<p>Flares involve releasing huge amounts of potential energy that are stored in stressed magnetic structures in the solar corona. So-called reconnection events can release this stress but at the same time accelerate charged particles to high energies. These are trapped along the magnetic field lines, spiralling around them, but travelling until they hit the footpoints of the loop that are anchored in the solar chromosphere and photosphere. The much denser plasma here is sufficient to stop the charged particles and this is where they dump all their kinetic energy, some of which is promptly released in the form of non-thermal hard X-rays, which are insufficient to cool the plasma.</p>

<p>The plasma heats up, increases its pressure and it expands to fill the overlying magnetic structures - a.k.a. chromospheric evaporation. This hot plasma radiates and because it is at temperatures between $10^{5}$ and $10^7$ K, most of that radiation is emitted at EUV and X-ray wavelengths in free-free and transitions in highly ionised species.</p>

<p>I guess the root cause as to why the plasma can get up to these temperatures is that the radiative and conductive cooling processes are much slower than the heating processes caused by the accelerated charged particles.</p>

CC BY-SA 3.0
2016-08-02T18:25:51.953Z
I think you are referring to but not directly stating that the heating is really from thermal (thick target) Bremsstrahlung radiation, right?
honeste_vivere
CC BY-SA 3.0
2016-08-02T20:13:24.350Z
@honeste_vivere the heat is transferred collisionally. Bremsstrahlung is a cooling process that is insufficient to prevent the heating and subsequent expansion of the plasma into the corona.
ProfRob
CC BY-SA 3.0
2016-08-05T14:38:02.930Z
Sorry, I didn't clarify that very well.  I meant that the hard x-rays observed near flare foot points result from thick target Bremsstrahlung emissions, which are effectively high energy Coulomb collisions between the flare-accelerated electrons and the ambient protons/ions in the lower corona, right?
honeste_vivere
CC BY-SA 3.0
2014-12-10T22:41:55.950Z
2016-08-05T16:42:12.210Z
2016-08-05T16:42:12.210Z
ProfRob
<p>During solar flare, electromagnetic energy is released at a wide range of wavelengths but the most dominating are x-rays and extreme ultraviolet rays. Why is that intensity of these wavelengths is greatest?</p>

CC BY-SA 3.0
2014-12-06T19:56:06.743Z
From http://hesperia.gsfc.nasa.gov/hessi/flares.htm
Aaron
<solar-flare><the-sun>
Spectra of electromagnetic radiation emitted during solar flare
seeking_infinity
# Spectra of electromagnetic radiation emitted during solar flare

(Asked by: username_0 on 2014-12-06)

During solar flare, electromagnetic energy is released at a wide range of wavelengths but the most dominating are x-rays and extreme ultraviolet rays. Why is that intensity of these wavelengths is greatest?

**Tags:** solar-flare, the-sun
> **Comments:**
> **username_1**: From http://hesperia.gsfc.nasa.gov/hessi/flares.htm  

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## 1 answers

### Answer by username_2 on 2014-12-10. Score: 3

Flares involve releasing huge amounts of potential energy that are stored in stressed magnetic structures in the solar corona. So-called reconnection events can release this stress but at the same time accelerate charged particles to high energies. These are trapped along the magnetic field lines, spiralling around them, but travelling until they hit the footpoints of the loop that are anchored in the solar chromosphere and photosphere. The much denser plasma here is sufficient to stop the charged particles and this is where they dump all their kinetic energy, some of which is promptly released in the form of non-thermal hard X-rays, which are insufficient to cool the plasma.

The plasma heats up, increases its pressure and it expands to fill the overlying magnetic structures - a.k.a. chromospheric evaporation. This hot plasma radiates and because it is at temperatures between $10^{5}$ and $10^7$ K, most of that radiation is emitted at EUV and X-ray wavelengths in free-free and transitions in highly ionised species.

I guess the root cause as to why the plasma can get up to these temperatures is that the radiative and conductive cooling processes are much slower than the heating processes caused by the accelerated charged particles.

> **Comments:**
> **username_3**: I think you are referring to but not directly stating that the heating is really from thermal (thick target) Bremsstrahlung radiation, right?  
> **username_2**: @honeste_vivere the heat is transferred collisionally. Bremsstrahlung is a cooling process that is insufficient to prevent the heating and subsequent expansion of the plasma into the corona.  
> **username_3**: Sorry, I didn't clarify that very well.  I meant that the hard x-rays observed near flare foot points result from thick target Bremsstrahlung emissions, which are effectively high energy Coulomb collisions between the flare-accelerated electrons and the ambient protons/ions in the lower corona, right?  

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