Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusmsh31a..03g&link_type=abstract
American Geophysical Union, Spring Meeting 2009, abstract #SH31A-03
Astronomy and Astrophysics
Astronomy
6954 Radio Astronomy, 6964 Radio Wave Propagation, 7534 Radio Emissions
Scientific paper
A new technique for the localization of the radio burst sources in the corona and interplanetary medium is presented. This technique uses the property of the medium, which permits the emission to escape the source as the direct and reflected signals along two different trajectories. Since the reflected signal (echo) travels closer to the center of the sun than the direct signal, it undergoes severe refraction, attenuation, and group delay. This leads to the different arrival directions, arrival times, and intensities. Both the direct and the echo signals can be detected by a single spacecraft as a superposition, as well as by a widely separated twin spacecraft as two distinct signals. By computing the trajectories of the direct and reflected rays, their escape angles and excess path lengths are obtained. The direct and reflected emission peaks corresponding to a type III radio burst have been identified in the data obtained by the spacecraft 'A' and 'B' of the STEREO mission, which were separated from each other by 42 degrees. By comparing the computed values with the angular separation of the spacecraft, the observed intensity ratios and the time delays, the emission source of this type III event is localized for three cases: (1) the mode of emission is unknown, (2) the mode of emission is the second harmonic, and (3) the mode of emission is the fundamental. The correction due to scattering is also provided. This method has a potential to predict the arrival times and arrival locations of the space weather critical CME shocks at 1 AU.
Golla T.
MacDowall R.
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