Density Structure of a Preeruption Coronal Flux Rope

Details Density Structure of a Preeruption Coronal Flux Rope Density Structure of a Preeruption Coronal Flux Rope

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005apj...628.1046k&link_type=abstract

The Astrophysical Journal, Volume 628, Issue 2, pp. 1046-1055.

Astronomy and Astrophysics

Astronomy

12

Sun: Coronal Mass Ejections (Cmes), Sun: Magnetic Fields, Sun: Prominences

Scientific paper

A density model is developed for a coronal flux rope with a specified magnetic field configuration in the noninteracting limit, for which transverse pressure forces can be neglected and flows are rapid enough (>1 km s-1) to invalidate a hydrostatic solution. In the coronal portion of the flux rope, we find that the plasma density is depleted on-axis, where the magnetic field lines are least twisted.

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