Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007a%26a...465..613s&link_type=abstract
Astronomy and Astrophysics, Volume 465, Issue 2, April II 2007, pp.613-619
Astronomy and Astrophysics
Astrophysics
5
Sun: Flares, Sun: Corona, Sun: Radio Radiation
Scientific paper
Aims:We study the solar flare on 28 August 1999 observed by the Nobeyama Radioheliograph at 17 and 34 GHz and analyze the unusual behavior of microwave source (a coronal loop) after injections of high-energy electrons. The observations reveal a propagation velocity of the emission front along the loop of about 104 km s-1, which is 30 times less than the velocity of high-energy electrons generating gyrosynchrotron emission at 17 and 34 GHz. The main goal is to understand the physical origin of this electron propagation. Methods: We interpret this anomalous propagation in terms of the collective effects of relativistic electrons interacting with plasma turbulence. A cloud of highly energetic electrons responsible for microwave emission generates low-frequency whistler waves, and a turbulent "wall" in the loop is formed. Results: The electrons undergo strong resonant scattering due to wave-particle interaction, and the emission front propagates with the wave phase velocity, which is much lower than the particle velocity.
Melnikov Victor F.
Shibasaki Kazuo
Stepanov Alexander V.
Yokoyama Tadashi
No associations
LandOfFree
Turbulent propagation of high-energy electrons in a solar coronal loop does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Turbulent propagation of high-energy electrons in a solar coronal loop, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Turbulent propagation of high-energy electrons in a solar coronal loop will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1679803