk. We also discuss the alterations induced in the geometry of the ejecta by the shielding effect of the disk, which has shown to cause reduced contamination of the companion star up to a factor \sim 1.5 - 2 in key nuclei produced during the nova outburst. In the framework of recurrent nova simulations, we report for the first time on the formation of a cavity in the ejecta after its interaction with the disk. We also describe the onset and development of several hydrodynamic instabilities such as Kelvin-Helmholtz and Richtmyer-Meshkov.