Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism
Our understanding of the core-collapse supernova explosion mechanism is incomplete. While the favoured scenario is delayed revival of the stalled shock by neutrino heating, it is difficult to reliably compute explosion outcomes and energies, which depend sensitively on the complex radiation hydrodynamics of the post-shock region. The dynamics of the (non-)explosion depend sensitively on how energy is transported from inside and near the proto-neutron star (PNS) to material just behind the supernova shock. Although most of the PNS energy is lost in the form of neutrinos, hydrodynamic and hydromagnetic waves can also carry energy from the PNS to the shock. We show that gravity waves excited by core PNS convection can couple with outgoing acoustic waves that present an appreciable source of energy and pressure in the post-shock region. Using one-dimensional simulations, we estimate the gravity wave energy flux excited by PNS convection and the fraction of this energy transmitted upwards to the post-shock region as acoustic waves. We find wave energy fluxes near 10⁵¹ergs⁻¹ are likely to persist for ∼1s post-bounce. The wave pressure on the shock may exceed 10 per cent of the thermal pressure, potentially contributing to shock revival and, subsequently, a successful and energetic explosion. We also discuss how future simulations can better capture the effects of waves, and more accurately quantify wave heating rates.
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2019 November 18. Received 2019 November 15; in original form 2019 October 16. Published: 20 November 2019. We acknowledge helpful discussions with T. Foglizzo, A. Harada, and E. Lentz of great benefit to this work. SEG thanks S. Nissanke, R. Wijers, the GRavitation AstroParticle Physics Amsterdam (GRAPPA) group, and the Anton Pannekoek Institute (API) for their hospitality at Universiteit van Amsterdam (UvA), where much of this work was carried out. This research is funded in part by an Innovator Grant from The Rose Hills Foundation, the Sloan Foundation through grant no. FG-2018-10515, and by the National Science Foundation under grant no. NSF PHY-1748958. Software: All figures presented in this paper were produced using PYTHON, MATPLOTLIB (Hunter 2007), NUMPY (Oliphant 2006; van der Walt, Colbert & Varoquaux 2011), and SCIPY (Jones et al. 2001).
Submitted - 1910.07599.pdf
Published - stz3243.pdf