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Dear all,</span><br>
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<p><font color="#212121" face="wf_segoe-ui_normal, Segoe UI, Segoe WP, Tahoma, Arial, sans-serif, serif, EmojiFont"><span style="font-size:14px">our first EO meeting of 2019 will be this Thursday <b>Feb 7 at 13:00 (</b>KTH meeting room on the 5th floor). </span></font></p>
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<p><b style="color:rgb(33,33,33); font-family:wf_segoe-ui_normal,"Segoe UI","Segoe WP",Tahoma,Arial,sans-serif,serif,EmojiFont; font-size:14px">Joonas Nättilä</b><span style="color:rgb(33,33,33); font-family:wf_segoe-ui_normal,"Segoe UI","Segoe WP",Tahoma,Arial,sans-serif,serif,EmojiFont; font-size:14px"> will </span><span style="color:rgb(33,33,33); font-family:wf_segoe-ui_normal,"Segoe UI","Segoe WP",Tahoma,Arial,sans-serif,serif,EmojiFont; font-size:14px">give</span><span style="color:rgb(33,33,33); font-family:wf_segoe-ui_normal,"Segoe UI","Segoe WP",Tahoma,Arial,sans-serif,serif,EmojiFont; font-size:14px"> </span><span style="color:rgb(33,33,33); font-family:wf_segoe-ui_normal,"Segoe UI","Segoe WP",Tahoma,Arial,sans-serif,serif,EmojiFont; font-size:14px">the
following talk:</span><br>
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<div style="font-size:15px">Title: Magnetically-dominated collisionless plasma flows in neutron star atmospheres</div>
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<div style="font-size:15px">Abstract: I will discuss collisionless plasma instabilities operating on magnetically-dominated flows in neutron star atmospheres. We define a criteria for out-of-resonance two-stream instability to be operational in the stratified
atmosphere. Our theoretical findings are then confirmed with high-resolution, first-principles relativistic Vlasov-Maxwell simulations. This allows us to study the subsequent non-linear turbulent evolution of the system. We find a new plasma mechanism that
reprocesses the incoming mildly-relativistic beams: The incoming beams are slowed down, heated up, but not brought to full halt either. Ultra-relativistic beams are still capable of penetrating into the star unaffected. This implies that diluted free-falling
accretion flows into neutron stars are always reprocessed in the uppermost layers of the star's atmosphere before entering the particle-collision-dominated layers below. This beam-atmosphere interaction is also responsible of heating the corona. The reprocessing
of the beam leads to a turbulent atmospheric layer where outward moving double layers are being excited. These uprising particle-acceleration sites are similar to earthly auroras, and are a possible new source of non-thermal X-ray radiation from neutron stars.</div>
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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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