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Capabilities of UV Coronagraphic Spectroscopy for Studying the Source Regions of Solar Energetic Particles and the Solar Wind

John L. Kohl·Steven R. Cranmer·Larry D. Gardner·Jun Lin·John C. Raymond·Leonard Strachan
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Abstract

We summarize the unique capabilities of UV coronagraphic spectroscopy for determining the detailed plasma properties (e.g., density, temperature, outflow speed, composition) of the source regions of both transient phenomena such as CMEs, flares, and solar energetic particles (SEPs) and more time-steady solar wind streams. UVCS/SOHO observations have provided the first detailed diagnostics of the physical conditions of CME plasma in the extended corona. It provided new insights into the roles of shock waves, reconnection, and magnetic helicity in CME eruptions. We summarize past observations and discuss the diagnostic potential of UV coronagraphic spectroscopy for characterizing two possible sites of SEP production: CME shocks and reconnection current sheets. UVCS/SOHO has also led to fundamentally new views of the acceleration region of the solar wind. Understanding the physical processes in this region, which ranges from the low corona (1.1 to 1.5 Rsun) past the sonic points (greater than 5 Rsun), is key to linking the results of solar imaging to in situ particle and field detection. Despite the advances that have resulted from UVCS/SOHO, more advanced instrumentation could determine properties of additional ions with a wider sampling of charge/mass combinations. This would provide much better constraints on the specific kinds of waves that are present as well as the specific collisionless damping modes. Electron temperatures and departures from Maxwellian velocity distributions could also be measured. The instrumentation capable of making the above observations will be described.

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John L. Kohl, Steven R. Cranmer, Larry D. Gardner, Jun Lin, John C. Raymond, Leonard Strachan. 2005-06-21. Capabilities of UV Coronagraphic Spectroscopy for Studying the Source Regions of Solar Energetic Particles and the Solar Wind. https://arxiv.org/abs/astro-ph/0506509

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