The Effect of Subsurface Flows during Flux Emergence

Details The Effect of Subsurface Flows during Flux Emergence The Effect of Subsurface Flows during Flux Emergence

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh54a..06f&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH54A-06

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere

Scientific paper

Here we carry out magnetohydrodynamic simulations on the emergence of a buoyant magnetic flux rope through a realistic convection zone that extends 21 Mm below the photosphere and 21 Mm up into the corona, with solar thermodynamic processes taken into account. The total maximum magnetic flux at the photosphere reaches 6.85±1020 Mx, of the same order of magnitude of solar pores. The main aim of the simulations is to study the mechanism of the energy and magnetic flux transfer during the interaction between the subphotospheric flows and the rising magnetic flux rope. The magnetic flux emerges as bipoles on the photospheric and subphotospheric layers, then the bipoles are quickly pulled apart by the horizontal flows and concentrate in downdrafts. The coalescence of the small-scale bipoles and convective collapse in the near surface layers form the large-scale concentrated magnetic flux, i.e. solar pores. The horizontal flow also exhibits a coherent pattern of rotation, which extends into the convection zone. Vertical flow in the convection zone pushes down the endpoints of the flux rope and maintains the bipolar pores during the emergence. Analysis of the Poynting energy fluxes associated with vertical and horizontal flows shows that horizontal flow is the main contributor to the energy transfer from the convection into the corona, with a value of 6.78±1031 ergs at the photosphere within 8 hours.

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