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Energy release in the solar corona from spatially resolved magnetic braids.

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What can observations tell us about coronal heating?

J T Schmelz1, A R Winebarger2

  • 1Department of Physics, University of Memphis, Memphis, TN 38152, USA jschmelz@memphis.edu.

Philosophical Transactions. Series A, Mathematical, Physical, and Engineering Sciences
|April 22, 2015
PubMed
Summary

The source of coronal heating remains a mystery, but new observations of coronal loops reveal complex structures and hot plasma. These findings challenge existing models and provide crucial data for future theories on solar atmospheric heating.

Keywords:
coronal loopshot plasmasolar corona

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Area of Science:

  • Astrophysics
  • Solar Physics
  • Plasma Physics

Background:

  • The origin of coronal heating is a long-standing enigma in astrophysics.
  • Coronal loops are key structures for understanding solar atmospheric energy transport.
  • Current observatories lack the spatial resolution to directly observe fundamental heating scales.

Purpose of the Study:

  • To investigate the structure, temperature, density, and evolution of coronal loops.
  • To infer information about coronal heating mechanisms through indirect observations.
  • To provide observational constraints for viable coronal heating models.

Main Methods:

  • Analysis of indirect observations of coronal loops.
  • Utilizing data from instruments like the Marshall Grazing Incidence X-ray Spectrometer (testing for hot plasma).
  • Observing magnetic braids untwisting and reconnecting with the High Resolution Coronal Imager.

Main Results:

  • Observed loops with unexpectedly high densities and multi-thermal cross-field temperatures.
  • Identified a hot plasma component (T>5 MK) within coronal loops.
  • Evidence of magnetic braids reconnecting and releasing energy, consistent with plasma heating.

Conclusions:

  • Steady uniform heating models are inconsistent with observed loop properties.
  • Multi-thermal, cooling loops and the presence of hot plasma are critical observational constraints.
  • Future coronal heating models must account for the observed complex dynamics and thermal properties of coronal loops.