Conveners
Poster Session 6.4
- Elena Khomenko (Instituto de Astrofisica de Canarias)
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Rajab Ismayilli (Centre for mathematical Plasma Astrophysics, KU Leuven)08/09/2021, 11:00Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
We are studying MHD plasma turbulence generated by unidirectional surface Alfven waves, called ”Uniturbulence.” We analyze uniturbulence in the theoretical model with a sharp interface where surface Alfvén wave propagates. We consider an equilibrium configuration in a Cartesian coordinate system with a background magnetic field directed along the z-axis and no background flow. We take...
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Ramada Sukarmadji (Northumbria University)08/09/2021, 11:13Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The recently discovered nanojets in a coronal loop (Antolin et al., 2021) were characterised in part by small (500-1500 km) and rapid (150-250 km/s) bursts of plasma ejected perpendicular to the field line of origin and accompanied by nanoflare-like intensity bursts in the UV and EUV. These nanojets were interpreted as a product of magnetic reconnection from small misalignments between the...
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Richard Morton (Northumbria University)08/09/2021, 11:26Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
The focus of many investigations on coronal wave heating has been on scrutinising the role of transverse (i.e. kink) modes; examining their damping by resonant absorption and the transfer of energy to Alfvén modes. Subsequently, the Alfvén modes are then subject to phase mixing and this leads to plasma heating. More recently, a non-linear mechanism for energy transfer has also been proposed,...
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Mr Ritesh Patel (ARIES, Nainital, India)08/09/2021, 11:39Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
We investigate the properties of plasmoids observed in the current sheet formed after an X-8.3 flare on September 10, 2017, using Extreme Ultraviolet (EUV) and white-light coronagraph images. The main aim is to understand the evolution of plasmoids at different Spatio-temporal scales using existing ground- and space-based instruments. We identified plasmoids in the current sheet observed in...
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Mr Robbe Vansintjan (Royal Observatory of Belgium)08/09/2021, 11:52Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
Developed in the framework of the H2020 SOLARNET project, the Solar Virtual Observatory (SVO) aims at making solar data more findable and accessible to the solar physics community. The SVO allows searching across multiple datasets as well as across the Heliophysics Event Database (HEK) and lets you search for data that overlaps with events from the HEK. It is conceived so that other event...
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Giulio Del Zanna (University of Cambridge (UK))08/09/2021, 12:05Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
Fundamentally different models are required for line emission in the corona compared to the chromosphere. Modelling the corona is remarkably straightforward by comparison, and the tendency for modellers and observers is to use coronal modelling in the transition region as well. Discrepancies with observations become obvious, however, when using the modelling for lines emitted by low charge...
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Rohit Sharma (University of Applied Sciences Northwestern Switzerland)08/09/2021, 12:18Session 3 - Fundamental Plasma Processes in the Solar Atmosphere: Magnetic Reconnection, Waves, Emission, Particle AccelerationPoster
During solar flares, particles are accelerated to relativistic energies producing radio bursts at a large range of frequencies. The intensity of these radio bursts depends on their emission mechanism and the local conditions such as magnetic field strength, plasma density and the distribution of accelerated electrons. However, the presence of MHD waves in the loops can periodically change the...
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