Long-Term Solar Variability (LSV) Section
Magnetic Flux Emergence
The current prevailing picture is that magnetic active regions on the solar surface originate from strong, predominantly toroidal magnetic fields generated by the solar dynamo mechanism at the thin tachocline layer at the base of the solar convection zone. Thus the magnetic fields need to traverse the entire convection zone (the outer 30% of the solar interior) before they reach the photosphere to form the observed sunspots and solar active regions, which are centers of solar eruptions. Understanding the process of magnetic flux emergence through the solar convection zone is therefore crucial for understanding the link between the observed magnetic activities at the surface and the dynamo-generated magnetic fields in the interior.
Using MHD numerical simulations, HAO scientists have modeled the formation and rise of buoyant of magnetic flux tubes in the solar convection zone and their emergence through the photosphere into the solar atmosphere. Read More »
Currently, HAO scientists lead and support modeling efforts studying flux emergence. Read More »
See Profiles in Science pages for Yuhong Fan, Mark Miesch, and Matthias Rempel.