Coronal heating by solar braiding

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SUMMARY

The phenomenon of "solar braiding," validated by images from orbital telescopes, explains how the Sun's corona achieves high temperatures. This theory, known as "Parker Braiding" after astrophysicist Eugene Parker, has been observed after 30 years of speculation. The Parker model suggests that the heating of the solar corona is due to the reconnection of braided magnetic flux elements, which occurs at various scales, including those observable by TRACE and Hinode. The study highlights the self-organized critical state of braided magnetic fields and the power-law distributions governing energy release during reconnection.

PREREQUISITES
  • Understanding of solar physics and coronal structures
  • Familiarity with magnetic reconnection processes
  • Knowledge of observational tools like TRACE and Hinode
  • Basic grasp of power-law distributions in physical systems
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  • Research the mechanisms of magnetic reconnection in solar physics
  • Explore the observational capabilities of TRACE and Hinode telescopes
  • Study the implications of self-organized criticality in astrophysical contexts
  • Investigate the role of energy release in coronal heating processes
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Astrophysicists, solar physicists, and researchers interested in solar corona dynamics and magnetic field interactions.

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Coronal heating by "solar braiding"

How the Sun's Corona Gets So Hot
The phenomenon of "solar braiding," hypothesized 30 years ago, has now been validated by images from an orbital telescope.
http://discovermagazine.com/2013/september/06-understanding-suns-energy

. . . .
Solar braiding is also known as “Parker Braiding” after Eugene Parker, the astrophysicist credited with weaving the theory together, Cirtain says. Parker, 86 and retired, says it’s gratifying that his 30-year-old theory has finally been observed. “I always hoped the resolution would creep up on this thing,” Parker says. . . .

NASA Telescope Observes How Sun Stores and Releases Energy
http://www.nasa.gov/home/hqnews/2013/jan/HQ_13-030_Hi-C_Sun_Energy.html


SELF-ORGANIZED BRAIDING AND THE STRUCTURE OF CORONAL LOOPS
http://iopscience.iop.org/0004-637X/705/1/347/fulltext/apj_705_1_347.text.html
http://iopscience.iop.org/0004-637X/705/1/347/pdf/0004-637X_705_1_347.pdf
Abstract: The Parker model for heating of the solar corona involves reconnection of braided magnetic flux elements. Much of this braiding is thought to occur at as yet unresolved scales, for example, braiding of threads within an extreme-ultraviolet or X-ray loop. However, some braiding may be still visible at scales accessible to TRACE or Hinode. We suggest that attempts to estimate the amount of braiding at these scales must take into account the degree of coherence of the braid structure. In this paper, we examine the effect of reconnection on the structure of a braided magnetic field. We demonstrate that simple models of braided magnetic fields which balance the input of topological structure with reconnection evolve to a self-organized critical state. An initially random braid can become highly ordered, with coherence lengths obeying power-law distributions. The energy released during reconnection also obeys a power law. Our model gives more frequent (but smaller) energy releases nearer to the ends of a coronal loop.
 
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