Cold channels in the accelerating region ?

Details Cold channels in the accelerating region ? Cold channels in the accelerating region ?

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..335g&link_type=abstract

8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel

Astronomy and Astrophysics

Astrophysics

Scientific paper

Channels have been observed up to several AU in Ulysses data (Buttighoffer, 1998) with the property that they conduct keV electrons with almost no diffusion. This has been shown by Buttighoffer et al. (submitted, 1999) to be related to a reduced level of compressive fluctuations, compared to the external plasma outside channels. These channels originate in the solar corona where they have an estimated transverse width of 7000km if projected on the solar surface. We show via numerical simulations of MHD wind in the accelerating region that cold spots in the corona lead to channels with the desired property (reduction of compressive fluctuations) and discuss the implications on the global dynamic of the wind and MHD wave propagation in the corona.

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