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Microwave emission from the trapped and precipitated electrons in solar bursts

Microwave emission from the trapped and precipitated electrons in solar bursts. J. E. R. Costa and A. C. Rosal1 2005, A&A, 436, 347. Abstract.

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Microwave emission from the trapped and precipitated electrons in solar bursts

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  1. Microwave emission from the trapped and precipitated electrons in solar bursts J. E. R. Costaand A. C. Rosal1 2005, A&A, 436, 347

  2. Abstract We analyzed the microwave spectra of a sample of 13 solar flares out of 40 events observed by the Nobeyama Radio Polarimeter in the period of August 8, 1998 through November 24, 2001. The solar burst time profiles were filtered to separate the slow component from the fast structures which were associated with the emission from trapped particles and to the emission from the minor precipitating population, respectively. The spectra of both components suggest a trap in a region with a mean magnetic field of about 600 G and a minor emission from the loop legs with a magnetic field of 1100 G, resulting in a mirror ratio of about two. The spectral indices of the optically thin emission from these two regions indicate pitch angle diffusion by Coulomb collisions.

  3. microwave hard X-ray ? Introduction

  4. Non-thermal electrons are accelerated during solar flares as a consequence of an impulsive energy release. The impulsive phase signatures of solar flares in HXR and microwave have been intensively analyzed and support the hypothesis of a common origin based on the emitting electron number and emission time profiles (Kudu 1961).

  5. Energy ⇒ Peak time Time difference in the emission signatures reflect mostly the time scale of diffusion time and/or the time of flight . • The ambient density is in general higher than 1010 electrons/cm3 which results in a collisional deflection time greater than 5s for electrons energies higher than 100 keV. • The collisional deflection time can be tens of seconds for the range of energy relevant for microwave emission (E>100keV). • energy dependence of particle trapping (Coulomb collision) τ= 9.5×107 E1.5/ N (Spitzer, Physics of Fully Ionized Gases)

  6. loss cone angle ; θ= arcsin ( Btop/Bfoot )1/2

  7. ±0 ±0 ±0 ＋2 ＋4 ±0 ＋4 ＋8 ＋2 Energy dependence of HXR time profiles L-band (14-23 keV) M1-band (23-33keV） M2-band (33-53 keV) H-band (53-93 keV)

  8. Energy ⇒ Peak time • The light curves present temporal features with time scale of about one second or less on top of a gradual bulk emission (Kiplinger et al. 1983).

  9. Many authors have worked on the electron kinetic equation to infer the particle number distribution during flares using HXR and/or microwave in trap plus precipitation model. The main weakness resides in the need to make assumptions for the unknown such as; source function time profile and duration of injected electrons, pitch angle distribution and the plasma ambient spatial structure such as density and magnetic field. They propose an analysis based on the B2 dependence of gyro-synchrotron emission of the microwave spectra and the separability of the emission of the fast component from the bulk emission of the gradually increasing number of the trapped electrons. Data analysis • Nobeyama Radio Polarimeter ; Mar. 1998～Dec. 2000 • flux densities higher than 30 sfu. • 　⇒　40 events

  10. Electrons with energy (＞100 keV)would have a time of flight of about one second or less. (Aschwanden 1998) ⇒fast component Trapping times are of the order of tens of seconds for the ambient densities (1011 electrons/cm3) (Trubnikov 1965) ⇒slow component In order to use a filter to separate both components of the observed total flux density, they had to assume that the precipitating electrons do not contribute much to the total emissions during the upper atmosphere part of the electron flight. Due to the strong dependence of the gyro-synchrotron emission on the magnetic field this should be a good first order approximation.

  11. Result ----- Filter The running mean is a better representation of the slow component in order to preserve the original peak time.

  12. Result ----- Inferred magnetic fields They use Ramaty’s code to search for the magnetic field that matches the observed peak. The important parameter for the gyro-synchrotron emission is the viewing angle of the magnetic field lines.

  13. Result ----- Spectral Analysis

  14. Results and discussion • They can observe that the spectral index is higher for the fast component(loop-leg) in 9 out of 13 cases. • mean value is 3.3±0.1 for loop-leg. • mean value is 4.1±0.1 for the loop-legs. • The magnetic fields are also higher in the loop-legs • mean values of 600 G for the loop-top • mean values of 1060 G for the loop-legs The harder spectra at the loop-top favors the hypothesis of Coulomb diffusion of the electron pitch angle in the trap.

  15. This result is not disagreement with Silva et al. (20000) measurements from HXR and microwave.

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