The Effects of Metallicity and Abundance Pattern of the ISM on Supernova Feedback. (arXiv:2004.10974v3 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Karpov_P/0/1/0/all/0/1">Platon I. Karpov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martizzi_D/0/1/0/all/0/1">Davide Martizzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Macias_P/0/1/0/all/0/1">Phillip Macias</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ramirez_Ruiz_E/0/1/0/all/0/1">Enrico Ramirez-Ruiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kolborg_A/0/1/0/all/0/1">Anne N. Kolborg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naiman_J/0/1/0/all/0/1">Jill P. Naiman</a>
Supernova (SN) feedback plays a vital role in the evolution of galaxies.
While modern cosmological simulations capture the leading structures within
galaxies, they struggle to provide sufficient resolution to study small-scale
stellar feedback, such as the detailed evolution of SN remnants. It is thus
common practice to assume subgrid models that are rarely extended to low
metallicities, and which routinely use the standard solar abundance pattern.
With the aid of 1-d hydrodynamical simulations, we extend these models to
consider low metallicities and non-solar abundance patterns as derived from
spectra of Milky Way stars. For that purpose, a simple, yet effective framework
has been developed to generate non-solar abundance pattern cooling functions.
We find that previous treatments markedly over-predict SN feedback at low
metallicities and show that non-negligible changes in the evolution of SN
remnants of up to $approx 50%$ in $cooling; mass$ and $approx 27%$ in
$momentum; injection; from; SN; remnants$ arise from non-solar abundance
patterns. We use our simulations to quantify these results as a function of
metallicity and abundance pattern variations and present analytic formulae to
accurately describe the trends. These formulae have been designed to serve as
subgrid models for SN feedback in cosmological hydrodynamical simulations.
Supernova (SN) feedback plays a vital role in the evolution of galaxies.
While modern cosmological simulations capture the leading structures within
galaxies, they struggle to provide sufficient resolution to study small-scale
stellar feedback, such as the detailed evolution of SN remnants. It is thus
common practice to assume subgrid models that are rarely extended to low
metallicities, and which routinely use the standard solar abundance pattern.
With the aid of 1-d hydrodynamical simulations, we extend these models to
consider low metallicities and non-solar abundance patterns as derived from
spectra of Milky Way stars. For that purpose, a simple, yet effective framework
has been developed to generate non-solar abundance pattern cooling functions.
We find that previous treatments markedly over-predict SN feedback at low
metallicities and show that non-negligible changes in the evolution of SN
remnants of up to $approx 50%$ in $cooling; mass$ and $approx 27%$ in
$momentum; injection; from; SN; remnants$ arise from non-solar abundance
patterns. We use our simulations to quantify these results as a function of
metallicity and abundance pattern variations and present analytic formulae to
accurately describe the trends. These formulae have been designed to serve as
subgrid models for SN feedback in cosmological hydrodynamical simulations.
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