Other
Scientific paper
Sep 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.535..841r&link_type=abstract
In: Solar variability as an input to the Earth's environment. International Solar Cycle Studies (ISCS) Symposium, 23 - 28 June 2
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Solar Radio Bursts, Solar Particle Acceleration
Scientific paper
An important problem of solar physics is the acceleration and transport of energetic particles (e.g., protons and electrons) produced during solar energetic processes, such as flares and coronal mass ejections (CMEs). One of the difficulties with solar particle observations is that they are made far from the Sun (usually at 1 AU). Extrapolating such in-situ observations back to an origin on the Sun is very difficult and involves many uncertainties. On the other hand, solar radio emissions, such as type II and type III bursts and decimeter/microwave emissions, are believed to be signatures of the acceleration of solar electrons. Since these radio emissions are observed remotely, they can facilitate tracing the signatures of solar energetic particles back to their solar origin, as well as providing information on the location of the acceleration regions in the corona. However, comparisons of these remote radio observations with in-situ particle observations have suggested that the acceleration and/or transport of solar energetic particles may be more complex than previously expected. For example, recent analyses suggest that there may be different classes of solar proton and electron events in the corona that may involve very different acceleration times, different acceleration locations, and different acceleration mechanisms, even for the same solar event. In this paper I will review some aspects of how the remotely observed solar radio emissions and in-situ particle observations are challenging our views of the acceleration and transport of energetic particles from the Sun.
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