temporal and spatial components. Finally, we verify the applicability of these principles on the general relativistic, radiation-hydrodynamic simulations of Müller, Janka, & Heger (2012), and discuss implications for the three-dimensional case.'
author:
- |
    Rodrigo Fernández$^{1,2,3}$, Bernhard Müller$^4$, Thierry Foglizzo$^5$, Hans-Thomas Janka$^4$\
    $^1$ Institute for Advanced Study, Princeton, NJ 08540, USA\
    $^2$ Department of Physics, University of California, Berkeley, CA 94720, USA\
    $^3$ Department of Astronomy & Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA\
    $^4$ Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany\
    $^5$ Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d’Astrophysique, CEA-Saclay F-91191, France
bibliography:
- 'ccsne.bib'
- 'apj-jour.bib'
date: Submitted to MNRAS
title: 'Characterizing SASI- and Convection-Dominated Core-Collapse Supernova Explosions in Two Dimensions'
---

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hydrodynamics — instabilities – neutrinos – nuclear reactions, nucleosynthesis, abundances — shock waves – supernovae: general

Introduction
============

In the neutrino mechanism of core-collapse supernovae, a small fraction of the energy emitted in neutrinos by the forming neutron star is deposited in a layer behind the stalled accretion shock, powering its final expansion [@bethe85]. Extensive theoretical work over the last two decades has led to a consensus on the failure of this mechanism in spherically symmetric systems, except for the very 