Dips and Waves

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Revision as of 08:29, 23 November 2009

Introduction

Solar flares feature the acceleration of non-thermal particles ofseveral descriptions. One of RHESSI's primary tasks is to study these particles via their [bremsstrahlung] X-rays. The X-ray spectrum typically follows a power law at high energies "hard X-rays", and an exponential at lower "soft X-ray" energies; in the standard interpretation these components reveal (respectively) the primary particle acceleration and its [Maxwellianized] "thermal" heating.The theory of the nonthermal radiation involves several processes: the initial acceleration of the particles, their propagation through the solar atmosphere, and their X-ray production as they lose energy to thebackground plasma.With several assumptions, all of this theory can be wrapped up intoa tractable problem in [inverse theory]. When this was first done at RHESSI's [high spectral resolution], a new and unexpected feature tended to appear: a [dip] in the spectrum at about 30 keV.</p>

There has been some heated discussion (for instance in this earlier Nugget) as to whether this "dip" seen in the mean electron spectrum derived from RHESSI X-ray observations is a real feature. It can often be removed by correcting for the [albedo] flux of X-rays scattered back to the observer from the solar atmosphere beneath the source. But for flares with relatively low thermal mission the standard [thick-target] interpretation says that the dip must be there. The thick-target model only accounts for Coulomb collisions between the propagating beam of accelerated electrons and the background plasma. In this Nugget we present simulation results from our recent paper, where we show what happens to the dip when you also include wave-particle interactions between the beam and the background plasma.

Wave-particle Interactions

In the standard interpretation of RHESSI's hard X-ray emission, a negative powerlaw of accelerated electrons (F₀(E) ~E^-δ₀) above a sharp low energy cutoff leaves the corona travelling down to the chromosphere. As the electrons propagate they lose energy to the background plasma through Coloumb collisions, eventually stopping in the dense chromosphere, where they emit hard X-rays as observed by RHESSI. The collisional energy losses also heat the local plasma, which then expands back upwards along the magnetic field. It can be analytically shown the the resulting mean electron flux spectrum <nVF(E)> will also have a negative power law above the cutoff (<nVF>~E^-δ₁) but will have a positive one (<nVF(E)>~E^δ₁) at low energies. The background plasma appears to have a thermal (Maxwellian) distribution with a mean energy kT well below the energies of the non-thermal electrons. This distribution falls rapidly with energy, and in combination with the positive slope of the low-energy non-thermal electrons results in a local minimum or "dip" in the total mean electron distribution <nVF>.

We have simulated the propagation of such a power law of accelerated electrons, with only Coulomb collisions acting on the beam, as shown in the left panel of Figure 1. But we have also run a second set of numerical simulations in which we include the wave-particle interactions of the beam electrons and the background plasma. Specifically we include beam-driven [Langmuir wave] [turbulence]. We want to include the wave-particle interactions as this non-collisional process may be faster than the Coulomb collision process. Furthermore the development of Langmuir waves from electron beams in solar flares is inferred from radio observations of [type III bursts].

The use the quasi-linear approach describing the resonant interaction between the electrons and Langmuir waves. We follow in time the variation of the electron distribution function f(v,x,t) and, self-consistently, the spectral energy density of the waves W(v,x,t). In Figure 1 we show snapshots from the simulations showing f(v,x,t) for the Coulomb collision simulation (left) and f(v,x,t) and W(v,x,t) for the wave-particle simulation (middle and right panel). A movie of this can also be found here.

Figure 1: The electron distribution f and energy density of the waves W showing the simulation results from the 2 different simulations: Coulomb collisions only on the left; wave-particle interactions on the right.) A movie of this can be found here

The immediate thing that happens is that the wave-particles very quickly flatten the low energy cutoff, producing a plateau in the electron distribution at low energies or velocities. The Coulomb collision alone are far slower at removing the low energy cutoff and produce the expected positive gradient in the electron distribution below the cutoff energy. To calculate the mean electron flux spectrum from our simulations we use the simulated f(v,x,t)/m, spatially integrating and averaging over time. The resulting spectra are shown in Figure 2.

Figure 2: The mean electron flux spectrum <nVF> for the simulation with Coulomb collisions actng on the beam only (left) and the inclusion of wave-particle interaction (right). The black line shows the simulation result, the orange dashed line an overplotted thermal model spectrum. The total spectrum is the dashed green line, indicating the presence of a dip in the Coulomb collision only case.

The positive slope increase in the Coulomb colision only case (left panel Figure 2) is clearly evident in the mean electron spectrum. The wave-particle interactions produce an almost flat, though slighlty negative, spectrum at low energies. With the inclusion of a thermal model spectrum, and using typical parameters for a small flare, we see the appearance of the local minimum or "dip" in the beam-only case. In the beam-and-waves case there is always a negative gradient.

Conclusions

The work shown here is a step towards a more complete treatment of electron transport in solar flares by consideration of wave-particle interactions. The inclusion of such effects goes beyond the traditional propagation theory, which typically relies on Coulomb scattering alone. The wave-particle interactions turn out to flatten any sharp low-energy cutoff in the inital accelerated electron distribution.