Description
Invited Speakers: N. Aunai (LULI), V. Brunn (Obs Arcetri, Italy), S. Masson (LPP)
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Dr Pierre Henri ((1) Laboratoire Lagrange, Observatoire Côte d'Azur, Université Côte d'Azur, CNRS, Nice, France & (2) LPC2E, CNRS, Univ. Orléans, CNES, Orléans, France)20/05/2026 09:25
This review synthesizes global hybrid Particle-in-Cell (PIC) simulations using the Menura code to investigate how solar wind turbulence dynamically reshapes the plasma environments of magnetized and unmagnetized bodies. We employ a two-step dynamical approach: decaying turbulence simulations to generate a fully developed turbulent solar wind, followed by global simulations of the...
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M. Enzo Figueiredo (IPAG)20/05/2026 10:25
The dynamics of black hole magnetospheres critically depend on the black hole spin and on the structure of the accretion flow. In the limit of a Schwarzschild black hole immersed in a zero-net angular momentum flow, accretion is spherical. However, in the presence of a large-scale vertical magnetic field, the classical Bondi accretion model is significantly altered. The frozen-in field is...
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Dr Sophie Masson (LPP - Observatoire de Paris)20/05/2026 11:30
Solar eruptions are initiated and develop in the solar corona and are one of the most extreme manifestation of the sun impulsive release of energy. Solar particles are accelerated during solar eruption. We observe their radiative signatures in the solar atmosphere over a large range of wavelengths from EUV to gamma rays and measure them in-situ in the heliosphere. Solar energetic particles...
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Dr Nicolas Aunai20/05/2026 14:00
Magnetic reconnection at Earth’s magnetopause is the key process controlling the coupling between the solar wind and the magnetosphere, enabling plasma and magnetic flux from the interplanetary medium to enter an otherwise largely closed cavity. A central question is where reconnection develops along the magnetopause, since its location strongly influences the efficiency of this coupling....
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Dr Sophie Aerdker (APC Paris)20/05/2026 15:00
Shearing flows give rise to a Fermi-type acceleration and have been proposed to explain e.g. the presence of high-energy electrons along astrophysical jets and to contribute to the acceleration of ultra-high energy cosmic rays.
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Particles diffusing along the shearing direction experience a change in the flow speed, which translates to a change in momentum. In a Fokker-Planck picture, shear... -
Dr Valentin Brunn (Arcetri Observatory)20/05/2026 15:50
Young stellar objects host strongly magnetised and highly variable plasma environments in which several acceleration processes may generate suprathermal and non-thermal particles. In this talk, I will discuss two complementary regimes of particle acceleration in the star-disc system. The first is associated with large-scale magnetic reconnection during flares in the innermost regions, where...
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M. Enzo Figueiredo
The dynamics of black hole magnetospheres critically depend on the black hole spin and on the structure of the accretion flow. In the limit of a Schwarzschild black hole immersed in a zero-net angular momentum flow, accretion is spherical. However, in the presence of a large-scale vertical magnetic field, the classical Bondi accretion model is significantly altered. The frozen-in field is...
Aller à la page de la contribution