We report results from a convection dynamo simulation of proto-neutron star
(PNS), with a nuclear equation of state (EOS) and the initial hydrodynamic
profile taken from a neutrino radiation-hydrodynamics simulation of a massive
stellar core-collapse. A moderately-rotating PNS with the spin period of $170$
ms in the lepton-driven convection stage is focused. We find that large-scale
flow and thermodynamic fields with north-south asymmetry develop in the
turbulent flow, as a consequence of the convection in the central part of the
PNS, which we call as a "deep core convection". Intriguingly, even with such a
moderate rotation, large-scale, $10^15$ G, magnetic field with dipole
symmetry is spontaneously built up in the PNS. The turbulent electro-motive
force arising from rotationally-constrained core convection is shown to play a
key role in the large-scale dynamo. The large-scale structures organized in the
PNS may impact the explosion dynamics of supernovae and subsequent evolution to
the neutron stars.
Description
Deep Core Convection and Dynamo in Newly-born Neutron Star
%0 Generic
%1 masada2020convection
%A Masada, Youhei
%A Takiwaki, Tomoya
%A Kotake, Kei
%D 2020
%K dynamo neutron star
%T Deep Core Convection and Dynamo in Newly-born Neutron Star
%U http://arxiv.org/abs/2001.08452
%X We report results from a convection dynamo simulation of proto-neutron star
(PNS), with a nuclear equation of state (EOS) and the initial hydrodynamic
profile taken from a neutrino radiation-hydrodynamics simulation of a massive
stellar core-collapse. A moderately-rotating PNS with the spin period of $170$
ms in the lepton-driven convection stage is focused. We find that large-scale
flow and thermodynamic fields with north-south asymmetry develop in the
turbulent flow, as a consequence of the convection in the central part of the
PNS, which we call as a "deep core convection". Intriguingly, even with such a
moderate rotation, large-scale, $10^15$ G, magnetic field with dipole
symmetry is spontaneously built up in the PNS. The turbulent electro-motive
force arising from rotationally-constrained core convection is shown to play a
key role in the large-scale dynamo. The large-scale structures organized in the
PNS may impact the explosion dynamics of supernovae and subsequent evolution to
the neutron stars.
@misc{masada2020convection,
abstract = {We report results from a convection dynamo simulation of proto-neutron star
(PNS), with a nuclear equation of state (EOS) and the initial hydrodynamic
profile taken from a neutrino radiation-hydrodynamics simulation of a massive
stellar core-collapse. A moderately-rotating PNS with the spin period of $170$
ms in the lepton-driven convection stage is focused. We find that large-scale
flow and thermodynamic fields with north-south asymmetry develop in the
turbulent flow, as a consequence of the convection in the central part of the
PNS, which we call as a "deep core convection". Intriguingly, even with such a
moderate rotation, large-scale, $10^{15}$ G, magnetic field with dipole
symmetry is spontaneously built up in the PNS. The turbulent electro-motive
force arising from rotationally-constrained core convection is shown to play a
key role in the large-scale dynamo. The large-scale structures organized in the
PNS may impact the explosion dynamics of supernovae and subsequent evolution to
the neutron stars.},
added-at = {2020-01-25T07:54:05.000+0100},
author = {Masada, Youhei and Takiwaki, Tomoya and Kotake, Kei},
biburl = {https://www.bibsonomy.org/bibtex/2473c4dac7416d12226ba630e9dfa090d/ericblackman},
description = {Deep Core Convection and Dynamo in Newly-born Neutron Star},
interhash = {009a9cde175becf1f4ccae6a0d3acb89},
intrahash = {473c4dac7416d12226ba630e9dfa090d},
keywords = {dynamo neutron star},
note = {cite arxiv:2001.08452Comment: 7 pages, 5 figures, submitted to ApJL},
timestamp = {2020-01-25T07:54:05.000+0100},
title = {Deep Core Convection and Dynamo in Newly-born Neutron Star},
url = {http://arxiv.org/abs/2001.08452},
year = 2020
}