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<div><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Dear colleagues,
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<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the next EO meeting will take place this Thursday Nov 21</span><br>
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<p><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">at 13:15 in the KTH meeting room on the 5th floor of the
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<div><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Speaker: Giovanni Camelio</span><br>
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<p><font size="2"><span style="font-size:10pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Title:
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<p><font size="2"><span style="font-size:10pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;"></span><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Rotating neutron stars with non-barotropic thermal
profile</span><br>
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<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Abstract:</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Being able to determine the stationary structure of a neutron star allows to</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">study its properties, like the parameter space of the equation of state, the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">mass-radius diagram, and the gravitational wave emission.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Moreover, this stationary configuration can be used as initial condition for a</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">much more resource demanding hydrodynamical simulation.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">A key approximation made for computing the stationary structure of hot and</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">rotating neutron stars is that of barotropicity, namely that all thermodynamical</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">quantities are in a one-to-one relationship, which in turn implies that the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">specific angular momentum of a fluid element is in a one-to-one relationship with</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">its angular velocity.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">However, this is a poor approximation for the compact remnant of a core-collapse</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">supernova or of a binary neutron star merger.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">In this talk I describe how, for the first time, we determine the structure of</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">stationary, hot, rotating neutron stars without the barotropic approximation.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">To do so, we introduce a potential formulation for the Euler equation, which is</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">a novel technique even in the context of Newtonian stars.</span><br>
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<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Coauthors:</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Tim Dietrich, Miguel Marques, Stephan Rosswog</span></span></font><br>
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<p><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">See you there!</span><br>
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<p style="font-size:16px; font-family:Calibri,Helvetica,sans-serif">---------------------------------</p>
<p style="font-size:16px; font-family:Calibri,Helvetica,sans-serif">André da Silva Schneider<br>
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<p style="font-size:16px; font-family:Calibri,Helvetica,sans-serif"><span style="font-size:10pt; font-family:Calibri,Helvetica,sans-serif,serif,EmojiFont">Department of Astronomy</span><br>
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<p style="font-size:16px; font-family:Calibri,Helvetica,sans-serif"><span style="font-family:Calibri,Helvetica,sans-serif,serif,EmojiFont"><span style="font-size:10pt">Stockholm University</span></span></p>
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