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<p>Reminder: Eric's talk will be in ~2 hours.<br>
</p>
<div class="moz-cite-prefix">On 2/21/25 7:02 PM, Pooyan Goodarzi
wrote:<br>
</div>
<blockquote type="cite"
cite="mid:CAN7Yd1JV3mtdT768_MTHz9kPQrfnQ1cK7hZCzkxw+8OasnqzUg@mail.gmail.com">
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<p>Hi all, <br>
<br>
We will have a <span class="gmail-il">PASS</span> <span
class="gmail-il">talk</span> next Monday. Please join us
at noon (from 12:00 pm to 1:00 pm) in the Nebula Room (PHYS
3027).<br>
<br>
<br>
</p>
<div align="center"><b>Eric Zhang, PhD student</b><br>
Monday, 12:00 pm, Nebula Room (PHYS 3027)<br>
<b><span>Implementing Supernova Feedback in Galaxy Formation
Simulations</span><span>: Sensitivity to Numerical Choices</span></b><br>
<br>
<br>
<div>
<div id="gmail-message-content-1342236415475318815"
class="gmail-markup__75297 gmail-messageContent_c19a55"><span>Simulations
of galaxy formation are mostly unable to resolve the
energy</span><span>-conserving phase of individual
supernova events</span><span>, having to resort to
subgrid models to distribute the energy and momentum
resulting from stellar feedback</span><span>. However</span><span>,
the properties of these simulated galaxies</span><span>,
including the morphology</span><span>, stellar mass
formed and the burstiness of the star formation history</span><span>,
are highly sensitive to numerical choices adopted in
these subgrid models</span><span>. Using the SMUGGLE
stellar feedback model</span><span>, we carry out
idealized simulations of a 𝑀vir ∼ 1010 M⊙ dwarf galaxy</span><span>,
a regime where most simulation codes predict significant
burstiness in star formation</span><span>, resulting in
strong gas flows that lead to the formation of dark
matter cores</span><span>. We find that by varying only
the directional distribution of momentum imparted from
supernovae to the surrounding gas</span><span>, while
holding the total momentum per supernova constant</span><span>,
bursty star formation may be amplified or completely
suppressed</span><span>, and the total stellar mass
formed can vary by as much as a factor of ∼ </span><span>3</span><span>.
In particular</span><span>, when momentum is primarily
directed perpendicular to the gas disk</span><span>,
less bursty and lower overall star formation rates
result</span><span>, yielding less gas turbulence</span><span>,
more disky morphologies and a retention of cuspy dark
matter density profiles</span><span>. An improved
understanding of the non</span><span>-linear coupling of
stellar feedback into inhomogeneous gaseous media is
thus needed to make robust predictions for stellar
morphologies and dark matter core formation in dwarfs
independent of uncertain numerical choices in the
baryonic treatment</span><span>.</span></div>
</div>
</div>
<br>
<br>
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>].<br>
<div><br>
</div>
<div><br>
</div>
Best,<br>
Pooyan<br>
Physics and Astronomy Student Seminar (<span class="gmail-il">PASS</span>)
<br>
<a href="https://ucrpass.arxiv.social/" target="_blank"
moz-do-not-send="true" class="moz-txt-link-freetext">https://ucrpass.arxiv.social</a></div>
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