Description
Chair: Matteo Palermo
A three-dimensional (3D) diffusion-barrier-type model is constructed for producing Forbush decreases (Fds) in the heliosphere. It is based on reduced diffusion inside these barriers, which is incorporated into a Stochastic Differential Equation (SDE) based time-dependent, cosmic ray transport model. This 3D numerical model for simulating Fds is built for and applied to a period of relatively...
Large gradual solar energetic particle (SEP) events are of particular importance because of their hazardous threats to astronauts and equipment in space. Although there are compelling observational evidence supporting the scenario of particle acceleration at strong shocks driven by coronal mass ejections, it is not clear how those high-energy particles are accelerated and what the determining...
Magnetic reconnection is an important driver of energetic particles in a variety of astrophysical phenomena, and may play a key role role in pre-heating and accelerating Solar Energetic Particles during events. Recently, we developed a guiding-center model that successfully described the fundamental electron energization mechanisms that operate during reconnection. The most efficient mechanism...
The protons in large solar energetic particle events are accelerated in the inner heliosphere by fast shocks produced by coronal mass ejections. Unless there are other sources, the protons these shocks act upon would be the solar wind. The efficiency of the acceleration depends on the kinetic energy of the protons. For 1 - 2 thousand km/s shocks, the most effective proton energies would be 10...
