<html>
<head>
<meta http-equiv="Content-Type" content="text/html; charset=iso-8859-1">
<style type="text/css" style="display:none;"><!-- P {margin-top:0;margin-bottom:0;} --></style>
</head>
<body dir="ltr">
<style type="text/css" style="display:none;"><!-- P {margin-top:0;margin-bottom:0;} --></style>
<div id="divtagdefaultwrapper" style="font-size:12pt;color:#000000;font-family:Calibri,Helvetica,sans-serif;" dir="ltr">
<p>Reminder of today's meeting. We meet in FC61 at 13:15.</p>
<p><br>
</p>
<p>Best,<br>
Haakon<br>
</p>
</div>
<hr style="display:inline-block;width:98%" tabindex="-1">
<div id="divRplyFwdMsg" dir="ltr"><font face="Calibri, sans-serif" style="font-size:11pt" color="#000000"><b>From:</b> Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se-bounces@lists.su.se> on behalf of Haakon Andresen via Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se@lists.su.se><br>
<b>Sent:</b> 20 May 2024 11:27:46<br>
<b>To:</b> EO meeting email<br>
<b>Subject:</b> [Okc-wp4] EO meeting on the 23rd of May</font>
<div> </div>
</div>
<div>
<div id="divtagdefaultwrapper" dir="ltr" style="font-size: 12pt; color: rgb(0, 0, 0); font-family: Calibri, Helvetica, sans-serif, "EmojiFont", "Apple Color Emoji", "Segoe UI Emoji", NotoColorEmoji, "Segoe UI Symbol", "Android Emoji", EmojiSymbols;">
<p></p>
<div>Dear everyone,<br>
<br>
On Thursday Finia Jost, who is visiting from TU Darmstadt, will present on <span>
core-collapse supernova</span></div>
<div>and the chemical evolution of galaxies. We will meet in FC61, instead of our normal room.<br>
<br>
Look forward to seeing you all there.<br>
<br>
Best,<br>
Haakon (on behalf of the organisers)<br>
<br>
<br>
When: 13:15, Thursday 23rd of May<br>
Where: FC61 (Astronomy department)<br>
<br>
<span class="c-mrkdwn__br"></span><b>Speaker: Finia Jost </b>(TU Darmstadt)<br>
<b>Title:</b> Core-collapse Supernova Yields for Galactic Chemical Evolution<br>
<b>Abstract: </b>The amount and composition of matter ejected in core-collapse supernovae (CCSNe) are key uncertainties in models of galactic chemical evolution (GCE). Extensive grids of stellar models with varying mass and metallicity are needed. Although
3D simulations of stellar evolution and CCSNe have recently become available, the large computational cost only allows large sets of simulations under the assumption of spherical symmetry. In this study, we simulate the collapse and explosion of 63 massive
stars with zero-age main sequence masses between 11 and 75 solar masses and three different metallicities. Our CCSN simulations include a self-consistent treatment of the proto-neutron star with a naturally evolving mass cut between remnant and ejecta. We
provide nucleosynthesis results from an in-situ nuclear reaction network and use them as input for a GCE model of the Milky Way. This self-consistent chain allows for the exploration of uncertainties and comparison of the results to observations. With this
study, we want to encourage the communities of stellar evolution and supernova simulations to use the latest advances in the respective fields to provide information useful for GCE models.<br>
<br>
<br>
<div>Join Zoom Meeting<br>
https://stockholmuniversity.zoom.us/j/3575421837<br>
Meeting ID: 357 542 1837</div>
<br>
</div>
<br>
<p></p>
</div>
</div>
</body>
</html>