Coronal heating by solar braiding

In summary, "solar braiding" is a phenomenon observed in the Sun's corona where magnetic flux elements become highly tangled and eventually release energy through reconnection. This theory was first proposed by astrophysicist Eugene Parker and has now been validated by images from an orbital telescope. Further research suggests that braiding occurs at both large and small scales, with the possibility of self-organization and frequent energy releases.
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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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1. What is coronal heating by solar braiding?

Coronal heating by solar braiding is a process by which the Sun's corona (outer atmosphere) is heated through the twisting and braiding of magnetic field lines.

2. How does solar braiding contribute to coronal heating?

Solar braiding involves the interactions between oppositely directed magnetic fields in the corona, which cause the fields to twist and tangle. This process releases energy in the form of heat, contributing to the overall heating of the corona.

3. Why is coronal heating by solar braiding important?

Coronal heating by solar braiding is important because it helps to explain the surprisingly high temperatures observed in the Sun's corona. This process is thought to be one of the main mechanisms responsible for heating the corona to millions of degrees Celsius.

4. How is coronal heating by solar braiding studied?

Coronal heating by solar braiding is studied through observations of the Sun using instruments such as telescopes and satellites. Scientists also use computer simulations and models to better understand and predict the effects of solar braiding on the corona.

5. What are the potential applications of understanding coronal heating by solar braiding?

Understanding coronal heating by solar braiding can help us better understand and predict space weather events, such as solar flares and coronal mass ejections. This knowledge can also aid in the development of more accurate climate and weather models, as the Sun's activity is closely linked to Earth's atmosphere.

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