Loss of counterstreaming suprathermal electrons on closed heliospheric magnetic flux by pitch-angle scattering

Details Loss of counterstreaming suprathermal electrons on closed heliospheric magnetic flux by pitch-angle scattering Loss of counterstreaming suprathermal electrons on closed heliospheric magnetic flux by pitch-angle scattering

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh31a..07o&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH31A-07

Physics

7511 Coronal Holes, 7513 Coronal Mass Ejections (2101), 7524 Magnetic Fields

Scientific paper

Suprathermal electrons can be used as tracers of magnetic field topology in the heliosphere, with counterstreaming electrons (CSEs) interpreted as a signature of closed magnetic loops (i.e., heliospheric magnetic field lines with both ends rooted at the photosphere). As the apex of a closed loop moves anti-sunward, however, pitch-angle scattering of suprathermal electrons on the increasing field-line length most likely results in eventual loss of the sunward beam and, hence, loss of the CSE signature. To test for the feasibility of this proposed phenomenon, we use a simple numerical model of electron evolution in which electrons undergo adiabatic focusing and pitch-angle scattering. The degree of scattering is a free parameter which is fixed by matching observed properties of suprathermal electron evolution in fast wind associated with open field from coronal holes. We then apply this model to closed loops to determine the how far out into the heliosphere a loop can travel before the CSE signature is lost and discuss the implications for coronal mass ejections.

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