Magnetic underdense regions and multiscale convection on the solar surface
Abstract
The turbulent convective flows on the solar surface govern the motion of magnetic elements. Such elements are arranged in typical patterns which are observed as a variety of multiscale magnetic underdense regions (voids). We investigate the physics of multiscale convection on Sun's surface, characterized by the coexistence of large-scale flow associated with supergiant cells and supergranules, and small-scale photospheric convection (i.e., granulation). The multiscale nature of solar convection is studied using the Void Distribution Function (VDF) calculated using an automatic void-searching algorithm for two-dimensional solar magnetograms. Exponential laws for the VDF as well as two regimes of convection are derived as a function of spatial scale. Our results have ruled out the presence of intrinsic convection scales in the range 5-60 Mm and support the presence of a quasi-continuous spectrum of flows on all scales from granular to global.
- Publication:
-
AGU Fall Meeting Abstracts
- Pub Date:
- December 2012
- Bibcode:
- 2012AGUFMSH51A2191B
- Keywords:
-
- 7500 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY;
- 7524 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY / Magnetic fields;
- 7594 SOLAR PHYSICS;
- ASTROPHYSICS;
- AND ASTRONOMY / Instruments and techniques