Plans for Measuring Coronal O(5+) Outflow Velocities with SPARTAN 201

Details Plans for Measuring Coronal O(5+) Outflow Velocities with SPARTAN 201 Plans for Measuring Coronal O(5+) Outflow Velocities with SPARTAN 201

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.5203s&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #52.03; Bulletin of the American Astronomical Society, Vol. 24, p.815

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Scientific paper

A goal of the Spartan 201 mission is to derive outflow velocities, W, of coronal O(5+) by using a Doppler dimming analysis of the expected resonantly scattered intensities of OVI lambda 1031.9 and lambda 1037.6. The technique is sensitive to velocities in the range 30 < W < 250 km s(-1) and will be used for probing regions of the inner solar corona, between 1.3 and 3.5 Rsun, where significant coronal heating and solar wind acceleration may be occurring. These velocity measurements, when combined with measurements of other plasma parameters (i.e., temperatures and densities of ions and electrons), can be used to estimate the energy and mass fluxes of coronal ions. In particular, it may be possible to locate where the flow changes from subsonic to supersonic and to identify source regions for the high- and low-speed solar wind. The velocity diagnostic technique is discussed with emphasis placed on the requirements needed for accurate outflow velocity determinations. Model calculations of outflow velocities based on expected detector count rates are also presented. This work is supported by NASA under Grant No. NAG5-613 to the Smithsonian Astrophysical Observatory.

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