Solar Physics

, Volume 98, Issue 1, pp 91–118 | Cite as

Analysis of loop flows observed on 27 March, 1980 by the UVSP instrument during the Solar Maximum Mission

  • R. A. Kopp
  • G. Poletto
  • G. Noci
  • M. Bruner
Article
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Abstract

In this paper we present the results of an analysis of a set of observations in the C iv 1548 Å line obtained on 27 March, 1980 by the Solar Maximum Mission Ultraviolet Spectrometer and Polarimeter (UVSP). The observed region covers an area of 240 × 240 arc sec and includes a system of bright loops at the limb. Simultaneous spectroheliograms and dopplergrams of the loop region allowed us to derive empirical velocity and emission-measure profiles on individual loops. These have been compared with the theoretical profiles for: (i) a steady-state loop model with siphon flow, (ii) a steady state loop model with downflow in both legs maintained by continuous mass addition near the loop summit, (iii) a non-steady 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 we still lack a realistic description of cool loop dynamics. New observations aimed at determining such parameters as the loop lifetime are considered crucial for providing the necessary constraints for future modeling efforts.

Keywords

Emission Measure Loop Model Initial Plasma Continuous Mass Loop Flow 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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Copyright information

© D. Reidel Publishing Company 1985

Authors and Affiliations

  • R. A. Kopp
    • 1
  • G. Poletto
    • 2
  • G. Noci
    • 3
    • 4
  • M. Bruner
    • 5
  1. 1.Inertial Fusion and Plasma Theory GroupLos Alamos National LaboratoryLos AlamosUSA
  2. 2.Osservatorio Astrofisico di ArcetriFirenzeItaly
  3. 3.Istituto di AstronomiaUniversità di PadovaPadovaItaly
  4. 4.Osservatorio Astrofisico di ArcetriFirenzeItaly
  5. 5.Lockheed Palo Alto Research LaboratoryPalo AltoUSA

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