The role of high resolution observations in determining energy release and transport processes

Details The role of high resolution observations in determining energy release and transport processes The role of high resolution observations in determining energy release and transport processes

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986sfcp.nasa..139s&link_type=abstract

In NASA. Marshall Space Flight Center Solar Flares and Coronal Physics Using P/OF as a Research Tool p 139-141 (SEE N86-24614

Physics

Energy Transfer, High Resolution, Solar Flares, Solar Maximum Mission, Solar X-Rays, Transport Properties, Conduction Electrons, Laser Fusion, Spatial Resolution

Scientific paper

With present observations from the Solar Maximum Mission, we are seeing a very selective sample of spatially large flares in the soft part (10 to 50 keV) of the hard X-ray spectrum. The spatial resolution is at best 5600 km with a corresponding time resolution of 4.5 s for adequate count statistics. This resolution gives rise to the following problems: We cannot resolve the minor radii of the loops involved or tell where and how the energy release occurs. The manner in which loops interact and the relationship between the soft and hard or approx 00 keV) parts of hard X-rays remains elusive. We cannot see how energy propagates in most cases. Thus it is desirable to determine the minimum increase in spatial and temporal resolution required to solve these problems. Spatially we need to resolve the minor radius of a small loop which is about 800 km or 1 arc s. Upper limits to observed speeds of conduction fronts and shocks are approx km/s with theoretical limits running about a factor of 2 higher. Thus, a compatible minimum time resolution is in the range of 0.2 to 0.4 s. With these spatial and temporal resolutions, sufficient count statistics are required to go up to approx 120 keV with a sufficient number of energy bands to obtain spectra.

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