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Wednesday, April 22 • 8:30am - 10:30am
Modeling Fast Radio Bursts in Stellar Coronae

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Fast radio bursts are astronomically observed radio frequency bursts which display dispersion, i.e. the speed of propagation is frequency-dependent and higher frequencies are detected before lower frequencies. This dispersion is caused by propagation through plasma, however, the location of this plasma is unknown. One model proposes that the bursts originate as stellar flares from galactic stars and experience dispersion within the coronal plasma present near the star. In addition to the frequency-dependent delay created by plasma dispersion, these flares would also encounter frequency-dependent refraction from the plasma, altering the path-length of the radiation, and hence further shifting the arrival time of different frequencies. An inverse square corona model is used to develop a geometrical treatment of the refraction. Using this treatment, the variation in path length is computed as a function of frequency, given particular physical parameters of the star and the radiation. These calculations will provide a point of comparison between the flare model and the data collected from FRB observations.


Wednesday April 22, 2015 8:30am - 10:30am PDT
Wilma Sherrill Center Concourse

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