TY - JOUR
T1 - A systematic study of proto-neutron star convection in three-dimensional core-collapse supernova simulations
AU - Nagakura, Hiroki
AU - Burrows, Adam
AU - Radice, David
AU - Vartanyan, David
N1 - Publisher Copyright:
© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
PY - 2020
Y1 - 2020
N2 - This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical FORNAX models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, ν¯μ, and ν¯τ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.
AB - This paper presents the first systematic study of proto-neutron star (PNS) convection in three dimensions (3D) based on our latest numerical FORNAX models of core-collapse supernova (CCSN). We confirm that PNS convection commonly occurs, and then quantify the basic physical characteristics of the convection. By virtue of the large number of long-term models, the diversity of PNS convective behaviour emerges. We find that the vigour of PNS convection is not correlated with CCSN dynamics at large radii, but rather with the mass of PNS − heavier masses are associated with stronger PNS convection. We find that PNS convection boosts the luminosities of νμ, ντ, ν¯μ, and ν¯τ neutrinos, while the impact on other species is complex due to a competition of factors. Finally, we assess the consequent impact on CCSN dynamics and the potential for PNS convection to generate pulsar magnetic fields.
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U2 - 10.1093/MNRAS/STAA261
DO - 10.1093/MNRAS/STAA261
M3 - Article
AN - SCOPUS:85084763055
SN - 0035-8711
VL - 492
SP - 5764
EP - 5779
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -