Analysis of loop flows observed on 27 March, 1980 by the UVSP instrument during the solar maximum mission

Details Analysis of loop flows observed on 27 March, 1980 by the UVSP instrument during the solar maximum mission Analysis of loop flows observed on 27 March, 1980 by the UVSP instrument during the solar maximum mission

Jul 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...98...91k&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 98, July 1985, p. 91-118. CNR-DOE-supported research.

Astronomy and Astrophysics

Astronomy

15

Coronal Loops, Magnetohydrodynamic Flow, Solar Maximum Mission, Ultraviolet Astronomy, Line Spectra, Steady Flow, Stellar Models, Time Dependence, Unsteady Flow

Scientific paper

The results of an analysis of a set of observations in the C IV 1548 A line obtained on March 27, 1980 by the Solar Maximum Mission Ultraviolet Spectrometer and Polarimeter (UVSP) are presented. The observed region covers an area of 240 x 240 arcsec, and includes a system of bright loops at the limb. Simultaneous spectroheliograms and dopplergrams of the loop region allowed the derivation of empirical velocity and emission-measure profiles on individual loops. These have been compared with the theoretical profiles for: (1) a steady-state loop model with siphon flow, (2) a steady state loop model with downflow in both legs, maintained by continuous mass addition near the loop summit, and (3) a nonsteady loop model with downflow, whereby the initial plasma density decays exponentially with time (similarity solution). None of these simple models is capable of simultaneously representing both the velocity and emission measure profiles; thus a realistic description of cool loop dynamics is lacking. New observations aimed at determining such parameters as the loop lifetime are considered crucial for providing the necessary constraints for future modeling efforts.

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