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<div>Dear Everyone,</div>
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<div>The next EO seminar will take place on the 16th of May. <br>
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<div>See you there.</div>
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<div>- Haakon (on behalf of the organizers)<br>
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<div><b>When/where:</b> 16th of May 13:15 <span>in A5:1003</span><br>
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<div><b>Speaker:</b><span><b> </b>Pia Jakobus</span><span class="_pe_N2 PersonaPaneLauncher" role="presentation"><span class="_pe_l"><span class="bidi allowTextSelection" aria-label="From Pia Jakobus <pia.jakobus@monash.edu>. Press the Enter key to open the contact card."></span></span></span><b>Title:</b>
Proto-Compact Star Convection and the Excitation Mechanism of the Core g-mode<u><br>
</u><b>Abstract:</b> Core-collapse supernovae (CCSNe), the explosion of massive stars, are among the several types of Gravitational Wave (GW) sources yet to be discovered by GW interferometers. In our general-relativistic neutrino hydrodynamics code CoCoNuT-FMT,
we recently identified GWs of a core g-mode residing in the inner regions of the proto-compact star that is sensitive to the Equation of State at multiple times nuclear saturation density. The proto-compact star (PCS) convection zone plays the dominant role
in the excitation mechanism of this mode. In this talk, I will present key properties of the PCS convection zone, and particularly focus on the question of why the core g-mode is absent in our 3D core-collapse supernova simulation whereas it is clearly visible
in 2D. I will also discuss the validity of the mixing-length theory approximation within the PCS convection zone and briefly talk about a possible connection between passive scalars and the lepton-number emission self-sustained asymmetry.</div>
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