Multiple flows in the solar transition region

Details Multiple flows in the solar transition region Multiple flows in the solar transition region

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.346..211b&link_type=abstract

In ESA, Study of the Solar-Terrestrial System p 211-216 (SEE N93-31674 12-90)

Computer Science

9

Boundary Layer Transition, Chromosphere, Fine Structure, Solar Corona, Sunspots, Transition Flow, Ultraviolet Spectra, Data Reduction, Flow Velocity, High Resolution

Scientific paper

Observations of the solar transition region between the chromosphere and the corona using the High Resolution Telescope and Spectrograph (HRTS) are addressed. The HRTS is described together with the data reduction and calibration. The derivation of line profiles is considered. The solar transition region shows clear evidence of a fine scale structure that is much smaller than the best available instrumental resolution in the UV of 1 by 1 arcsec. Previous studies have suggested filling factors of 0.01 to 0.001, with the solar gas being restricted to thin extended fibrills. New evidence of the fine scale structure is found from its dynamical characteristics, the presence of multiple flows. In multiple flows, the solar gas in small volumes shows several distinct velocities, resulting in line profiles with more than one velocity component within the spatial resolution element. Multiple velocities are particularly prominent above sunspots, but by no means restricted to these regions. Instead they are clearly a general feature in the solar transition region, occurring in quiet as well as active regions. The observation of multiple velocities makes it clear that the transition region can no longer be regarded as static or even as stationary.

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