@Article{SubramanianWhKaSySaAn:2007:ElAcPo,
               author = "Subramanian, P. and White, S. M. and Karlick{\'y}, M. and Sych, 
                         R. and Sawant, Hanumant Shankar and Ananthakrishnan, S.",
          affiliation = "{Indian Institute of Astrophysics} and {Department of Astronomy. 
                         University of Maryland} and {Astronomical Institute of the Academy 
                         of Sciences of the Czech Republic} and Institute of Solar 
                         Terrestrial Physics, Siberian Branch of the Russian Academy of 
                         Sciences (ISTP) and {Instituto Nacional de Pesquisas Espaciais 
                         (INPE)} and National Centre for Radio Astrophysics, Tata Institute 
                         of Fundamental Research, Pune University Campus",
                title = "Electron acceleration in a post-flare decimetric continuum 
                         source",
              journal = "Astronomy \& Astrophysics",
                 year = "2007",
               volume = "468",
               number = "3",
                pages = "1099--1102",
                month = "June",
             keywords = "acceleration of particles, plasmas, Sun : radio radiation, Sun : 
                         corona, Sun : flares, SOLAR RADIO-EMISSION, PLASMA-EMISSION, 
                         CONSTRAINTS.",
             abstract = "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 (similar to 10(9) 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 3 x 
                         10(25)-10(26) erg/s. The efficiency of the overall plasma emission 
                         process starting from electron acceleration and culminating in the 
                         observed emission could range from 2.87 x 10(-9) to 2.38 x 
                         10(-8).",
           copyholder = "SID/SCD",
                 issn = "0004-6361 and 1432-0746",
             language = "en",
           targetfile = "electron acceleration.pdf",
        urlaccessdate = "20 maio 2024"
}