Volume 468, Number 3, June IV 2007Extended baselines for the IRAM Plateau de Bure interferometer: First results
|Page(s)||1099 - 1102|
|Published online||24 April 2007|
Electron acceleration in a post-flare decimetric continuum source
Indian Institute of Astrophysics, Bangalore 560034, India e-mail: email@example.com
2 Dept. of Astronomy, University of Maryland, College Park, MD 20742, USA e-mail: firstname.lastname@example.org
3 Astronomical Institute of the Academy of Sciences of the Czech Republic, 25165 Ondřejov, Czech Republic e-mail: email@example.com
4 Institute of Solar Terrestrial Physics, Siberian Branch of the Russian Academy of Sciences (ISTP), PO Box 4026, Irkutsk 33, 664033, Russia e-mail: firstname.lastname@example.org
5 Instituto Nacional de Pesquisas Espaciais, 515, 12201-970, San Jose Dos Campos, SP, Brazil e-mail: email@example.com
6 National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, PO Bag 3, Ganeshkhind, Pune 411007, India e-mail: firstname.lastname@example.org
Accepted: 23 March 2007
Aims.To calculate the power budget for electron acceleration and the efficiency of the plasma emission mechanism in a post-flare decimetric continuum source.
Methods.We have imaged a high brightness temperature (∼109 K) post-flare source at 1060 MHz with the Giant Metrewave Radio Telescope (GMRT). We use information from these images and the dynamic spectrum from the Hiraiso spectrograph together with the theoretical method described in Subramanian & Becker (2006, Sol. Phys., 237, 185) to calculate the power input to the electron acceleration process. The method assumes that the electrons are accelerated via a second-order Fermi acceleration mechanism.
Results.We find that the power input to the nonthermal electrons is in the range –1026 erg/s. The efficiency of the overall plasma emission process starting from electron acceleration and culminating in the observed emission could range from to .
Key words: acceleration of particles / plasmas / Sun: radio radiation / Sun: corona / Sun: flares
© ESO, 2007
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