Towards an understanding of the resolution dependence of Core-Collapse Supernova simulations. Issue 4 (3rd October 2019)

• Record Type: Journal Article
• Authors: Nagakura, Hiroki; Burrows, Adam; Radice, David; Vartanyan, David
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 490:Issue 4(2019)
• Page Start: 4622
• Page End: 4637
• Publication Date: 2019-10-03
• Subjects: supernovae: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stz2730
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Using our new state-of-the-art core-collapse supernova (CCSN) code Fornax, we explore the dependence upon spatial resolution of the outcome and character of three-dimensional (3D) supernova simulations. For the same 19 M⊙ progenitor star, energy and radial binning, neutrino microphysics, and nuclear equation of state, changing only the number of angular bins in the θ and ϕ directions, we witness that our lowest resolution 3D simulation does not explode. However, when jumping progressively up in resolution by factors of two in each angular direction on our spherical-polar grid, models then explode, and explode slightly more vigorously with increasing resolution. This suggests that there can be a qualitative dependence of the outcome of 3D CCSN simulations upon spatial resolution. The critical aspect of higher spatial resolution is the adequate capturing of the physics of neutrino-driven turbulence, in particular its Reynolds stress. The greater numerical viscosity of lower resolution simulations results in greater drag on the turbulent eddies that embody turbulent stress, and, hence, in a diminution of their vigor. Turbulent stress not only pushes the temporarily stalled shock further out, but bootstraps a concomitant increase in the deposited neutrino power. Both effects together lie at the core of the resolution dependence we observe.