<div dir="ltr"><div class="gmail_quote"><br><br><div dir="ltr"><div dir="ltr" style="font-size:12.8px"><div dir="ltr"><b style="font-size:12.8px">DATE</b><span style="font-size:12.8px">: <span><span>Friday, September 2nd, 2016</span></span></span><b style="font-size:12.8px"><br><br></b><div style="font-size:12.8px"><b style="font-size:12.8px">TITLE</b><span style="font-size:12.8px">: </span> Quark Deconfinement in Neutron Stars</div><div><br style="font-size:12.8px"><b style="font-size:12.8px">TIME</b><span style="font-size:12.8px">: </span><span style="font-size:12.8px"><span><span>3:30 PM</span></span></span><br style="font-size:12.8px"><br style="font-size:12.8px"><b style="font-size:12.8px">LOCATION</b><span style="font-size:12.8px">: GMCS 324</span><br style="font-size:12.8px"><br style="font-size:12.8px"><b style="font-size:12.8px">SPEAKER</b><span style="font-size:12.8px">: </span>Dr. Fridolin Weber. Professor of Physics at San Diego State University.<br><br style="font-size:12.8px"><b style="font-size:12.8px">ABSTRACT</b><span style="font-size:12.8px">: </span>Neutron stars are the remnants of massive stars that blew apart in supernova explosions. Gravity compresses the matter in the cores of such objects to densities that are several times higher than the densities inside of atomic nuclei. At such enormous densities atoms themselves collapse and neutrons and protons are squeezed so tightly together that their quark contents may be released. In this talk, I will discuss the astrophysical implications of this phase transition for neutron stars, based on numerical state-of-the-art investigations.<br><br></div><div style="font-size:12.8px"><b style="font-size:12.8px">HOST</b><span style="font-size:12.8px">: Dr. </span><span style="font-size:12.8px">Calvin Johnson</span><span style="font-size:12.8px">.</span></div><div><span style="font-size:12.8px"><br></span></div></div></div></div>
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SDSU Computational Science Research Center<br>
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