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<p>Reminder: happening in ~2 hours.</p>
<div class="moz-cite-prefix">On 10/16/25 12:02 PM, Pooyan Goodarzi
wrote:<br>
</div>
<blockquote type="cite"
cite="mid:4dfc3bbc-098b-49ec-ad4f-211af4237488@email.ucr.edu">
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<p>Hi all,</p>
<p><br>
</p>
<p>We will have a PASS talk by Eric next <b>Monday</b>, October
20, at noon. Please join us at noon (<b>from 12:00 to 1:00 pm</b>)
in the Nebula Room (PHYS 3027). </p>
<p><br>
</p>
<p align="center"><b>Eric Zhang, PhD Student</b><br>
Monday, 12:00 pm, Nebula Room (PHYS 3027)</p>
<p align="center"><b>The Entangled Feedback Impacts of Supernovae
in Coarse- versus High-Resolution Galaxy Simulations</b></p>
<p align="center"><b><br>
</b></p>
<p align="center">It is often understood that supernova (SN)
feedback in galaxies is responsible for regulating star
formation and generating gaseous outflows. However, a detailed
look at their effect on the local interstellar medium (ISM) on
small mass scales in simulations shows that these processes
proceed in clearly distinct channels. We demonstrate this
finding in two independent simulations with solar-mass
resolution, LYRA and RIGEL, of an isolated dwarf galaxy.
Focusing on the immediate environment surrounding SNe, our
findings suggest that the large-scale effect of a given SN on
the galaxy is best predicted by its immediate local density.
Outflows are driven by SNe in diffuse regions expanding to their
cooling radii on large (∼ kpc) scales, while dense star-forming
regions are disrupted in a localized (∼ pc) manner. However,
these separate feedback channels are only distinguishable at
very high numerical resolutions capable of following scales ≪
10^3 M⊙. On larger scales, ISM densities are greatly
mis-estimated, and differences between local environments of SNe
become severely washed out. We demonstrate the practical
implications of this effect by comparing with a mid-resolution
simulation (𝑀ptcl. ∼ 200 M⊙) of the same dwarf using the
SMUGGLE model. The coarse-resolution simulation cannot
self-consistently determine whether a given SN is responsible
for generating outflows or suppressing star formation,
suggesting that emergent galaxy physics such as star formation
regulation through hot-phase outflows is fundamentally
unresolvable by subgrid stellar feedback models, without
appealing directly to simulations with highly resolved ISM.</p>
<p align="center"><br>
</p>
<div
id="m_-7314571423100097885m_-3414541767872711075m_9215603032040371864m_-1672972118947443868gmail-:1f4">
<div>
<div dir="ltr"><br>
</div>
<div dir="ltr">If you’re interested in sharing your work as a
speaker, please feel free to add your name to this
spreadsheet [<a
href="https://docs.google.com/spreadsheets/d/1N3ncf43jdB6aHYHhyWmyHMycxDg4_phHZXLkQvviO0o/edit?usp=sharing"
target="_blank" moz-do-not-send="true">Google Sheet</a>].
Recordings of all the previous talks are available on our
website: <a href="https://ucrpass.arxiv.social/"
target="_blank" class="moz-txt-link-freetext"
moz-do-not-send="true">https://ucrpass.arxiv.social</a>
<div><br>
</div>
<div><br>
</div>
Best,<br>
Pooyan<br>
Physics and Astronomy Student Seminar (<span><span>PASS</span></span>)
<br>
<a href="https://ucrpass.arxiv.social/" target="_blank"
class="moz-txt-link-freetext" moz-do-not-send="true">https://ucrpass.arxiv.social</a></div>
</div>
</div>
<div><br>
<br>
</div>
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</p>
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