From the Convection Zone to the Heliosphere

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From the Convection Zone to the Heliosphere

Presentation transcript:

From the Convection Zone to the Heliosphere Bridging the Great Divide: Linking the Solar Dynamo to the Dynamic Heliosphere Part II: From the Convection Zone to the Heliosphere Tuesday, July 12, 9:45am-12:45pm Session Leaders: George Fisher & Janet Luhmann

All about Active regions!!! Topic A: How does the small-scale surface dynamo interact with the interior dynamo? Can we tell what the large-scale fields are like below the surface (are they concentrated or are they turbulent) from what we see on the photosphere? How do the small-scale surface fields affect the sub-surface fields? All about Active regions!!!

Follow-up questions: Turbulence Vs. large-scale organization of the field (Spruit). What is the role of active regions and where does their characteristic developed (convection zone or near the surface shear layer). Meridional flow should address reconnection across the equator, while moving the opposite flux towards the poles.

Contribution by Maria Weber and Georgios Chintzoglou: Without Convection With Convection

Flux cancellation of active regions and large unipolar field (polar field)

MHD simulation of flux emergence by Ward B MHD simulation of flux emergence by Ward B. Manchester IV (Chip) (Fang et. al 2010): X-type flux cancellation

Topic B: Surface Flux Transport and Flux Cancellation Does surface flux transport really matter to the dynamo or are the large scale fields, including polar fields, just an end product of no consequence? Does the simplification of the magnetic field in the declining phase of the solar cycle, as observed on the photosphere, reflect anything about the evolution of the magnetic field in the interior? How does flux cancellation work -- can it be described via a turbulent diffusion model, or does it result in the expulsion of helicity and poynting flux into the outer solar atmosphere?

Why does the 2D flux transport picture work so well anyway Why does the 2D flux transport picture work so well anyway? What are the essential elements of field evolution inferred from these? Racine et al., ApJ 2011 Wang et al., ApJ 2002, 2005

Follow-up questions: How much does the observed field on the surface really matters to the field generation and evolution? How does the polar field canceled? The role of outer BC in dynamo models. Brown et al., ApJ 2011

Topic C: Larger Coronal and Heliospheric Involvement? How does the magnetic flux from the solar interior and photosphere interact with the open and closed magnetic fields in the corona and heliosphere? Does the observed escape of magnetic helicity into the corona and heliosphere influence the operation of the interior dynamo? To what extent is the helicity observed in the corona erupting from below, as opposed to being dynamically generated near the surface? Follow-up questions: Do CMEs are responsible for helicity removal from the Sun? Does the dynamo drives the surface and the corona or is there any feedback?

Contribution by Dick Altrock: Distribution of coronal holes based on PFSSM Number of Coronal Fe XIV Emission Regions

Bottom line of the session: The solar interior and the SHINE communities should talk to each other more often!!!