@Article{SawantLattBenzDenn:1990:HaXrAs,
               author = "Sawant, Hanumant Shankar and Lattari, C. J. B. and Benz, A. O. and 
                         Dennis, B. R",
                title = "Hard X-rays associated weak decimetric bursts",
              journal = "Solar Physics",
                 year = "1990",
               volume = "130",
               number = "1-2",
                pages = "57--73",
             keywords = "ASTROFISICA.",
             abstract = "In previous attempts to show one-to-one correlation between type 
                         III bursts and X-ray spikes, there have been ambiguities as to 
                         which of several X-rays spikes are correlated with any given type 
                         III burst. Here, we present observations that show clear 
                         associations of X-ray bursts with RS type III bursts between 16:46 
                         UT and 16:52 UT on July 9, 1985. The hard X-ray observations were 
                         made at energies above 25 keV with HXRBS on SMM and the radio 
                         observations were made at 1.63 GHz using the 13.7 m Itapetinga 
                         antenna in R and L polarization with a time resolution of 3 ms. 
                         Detailed comparison between the hard X-ray and radio observations 
                         shows: (1) In at least 13 cases we can identify the associated 
                         hard X-ray and decimetric RS bursts. (2) On average, the X-ray 
                         peaks were delayed from the peak of the RS bursts at 1.6 GHz by 
                         400 ms although a delay as long as 1 s was observed in one case. 
                         One possible explanation of the long delays between the RS bursts 
                         and the associated X-ray is that RS bursts is produced at the 
                         leading edge of the electron beam, whereas the X-ray burst peaks 
                         at the time of arrival of the bulk of the electrons at the high 
                         density region at the lower corona and upper chromosphere. Thus, 
                         the time comparison must be made between the peak of the radio 
                         pulse and the start of the X-ray burst. In that case the delays 
                         are consistent with an electron travel time with velocity 0.3 c 
                         from the 800 MHz plasma level to the lower corona assuming that 
                         the radio emission is at the second harmonic.",
                 issn = "0038-0938 and 1573-093X",
                label = "2958",
           targetfile = "5096.pdf",
        urlaccessdate = "10 maio 2024"
}