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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><span role="button" class="contextualExtensionHighlight ms-font-color-themePrimary ms-border-color-themePrimary ident_28_94" tabindex="0">our
next EO meeting will take place this Thursday Apr 6 at 13:15.</span> </span></font></font></div>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;">The meeting will take place via zoom
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><a href="https://stockholmuniversity.zoom.us/j/446165416" class="OWAAutoLink" id="LPlnk820694" previewremoved="true">https://stockholmuniversity.zoom.us/j/446165416</a></span></font></font><br>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;">You'll be able to join the meeting after 1:00PM.</span></font></font></div>
<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;">Meeting will start at 1:15PM. More details below.<br>
</span></font></font></div>
<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><br>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><br>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;" id="divtagdefaultwrapper"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;">This
week <b>Vivek Chaurasia</b></span></font><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><b></b> (Stockholm University) will present
</span></font><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><br>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;" id="divtagdefaultwrapper"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><br>
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<div><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;" id="divtagdefaultwrapper"><font size="3" face="Calibri,Helvetica,sans-serif,serif,EmojiFont" color="black"><span style="font-size:12pt;"><font size="2"><span style="font-size:10pt;"><span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Title:
BNS Mergers: Effect of Spin Orientation</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; 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 style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">In this talk I will review the results of arXiv: 2003.11901 which is a</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">continuation of our study of the binary neutron star parameter space</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">by investigating the effect of the spin orientation on the dynamics,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">gravitational wave emission, and mass ejection during the binary</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">neutron star coalescence. For this we perform fully consistent (3+1) D</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">numerical relativity simulations for various precessing systems.</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">Although pulsar observations of BNS systems suggest that most NSs have</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">small spins this conclusion is based on a small selected set of</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">observed binaries. Similar to the uncertainty in the spin magnitude,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the orientation of spins in BNS systems is also highly uncertain and</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">unknown. Misaligned spins can be caused by the supernova explosions of</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the progenitor stars. A possible realignment of the spin with the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">orbital angular momentum due to accretion is only possible for the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">more massive NS, but not for the secondary star. In addition, for BNS</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">systems formed due to dynamical capture, there is no reason to have</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">aligned spins at all. We find that due to the particular choice</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">of the setups, five configurations show precession effects,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">from which two show a precession (‘wobbling’) of the orbital</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">plane, while three show a ‘bobbing’ motion, i.e., the orbital</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">angular momentum does not precess, while the orbital plane moves along</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the orbital angular momentum axis. Considering the ejection of mass,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">we find that precessing systems can have an anisotropic mass ejection,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">which could lead to a final remnant kick of about ∼40km/s for the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">studied systems. Furthermore, for the chosen configurations,</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">anti-aligned spins lead to larger mass ejecta than aligned spins, so</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">that brighter electromagnetic counterparts could be expected for these</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">configurations. Finally, we compare our simulations with the</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">precessing, tidal waveform approximant and find good agreement between</span><br>
<span style="font-family: Calibri, Helvetica, sans-serif; font-size: 12pt;">the approximant and our numerical relativity simulations.</span></span></font><br>
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<div>See you then!<br>
</div>
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<div>Topic: EO Meeting<br>
Time: Apr 9, 2020 01:00 PM Stockholm<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>
</p>
<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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