MHD Simulation and Physical Observations Support the Zero-IMF, Extended-Tail Theorem

Details MHD Simulation and Physical Observations Support the Zero-IMF, Extended-Tail Theorem MHD Simulation and Physical Observations Support the Zero-IMF, Extended-Tail Theorem

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm11b0825w&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM11B-0825

Physics

2744 Magnetotail

Scientific paper

An extended-tail solution for the magnetosphere in the classical Chapman/Ferraro/Parker field-free (zero-IMF), finite temperature solar wind was first postulated by the author in the 1960s. Since then, a number of developments have lent support to this suggestion. First, a zero-IMF MHD simulation showed the development of an extended tail (to the limits of the study). In addition, two (alternating) types of plasmoids in the near tail were seen, the well-known plasmoids along the midnight6 meridian associated with substorms, and intermediate plasmoids along the flanks (which are probably associated with the transfer of formerly closed field lines back into the tail along the flanks). Second, recent physical studies show a statistical asymmetric enhancement of plasma injection along the dawn flank. Since the extended-tail solution contains such an asymmetric injection mechanism (the gradient-drift effect), this physical observation may also support the extended-tail theorem.

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