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<p>Reminder of the EO meeting this afternoon!<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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<div id="divRplyFwdMsg" dir="ltr"><font face="Calibri, sans-serif" style="font-size:11pt" color="#000000"><b>From:</b> Okc-wp4-at-fysik.su.se <okc-wp4-at-fysik.su.se-bounces@lists.su.se> on behalf of Andre Schneider <andre.schneider@astro.su.se><br>
<b>Sent:</b> Monday, December 2, 2019 7:43:34 PM<br>
<b>To:</b> Okc-wp4@fysik.su.se; people@nordita.org<br>
<b>Subject:</b> [Okc-wp4] EO meeting Thu Dec 5 @ 13:15 KTH meeting room</font>
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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;"></span><span style="font-family: Calibri, Helvetica, sans-serif, serif, "EmojiFont"; font-size: 12pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the
next EO meeting will take place this Thursday Dec</span><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;"> 5</span></span><br>
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<p><span style="font-family: Calibri, Helvetica, sans-serif, serif, "EmojiFont"; font-size: 12pt;"><span role="button" class="contextualExtensionHighlight ms-font-color-themePrimary ms-border-color-themePrimary ident_146_202" style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;" tabindex="0">at
13:15 in the KTH meeting room on the 5th floor of the</span><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">
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<p><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">AlbaNova University Centre.</span><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">
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<p><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">There will be two speakers.</span></p>
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<p><span style="font-family: Calibri, Helvetica, sans-serif, serif, "EmojiFont"; font-size: 12pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Speaker:</span><b></b><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">
</span><span></span><b><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Joonas Nättilä</span></b><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, serif, "EmojiFont"; font-size: 12pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Physics of turbulence in magnetically-dominated
collisionless plasmas</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;"></span></span></span></font></p>
<p><font size="2"><span style="font-size:10pt"><span style="font-family: Calibri, Helvetica, sans-serif, serif, "EmojiFont"; font-size: 12pt;"></span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;"></span><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Abstract:</span></span></font></p>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">I'll present our current efforts for understanding the physics of turbulence in magnetized, weakly-collisional plasmas. Such turbulent plasmas can be found, for example, in accretion
disk coronae, pulsar wind nebulae, gamma-ray bursts, and magnetically-confined fusion reactors. Our results are based on new massively-parallel fully-kinetic particle-in-cell simulations of decaying turbulence. These simulations offer new insights into the
physics of the turbulent energy cascade, particle acceleration mechanisms, and possible radiation signatures from such plasma.</span><br>
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<div><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Speaker:
</span><b><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Ana Sagués Carracedo</span></b></div>
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<p><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Title:</span></p>
<div><font style="font-family: Helvetica Neue, serif, "EmojiFont";" face="Helvetica Neue"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Detection and follow-up of Kilonovae with the Zwicky Transient Facility</span></font>
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<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Abstract:</span></div>
<div><font style="font-family: Helvetica Neue, serif, "EmojiFont";" face="Helvetica Neue"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">The first detection of gravitational waves from a binary neutron star merger, GW170817, was
associated with a short gamma-ray burst and the kilonova AT2017gfo, localised to nearby galaxy NGC 4993 at around 40 Mpc. The kilonovae was followed-up over the following days and weeks along the electromagnetic spectrum from UV to NIR and it was found The
orientation of the merger plane was facing-on, a favorable scenario for the follow-up campaign.This unique discovery gave rise to a new era in multi-messenger astronomy and showed the relevance of these events in astrophysics, cosmology, and nuclear physics.
Today, we aim at detecting many more kilonovae to answer the many open questions related to BNS and their use as physics laboratories. However, the observations of kilonovae are generally challenging as these are rare, fast and faint transients. During the
talk, I will present the observational challenges and how to study the detectability of kilonovae using survey simulations. I will show results from the Zwicky Transient Facility (ZTF) that quantifies the importance of the observing strategy. I will outline
the plans to use the available ZTF all-sky observations to constrain the rates of short-lived transients compatible with kilonovae.
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<div>See you there!<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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