BEGIN:VCALENDAR
VERSION:2.0
PRODID:icalendar-ruby
CALSCALE:GREGORIAN
METHOD:PUBLISH
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
UID:https://www.ipp.mpg.de/events/41197/5593513
DTSTART:20250320T093000Z
DTEND:20250320T110000Z
CLASS:PUBLIC
CREATED:20250312T081213Z
DESCRIPTION:Abstract: How magnetized turbulent plasmas can accelerate charg
 ed particles to high energies forms a long-standing question with far-reac
 hing implications for multi-messenger astrophysics. It indeed goes back to
  the seminal works of Enrico Fermi in the late 1940s and nowadays\, it is 
 commonly invoked to model the generation of non-thermal particle spectra i
 n a broad variety of astrophysical sites\, including extreme\, relativisti
 c sources such as black hole accretion disks\, pulsar wind nebulae\, or re
 lativistic jets from active galactic nuclei. In a first part\, this semina
 r will summarize recent progress in this area and propose a modern theoret
 ical picture of the physics at play\, which can be regarded as a generaliz
 ation of the original Fermi scenario. In a second part\, these results wil
 l be placed in the context of magnetized turbulent coronae of active galac
 tic nuclei to understand if and how this process can explain the origin of
  high-energy neutrinos recently detected by the Ice Cube experiment in the
  direction of Seyfert galaxies.\nVortragende(r): Dr. Martin Lemoine
LAST-MODIFIED:20250312T081727Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Astrophysical turbulent plasmas as extreme particle accelerators an
 d sources of very high-energy neutrinos
URL;VALUE=URI:https://www.ipp.mpg.de/events/41197/5593513
END:VEVENT
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
UID:https://www.ipp.mpg.de/events/41198/5593513
DTSTART:20250327T093000Z
DTEND:20250327T110000Z
CLASS:PUBLIC
CREATED:20250312T081827Z
DESCRIPTION:Abstract: Blazars are promising candidates for astrophysical ne
 utrino sources. Multi-messenger lepto-hadronic models based on proton--pho
 ton (p-gamma) interactions predict spectra that peak at high energies\, wh
 ereas statistical searches often assume a power-law shape\, emphasising lo
 wer energies. We investigate how these spectral assumptions impact neutrin
 o--blazar associations by incorporating physically motivated spectra into 
 our Bayesian point-source framework. Using predictions from Rodrigues et a
 l. (2024)\, we analyse 10 years of IceCube data and identify five candidat
 e sources. Our results show that $p\\gamma$ spectra suppress low-energy as
 sociations but may enhance high-energy ones. Strong associations then impl
 y that energetic neutrino events likely have much higher true energies tha
 n those inferred under a power-law assumption. This is particularly releva
 nt in light of the recent KM3NeT detection of the highest-energy neutrino\
 , reinforcing the need for theory-driven models to interpret multi-messeng
 er signals.\nVortragende(r): Julian Kuhlmann
LAST-MODIFIED:20250312T081944Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Impact of multi-messenger spectral modelling on blazar--neutrino as
 sociations
URL;VALUE=URI:https://www.ipp.mpg.de/events/41198/5593513
END:VEVENT
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
UID:https://www.ipp.mpg.de/events/41778/5593513
DTSTART:20250515T083000Z
DTEND:20250515T100000Z
CLASS:PUBLIC
CREATED:20250506T131350Z
DESCRIPTION:Abstract: The origin and propagation of cosmic rays (CRs) is a 
 multi-disciplinary problem in which plasma (astro)physics plays a major ro
 le. Plasma processes are indeed determining how these charged particles ar
 e injected and accelerated at their astrophysical sources\, as well as the
  type of turbulence that CRs encounter as they propagate through different
  Galactic environments\; cosmic-ray propagation itself is defined by plasm
 a processes underlying their non-linear interaction with turbulence. More 
 than a century after their discovery\, our understanding of the processes 
 yielding cosmic rays and defining their journey through the Galaxy cannot 
 be considered satisfactory.In this talk\, I will discuss how the most-rece
 nt direct and indirect CR measurements challenge the naive picture of cosm
 ic-ray transport that is usually adopted by the astroparticle community\, 
 delving in what are the issues with a standard description of CR scatterin
 g based on Alfvénic fluctuations. I will also present recent results base
 d on different approaches that may solve some of the typical issues\, but 
 that simultaneously lead to new open questions.\nVortragende(r): Dr. Silvi
 o Sergio Cerri
LAST-MODIFIED:20250506T131608Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Cosmic-ray transport (in the Galaxy): a micro-physics perspective
URL;VALUE=URI:https://www.ipp.mpg.de/events/41778/5593513
END:VEVENT
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
UID:https://www.ipp.mpg.de/events/41811/5593513
DTSTART:20250519T120000Z
DTEND:20250519T133000Z
CLASS:PUBLIC
CREATED:20250509T140559Z
DESCRIPTION:Abstract: Cosmic rays (CRs) with energies below the 'knee' at a
 bout 3 PeV are believed to be of Galactic origin\, but it is still not ful
 ly understood in which astrophysical objects they are produced. The classi
 cal paradigm states that Supernova remnants (SNRs) are the main sources of
  Galactic CRs mainly on the account of their energy budget that is suffici
 ent to explain the energy density of low-energy CRs. But whether SNRs are 
 responsible for all the Galactic CRs or not remains an open question as ma
 ny pieces of the puzzle are still missing. To answer this question it is n
 ecessary to understand whether SNRs can accelerate particles beyond PeV en
 ergies and whether the total yield of CRs from SNRs is compatible with obs
 ervations in terms of the spectral shaper and elemental composition. In th
 is talk I will critically assess the capabilities of SNRs as CR accelerato
 rs by the means of multiwavelength observations and numerical simulations.
 \nVortragende(r): Dr. Iurii Sushch
LAST-MODIFIED:20250509T141629Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Supernova remnants as factories of cosmic rays
URL;VALUE=URI:https://www.ipp.mpg.de/events/41811/5593513
END:VEVENT
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
UID:https://www.ipp.mpg.de/events/41897/5593513
DTSTART:20250522T083000Z
DTEND:20250522T100000Z
CLASS:PUBLIC
CREATED:20250520T065922Z
DESCRIPTION:Abstract: The detection of a flux of TeV neutrinos from the nea
 rby Seyfert galaxy NGC1068 is particularly intriguing. The neutrino flux m
 easured by the IceCube neutrino observatory is at least two orders of magn
 itude higher than its gamma-ray counterpart\, in contrast with the hypothe
 sis of correlation between high-energy neutrinos and gamma-rays in AGN. Th
 is finding motivated further searches for neutrino emission in sources sim
 ilar to NGC 1068. This source is among the brightest X-ray Seyfert galaxie
 s\, supporting models that suggest that high-energy neutrinos are produced
  in the vicinity of the supermassive black hole\, most likely in the AGN c
 orona. I will present the most recent IceCube results on searches for neut
 rino sources\, including both a follow-up of already published results and
  findings on a newly compiled list of X-ray bright non-blazars AGN. In par
 ticular\, we confirm the measurement of a neutrino flux from NGC1068\, and
  we report the evidence of neutrino emission from a subset of 11 X-ray bri
 ght AGN at a 3.3σ level.\nVortragende(r): Elena Manao
LAST-MODIFIED:20250520T070017Z
LOCATION:IPP L7A\, Raum: 121
ORGANIZER;CN=Plasma Astrophysics group (TOK):mailto:artem.bohdan@ipp.mpg.de
SUMMARY:Neutrino Emission from X-ray Bright Active Galactic Nuclei: a revie
 w of recent IceCube results
URL;VALUE=URI:https://www.ipp.mpg.de/events/41897/5593513
END:VEVENT
BEGIN:VEVENT
DTSTAMP:20260522T071536Z
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
END:VEVENT
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