Fine Structure in the Corona at High Latitudes at Solar Maximum

Details Fine Structure in the Corona at High Latitudes at Solar Maximum Fine Structure in the Corona at High Latitudes at Solar Maximum

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001ssrv...97...55s&link_type=abstract

Space Science Reviews, v. 97, Issue 1/4, p. 55-58 (2001).

Physics

Scientific paper

Microstreams and pressure balance structures in fast solar wind were more easily detected at Ulysses at 2.2 AU over the poles than at Helios at 0.3 AU. This is because solar rotation leads to dynamic interactions between different speed regimes at a rate that depends on latitude for the same size features. Dynamic interactions make structures more difficult to detect with increasing distance from the Sun. At solar maximum, Ulysses will sample high latitude solar wind coming from streamers, providing information on fine structure at the tops of streamers and on the source of slow solar wind. Examples are given here of the detectability of various sized structures at Ulysses when it is over the polar regions of the Sun.

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