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Parallel sessions
Sessions
id
date time
2022-03-08 11:45:00
New light on solar coronal heating: convergence of theory, numerical models, and observations
Solar7
Since Grotrian (1939) discovered 'forbidden lines' of iron in the Sun's emission spectrum, the question of what sustains the multi-million-degree temperatures in the solar atmosphere has been one of the most significant and enduring questions in solar physics. Most proposed solutions involve a crucial role for the magnetic field. On short, oscillatory timescales, it supports a mixture of waves, which carry energy into the corona that can then dissipate. On longer timescales, it allows the build-up of magnetic energy, which is then explosively released by instabilities and magnetic reconnection. Both can lead to a cascade to shorter length scales, bringing about the onset of plasma and MHD turbulence. All of the micro-physical processes involved on these short length scales are poorly understood. Increasingly sophisticated theories propose new explanations for them. Prominently, magnetic reconnection on the Sun is now far better understood, in terms of the tearing mode, having developed from early concepts of Sweet and Parker. Through the combination of new numerical techniques, growing computational power, and greater insight into the underlying physics, numerical models have similarly advanced. Now, they can study the onset of these processes, and their dynamic, non-linear evolution, with increasing accuracy. Recent, state-of-the-art facilities and instruments, such as DKIST, Solar Orbiter, and the Parker Solar Probe, give a new perspective on the physical processes underway in heating the solar atmosphere. With closer physical proximity and finer optical resolution, they shed new light on the conditions in which these several processes commence, as well as their dynamic and thermodynamic aftermath. Theoretical and numerical conjectures can then be tested and assessed against these results. Therefore, this session will explore coronal heating by magnetohydrodynamic and micro-physical instabilities, standing and propagating waves, and plasma turbulence. Complex behaviours that contribute to coronal heating will be discussed, informed by the latest advances in theory, numerical modelling, and observations. Convergence between these approaches will advance our understanding of the processes that release energy in the atmosphere and maintain coronal temperatures.
Thomas Howson & Jack Reid
Mon. 16:30-18:00 / Tues. 09:00-10:30
16:30-17:00 Konstantinos Karampelas: Oscillatory Reconnection in a hot coronal plasma [invited]
17:00-17:12 Jack Reid: Linking 3D and 1D computational models to follow evolution of heated coronal plasma
17:12-17:24 Daniel Johnson: A Numerical Investigation of Sunspot Rotation
17:24-17:36 Seray Sahin: Prevalence of Thermal Non-Equilibrium over an Active Region
17:36-17:48 Patrick Antolin: Thermal Instability–Induced Fundamental Magnetic Field Strands in the Solar Corona
17:48-18:00 Anthony Yeates: On the limitations of magneto-frictional relaxation
09:00-09:30 Paola Testa: Observations of the solar atmosphere and diagnostics of coronal heating mechanisms [invited]
09:30-09:42 Ramada Sukarmadji: Transverse MHD waves as signatures of braiding-induced magnetic reconnection in coronal loops
09:42-09:54 Tongjiang Wang: Observation and modeling of standing and reflected propagating slow-mode waves in flaring coronal loops
09:54-10:06 Andrew Hillier: Turbulent damping of MHD kink waves
10:06-10:18 Rahul Sharma: Quantifying transverse dimension scales associated with Alfvenic turbulence in solar corona
10:18-10:30 Adam J. Finley: Stirring the Base of the Solar Wind