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New Evidence that Magnetoconvection Drives Solar-Stellar Coronal Heating View all abstracts by submitter

Sanjiv Tiwari   Submitted: 2017-06-28 12:52

How magnetic energy is injected and released in the solar corona, keeping it heated to several million degrees, remains elusive. Coronal heating generally increases with increasing magnetic field strength. From comparison of a non-linear force-free model of the three-dimensional active-region coronal field to observed extreme-ultraviolet loops, we find that (1) umbra-to-umbra coronal loops, despite being rooted in the strongest magnetic flux, are invisible, and (2) the brightest loops have one foot in an umbra or penumbra and the other foot in another sunspot?s penumbra or in unipolar or mixed-polarity plage. The invisibility of umbra-to-umbra loops is new evidence that magnetoconvection drives solar-stellar coronal heating: evidently the strong umbral field at both ends quenches the magnetoconvection and hence the heating. Broadly, our results indicate that, depending on the field strength in both feet, the photospheric feet of a coronal loop on any convective star can either engender or quench coronal heating in the loop?s body.

Authors: Sanjiv K. Tiwari, Julia K. Thalmann, Navdeep K. Panesar, Ronald L. Moore, Amy R. Winebarger
Projects: SDO-AIA,SDO-HMI

Publication Status: ApJ Letters, in press
Last Modified: 2017-06-29 12:34
Go to main E-Print page  Heating of an erupting prominence associated with a solar coronal mass   ejection on 2012 January 27  Beam electrons as a source of Hα flare ribbons  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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