SH002-0008
Global Solar Flows and Magnetic Fields: Observing, Simulating and Predicting Their Impact on the Heliosphere and Terrestrial Atmosphere
Global Solar Flows and Magnetic Fields: Observing, Simulating and Predicting Their Impact on the Heliosphere and Terrestrial Atmosphere
Monday, 7 December 2020
Poster
Abstract:
Understanding origins and evolution of solar magnetic activity occurring on a wide range of time-scales, and the space weather effects caused by the particles and electromagnetic outputs that reach the Earth, requires knowledge of the physical origins of this activity below photosphere. Despite much progress, our knowledge of processes responsible for driving the magnetohydrodynamics of flows and fields below
photosphere and their relation to observed flows and magnetic activity is far from complete. For example, there is no consensus as to the number of meridional circulation-cells that exist in the Sun and the depth at which the poleward-flow switches direction to equatorward. Main objective of our LWS focused-science team is to jointly develop the most comprehensive, dynamically consistent picture of solar flows at the surface, in the convection zone and tachocline, and determine the MHD effects induced by these motions. We will present how we are developing consensus sets of observational constraints and simulating model-outputs of magnetic activity and flows, which can reliably be used as inputs to heliospheric and terrestrial-atmospheric models. The ultimate success will be in our ability to predict the features of solar cycle 25, including the active-latitudes and -longitudes, global- and localized-flows several months to years ahead.
photosphere and their relation to observed flows and magnetic activity is far from complete. For example, there is no consensus as to the number of meridional circulation-cells that exist in the Sun and the depth at which the poleward-flow switches direction to equatorward. Main objective of our LWS focused-science team is to jointly develop the most comprehensive, dynamically consistent picture of solar flows at the surface, in the convection zone and tachocline, and determine the MHD effects induced by these motions. We will present how we are developing consensus sets of observational constraints and simulating model-outputs of magnetic activity and flows, which can reliably be used as inputs to heliospheric and terrestrial-atmospheric models. The ultimate success will be in our ability to predict the features of solar cycle 25, including the active-latitudes and -longitudes, global- and localized-flows several months to years ahead.