Physics – Optics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh31d07d&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SH31D-07 INVITED
Physics
Optics
7509 Corona, 7519 Flares, 7546 Transition Region, 7549 Ultraviolet Emissions, 7594 Instruments And Techniques
Scientific paper
The development of high spectral resolution solar spectroscopy has occurred in three main steps: (1) The Exploration of the Solar Spectrum (spectral line identifications, determining atomic energy levels of solar abundant ions), (2) The Spectrum as a Tool for Solar Physics (understanding atomic processes in hot plasmas and developing plasma diagnostics useful for solar physics), and, (3) Imaging Spectroscopy (applying well-developed plasma diagnostic techniques to individual structures in the solar atmosphere with simultaneous high spatial and temporal resolution). Due to technological advances such as multilayer optics and the development of CCDs for extreme-ultraviolet wavelength regions, high resolution imaging spectroscopy is now on the threshold of providing key information for testing theories of coronal heating and the mechanisms of solar activity. Apart from providing detailed information on solar element abundances, electron and ion temperatures, electron densities and filling factors, high resolution solar spectroscopy provides unambiguous information on the dynamics of individual solar structures through measurements of Doppler effects in the profiles of spectral emission lines. And it is the dynamics that provide key tests for coronal heating and solar activity theories involving physical processes such as magnetic reconnection and wave heating. In this talk I will discuss how a new generation of imaging spectrometers should provide breakthroughs in our understanding of many of the major problems of the solar atmosphere. This work was supported by NASA and NRL/ONR
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