Diagnosing the Source Region of a Solar Burst on 26 September 2011 by Using Microwave Type-III Pairs

• Published in: Solar physics 2016-10, Vol.291 (8), p.2407-2418
• Main Authors: Tan, B. L., Karlický, M., Mészárosová, H., Kashapova, L., Huang, J., Yan, Y., Kontar, E. P.
• Format: Article
• Language: English
• Subjects: Acceleration; Astrophysics and Astroparticles; Atmospheric Sciences; Autonomy; Bursting; Detectors; Emission spectroscopy; Gamma ray bursts; Gamma rays; Image processing; Magnetic fields; Microwave communications; Onboard; Physics; Physics and Astronomy; Plasma; Plasma density; Plasmas (physics); Solar energy; Solar flares; Solar instruments; Solar magnetic field; Solar physics; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Space telescopes; Spectrometers; Starbursts; X-ray emissions
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/s11207-016-0986-y

We report a peculiar and interesting train of microwave Type-III pair bursts in the impulsive rising phase of a solar flare on 26 September 2011. The observations include radio spectrometers at frequencies of 0.80 – 2.00 GHz from the Ondřejov radiospectrograph in the Czech Republic (ORSC), hard X-ray from the Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and Gamma-Ray Burst Monitor onboard the Fermi Space Telescope ( Fermi /GRB), EUV images from the Sun Watcher using APS detectors and image Processing instrument onboard the Project for Onboard Autonomy 2 (SWAP/PROBA2), and magnetograms from the Helioseismic and Magnetic Imager onboard the Solar Dynamic Observatory (SDO/HMI). By using a recently developed method (Tan et al. , Res. Astron. Astrophys. 16 , 82, 2016a ), we diagnosed the plasma density, temperature, plasma- β , magnetic field near the source region, the energy of energetic electrons, and the distance between the acceleration region and the emission start sites of Type-III bursts. From the diagnostics, we find that i) The plasma density, temperature, magnetic field, and the distance between the acceleration region and the emission start sites have almost no obvious variations during the period of Type-III pair trains, while the energy of electrons has an obvious peak value that is consistent with the hard X-ray emission. ii) The plasma- β is much higher than unity, showing a highly dynamic process near the emission start site of Type-III bursts. iii) Although the reversed-slope Type-III branches drift more slowly by one order of magnitude than that of the normal Type-IIIs, the related descending and ascending electrons still could have energy of the same order of magnitude. These facts indicate that both the ascending and descending electrons are possibly accelerated by a similar mechanism and in a small source region. These diagnostics can help us to understand the physics in the source region of solar bursts.