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<p>Dear everyone,</p>
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<p>The next EO meeting will take place in the MEGA room on the 24th of November.</p>
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<div><font color="black">Looking forward to see you all next week!</font></div>
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<div><font color="black">Kind regards, </font></div>
<div><font color="black">Ana Sagués Carracedo & Haakon Andresen</font></div>
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<p><b>When: 27th of November, </b><b>13:15</b><b><br>
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<p><b>Where: MEGA</b></p>
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<p><b>Speaker: <span>Rodrigo Fernandez </span></b></p>
<div><b>Title: Mass ejection in non-rotating failed supernovae<br>
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<div><b>Abstract:</b><br>
The core-collapse of a slowly-rotating massive star that fails to explode results in the formation of a black hole (BH). Below the pair-instability threshold, a protoneutron star phase always precedes BH formation, with a corresponding reduction in the total
gravitational mass due to neutrino emission. The ensuing deviation from hydrostatic equilibrium in the outer layers of the star results in the ejection of a small amount of mass with much lower energies than in successful supernovae. The mass and velocity
of the ejecta depend on properties of the core and envelope of the progenitor. I'll discuss an exploration of this mechanism over a wide range of stellar progenitors using spherically-symmetric hydrodynamic simulations, focusing on the effect of the dense-matter
equation of state and spatial resolution on the ejecta properties, expected electromagnetic counterparts, and upper limits to the mass of the BH remnant.</div>
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