Unfolding the sources of solar magnetism with helioseismology and simulations
by
Juri Toomre(JILA, University of Colorado, Boulder)
→
Europe/Stockholm
Klein Auditorium
Klein Auditorium
Description
There exist major challenges to understand how the Sun builds the large-scale
and intense magnetic fields that we observe at its surface and how these fields
evolve in time. The origin of these magnetic fields must rest with dynamo
processes occurring deep within the star. Many complex dynamical elements are
involved in the operation of the solar global dynamo. These include the
differential rotation of the convection zone and the tachocline at its base,
turbulent production and transport of the magnetic fields by the convection,
shear amplification of the fields, and magnetic buoyancy that leads to the
eventual field eruption onto the photosphere. Major advances in supercomputing
are allowing us to improve the fidelity with which we can model these intensely
turbulent processes. These efforts are aided by continuing guidance provided by
helioseismology in probing dynamics in the solar interior. We discuss the close
interplay between helioseismology and recent 3-D simulations in studying the
solar global dynamo.
