ST15 ‘MHD Waves and Instabilities in the Solar Atmosphere: Identification and Modelling’, AOGS 2019 – deadline extended to 19 February 2019February 14, 2019, from Viktor Fedun
We would like to draw your attention to the ST15 session: ‘MHD Waves and Instabilities in the Solar Atmosphere: Identification and Modelling’ in the framework of Asia Oceania Geosciences Society (AOGS) conference. The 16th Annual AOGS will take place in Singapore, 28 July-02 August 2019. Further details regarding abstract submission, registration, accommodation and relevant deadlines can be found on the meeting website: http://www.asiaoceania.org/aogs2019/public.asp?page=abstract.htm
Important! Abstract submission deadline is 19 February 2019.
ST15 ‘MHD Waves and Instabilities in the Solar Atmosphere: Identification and Modelling’
Dr Viktor Fedun (The University of Sheffield, United Kingdom), firstname.lastname@example.org
Dr Wernher Brevis (Pontificia Universidad Catolica de Chile, Chile), email@example.com
Dr Sergiy Shelyag (Deakin University, Australia), firstname.lastname@example.org
Dr Marco Stangalini (INAF-OAR National Institute for Astrophysics, Italy), email@example.com
Dr Gary Verth (The University of Sheffield, United Kingdom), firstname.lastname@example.org
Space-based and ground solar observations have detected a variety of plasma waves, oscillations, and instabilities (e.g., fast/slow/EUV waves, global kink and sausage mode oscillations, Alfven waves) propagating in the magnetised plasma structures on the Sun. These magnetic configurations are observed across a wide range of spatio-temporal scales (e.g., small scale flux ropes in the surface-granulation pattern, spicules, solar prominences, coronal loops). Over the last years, due to both technical advancements and improved inversion techniques, spectropolarimetry has become an import tool for the investigation of the plasma-magnetic field interaction in the solar atmosphere, providing new diagnostics useful for the study and identification of MHD waves and modes in different magnetic concentrations, down to the present resolution limit of solar telescopes (100-150 km). However, forthcoming and recently launched next generation of solar observational facilities e.g. The Daniel K. Inouye Solar Telescope (DKIST) and European Solar Telescope (EST), COronal Solar Magnetism Observatory (COSMO), Solar Orbiter and Solar Probe, thanks to their unmatched spatial resolution and spectropolarimetric sensitivity and accuracy, will further advance our possibilities, by providing an unprecedented view of the mechanisms of excitation and dissipation of MHD waves in the solar atmosphere. Development of mathematical models (analytical and numerical) and data analysis techniques of observable solar plasma structures can help us fully utilize their diagnostic capabilities and better understand the role of various plasma processes in energy transport across different layers of the solar atmosphere. The proposed session will provide us an excellent platform to bring together world-leading experts in solar observational analysis and numerical analytical / modelling, in order to exploit different approaches in the investigation of plasma processes in the solar atmosphere.
With our Best Regards,
Viktor Fedun, Wernher Brevis, Sergiy Shelyag, Marco Stangalini and Gary Verth