Conveners
Poster Session 5.4
- Elena Khomenko (Instituto de Astrofisica de Canarias)
-
Mariana Cécere (Instituto de Astronomía Teórica y Experimental (CONICET/UNC))08/09/2021, 09:00Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
In order to infer the properties of the coronal plasma, coronal seismology combines the measurement of temporal and spatial signals of oscillations and magnetohydrodynamic waves of different magnetic structures with their theoretical modeling. In the particular case of coronal loops, fast sausage modes and standing slow modes are the most studied oscillation modes, because their...
Go to contribution page -
Michaël Geeraerts08/09/2021, 09:13Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
In the context of the solar coronal heating problem, one possible explanation for the high coronal temperature is the release of energy by magnetohydrodynamic (MHD) waves. The energy transfer is believed to be possible, among others, by the development of the Kelvin-Helmholtz instability (KHI) in coronal loops. Our aim is to determine if standing slow waves in solar atmospheric structures such...
Go to contribution page -
Mikhail Modestov (Instituto de Astrofísica de Canarias)08/09/2021, 09:26Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The MANCHA code development was started in 2006 to study wave dynamics in sunspots at the Instituto de Astrofísica de Canarias.
Go to contribution page
Since then it has gradually been upgraded by adding new physics and improved programming techniques.
The code can be used for a large variety of problems from linear wave propagation and classical hydrodynamic instabilities to highly realistic simulations of... -
Dr Nenad Sakan (Institute of Physics Belgrade)08/09/2021, 09:39Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The absorption coefficients of hydrogen plasma, calculated within the frame of cut-off Coulomb potential model, for the wide area of electron densities and temperatures observed within the solar atmosphere are presented here. The optical parameter of hydrogen plasma of mid and moderately high nonideality parameter could be described successfully, thus enabling the modeling of optical...
Go to contribution page -
Ms Noémi Kinga Zsámberger08/09/2021, 09:52Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
We present our findings on MHD wave propagation and instabilities in asymmetric Cartesian waveguide models. Generalising the classical slab models this way, thanks to the introduction of various sources of asymmetry (background density, magnetic field or flow speed) allows us to more precisely investigate several important features in the richly structured solar atmosphere. By developing solar...
Go to contribution page -
Dr Peter Hunana (Instituto de Astrofisica de Canarias (IAC))08/09/2021, 10:05Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The atmosphere of the sun represents a complex physical environment
Go to contribution page
where two traditional classes of fluid theories come to interplay. While the solar chromosphere is typically modeled with fluid models derived under the highly-collisional assumption, whereas the collisional frequencies in the solar corona can become so small, that collisionless fluid models seem to be more appropriate. We... -
Philippe-A. Bourdin (University Graz)08/09/2021, 10:18Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The magnetic and current helicity of the field above active regions is thought to play a role when estimating the probability for coronal mass ejections or strong reconnection events. A deeper understanding of the mechanisms generating the helicity in the corona can be obtained with the help of observationally driven models, in particular magneto-hydrodynamic and ambipolar-diffusion...
Go to contribution page