Community of European Solar Radio Astronomers – Page 28

Are there Radio-quiet Solar Flares?
by Arnold Benz

2007-01-04

Solar flares accelerate particles, and their distribution is usually non-thermal. Non-thermal electrons are prone to velocity space instabilities driving various plasma waves which, in turn, couple into observable radio waves. Such coherent emissions are the result of the combined action of many electrons organized by kinetic plasma waves and can therefore be extremely efficient. Small coherent radio bursts at the limit of present routine observations emit an energy of some […]

High dynamic range solar radio images by combining visibilities from the Giant Meterwave Radio Telescope and the Nancay Radioheliograph
by Claude Mercier

2006-12-07

We present first results from an ongoing program of combining data from the Nancay Radioheliograph NRH and the Giant Meterwave Radio Telescope GMRT, to produce snapshot images of the Sun at meter wavelengths. The data processing includes a superposition of complex visibilities from NRH and GMRT, a Fourier Transform and a cleaning multi-scale algorithm. We show results from a simulation and an observation of a complex noise storm at 327 […]

Particle acceleration during flares – the part played by an outflow termination shock
by Gottfried Mann

2006-10-11

During solar flares energetic nonthermal electromagnetic radiation up to the gamma-ray range is emitted from the solar atmosphere, implying the generation of accelerated electrons and ions. Particle acceleration in cosmic plasma is of fundamental physical interest. The solar corona offers detailed remote sounding of these processes. A fine example An interesting example is the X17-flare of 28 October 2003, one of the strongest events of the last activity cycle. Figure 1 […]

Coronal shock waves: tracking down the drivers for radio emission
by Silja Pohjolainen

2006-09-21

In the solar corona, shocks are formed when the speed of a disturbance exceeds the local magnetosonic (Alfvén) speed. At low atmospheric heights, above high-density active regions, the Alfvén velocity can drop down to a few hundred km/s, but it then rises steadily to a global maximum of about 1000 km/s near the heliocentric height of 3.5 R (see calculations in Warmuth & Mann 2005). At heights above 1.5 R […]

Radio “crystallography” of the solar corona
by Miroslav Bárta and Marian Karlický

2006-05-10

We suggest a new method for the analysis of fine structures in the cosmic plasma and investigate its applicability for the diagnostics of the solar atmosphere on scales that are not accessible by current observational techniques. The method is based on coherent interaction (diffraction) of radio waves with regular structures – as an example one can consider plasma waves of various kinds, periodic oscillations in the shock-fronts, or even stationary […]

Combining radio and optical observations for coronal magnetic field determination
by Henry Aurass

2006-02-15

We present a method newly developed at the Astrophysikalisches Institut Potsdam (AIP) for determining the structure and the strength of coronal magnetic fields during the late phase of solar flares. Fiber bursts Fiber bursts are a spectral fine structure occuring in some type IV radio burst continua. Here we assume that the fiber bursts are excited by whistler waves and their interaction with nonthermal electrons trapped in a magnetic loop. […]

Instructions on writing a Highlight in Solar Radio Physics aka CESRA nugget

2006-02-02

The Highlight of Solar Radio Physics aka CESRA Nugget allows you to publish fresh research (normally based on a refereed paper published within 3 month) to keep CESRA community informed and up-to-date. These are short communications written in the language accessible to a non-expert in the specific area. The text does not have to be as detailed as a scientific article, but rather written in a more discursive ‘news & […]