17th European Solar Physics Meeting ESPM-17

Session

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

2

9 Sept 2024, 11:30

Turin, Italy

Conveners

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

• Istvan Ballai (University of Sheffield)

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

• Daniel Müller (ESA)

29. Disentangling magnetic reconnection in the solar atmosphere.

Daniel Nóbrega-Siverio (Instituto de Astrofísica de Canarias (IAC) | Rosseland Centre for Solar Physics (RoCS))

09/09/2024, 11:30

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Invited

In this presentation, we will explore the fundamental properties of magnetic reconnection, with a particular emphasis on the complexities of three-dimensional (3D) reconnection and the differences with two-dimensional (2D) scenarios. We will present recent state-of-the-art numerical simulations that show how 3D reconnection is key to understanding a variety of phenomena such as braiding,...

230. Flux-rope mediated turbulent reconnection

Alexander Russell (University of St Andrews)

09/09/2024, 11:55

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Understanding the interplay between magnetic reconnection and turbulence is an important challenge in solar physics, which must be solved to address the fundamental processes and properties of solar flares and other coronal energy releases. In the last few years, exciting advances in this area have been enabled by 3D direct numerical simulations that capture the generation of turbulence inside...

202. State-of-the-art observational aspects of MHD waves in the lower atmosphere

Marco Stangalini (ASI Italian Space Agency)

09/09/2024, 12:10

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Invited

MHD waves are recognized as significant contributors to the energy budget of the solar atmosphere, the acceleration of the solar wind and the composition of coronal plasma. Recent advancements in instrumentation, techniques, and processing methods have unlocked new diagnostic capabilities for exploring the excitation and propagation of MHD waves within various magnetic structures in the solar...

86. Simulating Energetic Particle Transport in the Solar Corona with COCONUT+PARADISE

Edin Husidic (KU Leuven, Belgium/University of Turku, Finland)

09/09/2024, 12:35

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Solar eruptive events such as coronal mass ejections (CMEs), along with the associated solar energetic particles (SEPs), pose serious threats to spacecraft and astronauts. The growing impact of these harsh space weather events on modern societies has driven the development of numerical models capable of enhancing our understanding of the underlying physics and reliably forecasting these...

330. Radiation Properties of Cool Coronal Condensations

Petr Heinzel (Czech Academy of Sciences)

09/09/2024, 14:35

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Invited

Cool plasma condensations in the corona manifest themselves as various types of
prominences, loop structures, flare loops, coronal rain etc. They can be highly
dynamical, exhibiting fine structures down to resolution of current instruments.
Nowadays they are modeled using multidimensional MHD simulations. But to compare
with observations, a non-LTE radiative-transfer spectral synthesis is...

128. Nanoflare and nanojets in MHD simulations of magnetic reconnection in coronal loops.

Paolo Pagano (Università degli Studi di Palermo)

09/09/2024, 15:00

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Reconnection events in coronal loops are singularly too small and fast to be detected (nanoflares), whereas their collective action could be sufficient to sustain the million degrees corona against thermal conduction and radiative losses. Recent studies have observed and modelled the dynamic counter part of nanoflares, i.e. the nanojets, which are a byproduct of the magnetic reconnection and...

148. Estimating the total energy content in escaping accelerated solar electron beams

Dr Alexander James (University College London)

09/09/2024, 15:15

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Quantifying the energy content of accelerated electron beams during solar eruptive events is a key outstanding objective that must be constrained to refine particle acceleration models and understand the electron component of space weather. Previous estimations have used in situ measurements near the Earth, and consequently suffer from electron beam propagation effects. In this study, we...

155. The angular dependence of rise and decay times of solar radio bursts using multi-spacecraft observations

Dr Nicolina Chrysaphi (LPP, Sorbonne University, France)

09/09/2024, 15:30

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Radio photons interact with anisotropic density fluctuations in the heliosphere which can alter their trajectory and distort the properties that are deduced from observations. This is particularly evident in solar radio observations, where anisotropic scattering leads to highly-directional radio emissions, meaning that observers at varying locations will measure different radio-source...

184. Simulation of particle acceleration and transport in 3D turbulent reconnection regions

Xin Cheng (Nanjing University)

09/09/2024, 15:45

Fundamental mechanisms of solar plasmas: magnetic reconnection, waves, radiation and particle acceleration

Talk

Observation and simulation studies suggest that particles can be accelerated in the current sheet and above the loop-top during solar flares. Considering the flare process is a turbulent 3D phenomenon in reality, 3D models are crucial for understanding and interpreting particle acceleration in flares. Using the Stochastic Differential Equations (SDE) method to solve the Parker Transport...