UV Spectro-Coronagraphic Observations of Solar Energetic Particle Related Phenomena
Abstract
One of the most difficult problems in space weather is the prediction of Solar Energetic Particles (SEPs). New theoretical models are providing information about the precise source region of the energetic particles. NRL has developed concepts for a new generation of instruments to provide new insights into energetic particle-producing Coronal Mass Ejections (CMEs) and the associated shocks as they traverse the corona and enter the solar wind. This understanding of SEP shocks is directly relevant for Space Weather prediction as they uniquely define the source regions for geo-effective events. Specifically, the empirical characterization of the coronal pre-shock/shock conditions and the ambient solar wind properties can be directly used as inputs for shock propagation and SEP acceleration models. Such observations on real events are required to provide constraints on a comprehensive predictive SEP model. These new UV spectro-coronagraphs will observe the non-thermal characteristics of energetic particle-producing CMEs traversing the corona and inner heliosphere. Particle acceleration at CME shock fronts is a leading candidate for the production of SEP events. UVSC will demonstrate that the site of SEP acceleration can be identified and measure critical parameters in pre- and post-shock coronal plasmas including suprathermal seed particle populations. When combined with an integrated theory and modeling program, these measurements will be used to significantly advance our fundamental understanding of energetic particle acceleration. Ultimately this understanding will be used to develop a predictive capability for the flux, energy spectrum, and composition of SEPs and uniquely obtain the observations required to test the basis for an unprecedented breakthrough in the prediction of SEP events. The instruments will detect the generation of suprathermal particle populations above the threshold necessary for efficient acceleration by shocks associated with high speed CMEs by providing sufficient throughput to detect high energy tails in the profiles of H I, He II and O VI. The non-thermal component detected in the UV/EUV spectra will indicate the presence of a population of seed particles that can be further accelerated in SEP events.
- Publication:
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AGU Spring Meeting Abstracts
- Pub Date:
- May 2008
- Bibcode:
- 2008AGUSMSP43A..07N
- Keywords:
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- 7513 Coronal mass ejections (2101);
- 7514 Energetic particles (2114);
- 7594 Instruments and techniques;
- 7845 Particle acceleration;
- 7974 Solar effects