Coronal plumes and final scale structure in high speed solar wind streams

Details Coronal plumes and final scale structure in high speed solar wind streams Coronal plumes and final scale structure in high speed solar wind streams

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ssrv...70..391v&link_type=abstract

Space Science Reviews, Volume 70, Issue 1-2, pp. 391-396

Computer Science

19

Solar Wind, Coronal Plumes

Scientific paper

We present a solar wind model which takes into account the possible origin of fast solar wind streams in coronal plumes. We treat coronal holes as being made up of essentially 2 plasma species, denser, warmer coronal plumes embedded in a surrounding less dense and cooler medium. Pressure balance at the coronal base implies a smaller magnetic field within coronal plumes than without. Considering the total coronal hole areal expansion as given, we calculate the relative expansion of plumes and the ambient medium subject to transverse pressure balance as the wind accelerates. The magnetic flux is assumed to be conserved independently both within plumes and the surrounding coronal hole. Magnetic field curvature terms are neglected so the model is essentially one dimensional along the coronal plumes, which are treated as thin flux-tubes. We compare the results from this model with white-light photographs of the solar corona and in-situ measurements of the spaghetti-like fine-structure of high-speed winds.

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