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Convection-driven generation of ubiquitous coronal waves View all abstracts by submitter

Markus J Aschwanden   Submitted: 2019-06-13 09:46

We develop a new method to measure the 3-D kinematics of the sub-photospheric motion of magnetic elements, which is used to study the coupling between the convection-driven vortex motion and the generation of ubiquitous coronal waves. We use the method of decomposing a line-of-sight magnetogram from HMI/SDO into unipolar magnetic charges, which yields the (projected) 2-D motion [x(t), y(t)] and the (half) width evolution w(t) of an emerging magnetic el- ement, from an initial depth of d <∼ 1500 km below the photosphere. A simple model of rotational vortex motion with magnetic flux conservation during the emergence process of a magnetic ele- ment predicts the width evolution, i.e., w(t)/w0 = [B(t)/B0]-1/2, and an upper limit of the depth variation d(t) ≤ 1.3 w(t). While previous 2-D tracing of magnetic elements provided information on advection and super-diffusion, our 3-D tracing during the emergence process of a magnetic element is consistent with a ballistic trajectory in upward direction. From the estimated Poynt- ing flux and life times of convective cells we conclude that the CoMP-detected low-amplitude transverse MHD waves are generated by the convection-driven vortex motion. Our observational measurements of magnetic elements appear to contradict the theoretical random-walk braiding scenario of Parker (1983, 1988).

Authors: Aschwanden,M.J., Gosic,M., Hurlburt,N.E., and Scullion,E.
Projects: SDO-HMI

Publication Status: ApJ 866, 72 (13pp)
Last Modified: 2019-06-15 17:41
Go to main E-Print page  Order out of randomness: Self-organization processes in astrophysics  The minimum energy principle applied to Parker's coronal braiding and nanoflaring scenario  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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