Observational constraints on coronal hole density model

Details Observational constraints on coronal hole density model Observational constraints on coronal hole density model

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992esasp.348..109g&link_type=abstract

In ESA, Proceedings of the First SOHO Workshop: Coronal Streamers, Coronal Loops, and Coronal and Solar Wind Composition p 109-1

Astronomy and Astrophysics

Astronomy

2

Coronal Holes, Mathematical Models, Plasma Density, Solar Corona, Astronomical Models, Brightness, Solar Wind, Space Plasmas

Scientific paper

Measuring the polarization brightness (pB) intensity inside a polar coronal hole is an extremely difficult process and the signal to noise ratio is rather low. Under these circumstances, it is sometimes possible to over interpret the data. For example, analysis of white light coronagraph observations of a polar coronal hole during Jun. 29 - Jul. 13 1973 led Munro and Jackson (MJ) to infer that the density inside the hole varied as a function of r (heliocentric north) and theta (colatitude). However, recent analysis of the white light data during Dec. 3 1973 - Jan. 24 1974, indicate that the density inside a polar coronal hole, within limits of uncertainties inherent in the coronal white light observations, is consistent with the interpretation that it is a function of r only. The inherent uncertainties in the observed pB data are discussed and the data from the Munro and Jackson period are reexamined. Results demonstrate that within limits of inherent uncertainty in the polar coronal pB measurements, the density inside a polar coronal hole is independent of magnetic latitude and longitude. The angular width of the coronal hole obtained by MJ is smaller than this study estimated and the divergence is slightly higher than that of MJ. The present model should have significant impact in terms of understanding the hydrodynamic structure of the corona.

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