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METHOD:PUBLISH
BEGIN:VEVENT
DTSTAMP:20260522T132621Z
UID:https://www.ipp.mpg.de/events/43274/5593513
DTSTART:20251009T083000Z
DTEND:20251009T100000Z
CLASS:PUBLIC
CREATED:20251002T123404Z
DESCRIPTION:Abstract: Shocks are promising sites of particle acceleration i
 n extragalactic jets. In electron-ion shocks\, electrons can be heated up 
 to large Lorentz factors\, making them an attractive explanation for the h
 igh minimum electron Lorentz factors regularly needed to model blazar SEDs
 . Still\, the thermal electron component is commonly neglected when modell
 ing observations. In this talk\, we present a multi-wavelength modelling o
 f the blazar Mrk421 employing a particle distribution whose shape is direc
 tly motivated by predictions of plasma PIC simulations. We demonstrate tha
 t fluxes in the optical/UV and MeV-GeV bands efficiently restrict the emis
 sion from the thermal (relativistic) Maxwellian electrons\, allowing us to
  obtain constraints on the shock properties. Notably\, we find that at lea
 st ~10% of the shock energy must be transferred to the nonthermal electron
 s in order to stay compatible with the fluxes in the optical/UV and MeV-Ge
 V bands. These results are almost insensitive to the shock velocity\, alth
 ough radio observations suggest a shock Lorentz factor above ~5. In the se
 cond part of the talk\, we present preliminary results of dedicated PIC si
 mulations to verify under which physical conditions of electron-ion shocks
  these findings can be matched.\nVortragende(r): Dr. Axel Arbet-Engels
LAST-MODIFIED:20251002T123809Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Radiative signatures of electron-ion shocks in blazar jets
URL;VALUE=URI:https://www.ipp.mpg.de/events/43274/5593513
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