Type III-L Solar Radio Bursts and Their Associations with Solar Energetic Proton Events

Details Type III-L Solar Radio Bursts and Their Associations with Solar Energetic Proton Events Type III-L Solar Radio Bursts and Their Associations with Solar Energetic Proton Events

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21632106d&link_type=abstract

American Astronomical Society, AAS Meeting #216, #321.06; Bulletin of the American Astronomical Society, Vol. 41, p.912

Astronomy and Astrophysics

Astronomy

Scientific paper

Type III-L bursts are a sub-class of type III solar radio bursts that tend to occur after the impulsive phase of flares; are longer in duration than individual type IIIs and tend to be low-frequency. There has been a proposal that type III-Ls are connected to solar energetic proton (SEP) events. Most work on this connection has started from samples of SEP events, but if type III-Ls are to be useful for prediction of SEP events, then we need to understand the properties of samples of type III-L bursts. This talk reports preliminary results from such a study. An operating definition based on previous work is used to identify type III-L events amongst M- and X-class flares from 2001; and then associations with other properties of these events are investigated, including association with SEP events. If there is an association with SEP events, one important factor that these bursts allow us to address is the question of whether acceleration takes place at an associated CME, or closer to the flare site well below the CME. Work has been developed on a type III fitting tool. A Template is chosen from a representative individual type III burst and fit to individual type III bursts and components of Complex type III bursts in order to help analyze and distinguish these bursts. This type III fitting tool can also be used to fit and distinguish Impulsive type III and type III-L bursts and help analyze various characteristics of the components of these bursts such as drift-rate and change in the duration of their intensity-time profiles with frequency.
Funding for this research came from the Naval Research Laboratory where basic research in radio astronomy is funded by the Office of Naval Research, and from NASA LWS Grant FRS 526249.

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