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<span style="font-family: Aptos Narrow, Aptos_EmbeddedFont, Aptos_MSFontService, sans-serif; font-size: 11pt;">Greetings everyone,</span><span style="font-family: Aptos Narrow, Aptos_EmbeddedFont, Aptos_MSFontService, sans-serif; font-size: 11pt; color: black;"><br>
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Tomorrow, on Monday, </span><span style="color: rgb(0, 0, 0); background-color: white;">April 28</span><span style="color: black;"><sup>th</sup>, 2025 at 1:00PM EDT, we will have a virtual seminar given by
</span><span style="color: rgb(0, 0, 0); background-color: white;">Peter Rau of Columbia University on the following Zoom link:</span><span style="color: black;"> </span></div>
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<a href="https://jlab-org.zoomgov.com/j/1619687042?pwd=nazDiNhmbaexz8eV2eZ5XYH93A7uxa.1" target="_blank" id="OWAcf896fb6-a59b-a12d-0065-4e1b9510fc5e" class="x_OWAAutoLink" title="https://jlab-org.zoomgov.com/j/1619687042?pwd=nazDiNhmbaexz8eV2eZ5XYH93A7uxa.1" rel="noopener noreferrer" style="margin: 0px; text-align: left;" data-linkindex="0" data-olk-copy-source="MessageBody" data-auth="NotApplicable" data-ogsc="">https://jlab-org.zoomgov.com/j/1619687042?pwd=nazDiNhmbaexz8eV2eZ5XYH93A7uxa.1</a></div>
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<span style="background-color: white;">Although it’s not an in-person seminar, you can also join your colleagues for a remote streaming of the seminar in CEBAF Center F326-327.</span></div>
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Please see below for the title and abstract. </div>
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<span style="color: black;"><b><u>Theory Seminar</u></b>:<b> </b></span><span style="color: rgb(0, 0, 0); background-color: white;">April 28</span><span style="color: black;"><sup>th</sup>, 1pm EDT (virtual) </span></div>
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<b><u>Speaker</u></b>: Peter Rau (Columbia University) </div>
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<b><u>Title</u></b>:<b> </b><span style="background-color: white;">Neutron stars under extreme magnetic fields and temperatures
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<span style="font-family: Aptos Narrow, Aptos_EmbeddedFont, Aptos_MSFontService, sans-serif; font-size: 11pt; color: black;"><b><u>Abstract</u></b>:
</span><span style="font-family: Aptos Narrow, Aptos_EmbeddedFont, Aptos_MSFontService, sans-serif; font-size: 11pt; color: black; line-height: 1.284;">In addition to their astrophysical significance as the compact remnants of massive stars, neutron stars are
excellent laboratories for studying extreme physics. I will discuss two aspects of this extreme physics. First, the most strongly-magnetized neutron stars possess magnetic fields which can confine electrons into a small to moderate number of quantized Landau
levels. This can have a dramatic effect on their thermodynamic and transport properties. In a recent paper, we studied magnetic field evolution in neutron star crusts, including for the first time field-dependent de Haas--van Alphen oscillations of magnetization
and magnetic susceptibility. I will explain how this mechanism could help explain why more strongly-magnetized neutron stars are observed to be hotter, which requires physics beyond standard Ohmic dissipation. I will then discuss neutron star stellar oscillation
modes, which provide key insights into stellar composition and the dense matter equation of state. These oscillations are modified at high temperatures typical for newborn neutron stars and binary merger remnants, which violate the usual assumption of chemical
equilibrium used to compute buoyancy-supported g-modes. We show that when weak interactions are consistently included in oscillation mode calculations, g-modes are suppressed above MeV-range temperatures. This could modify the expected gravitational wave spectrum
produced by "warm" neutron stars.</span><span style="font-family: Aptos Narrow, Aptos_EmbeddedFont, Aptos_MSFontService, sans-serif; font-size: 11pt; color: black;"> </span></p>
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See you on Monday. </div>
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Kind regards, </div>
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Joe, Zheng-Yang, Gloria and Adam</div>
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