Structure of flow near heliopause stagnation point

Details Structure of flow near heliopause stagnation point Structure of flow near heliopause stagnation point

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..547b&link_type=abstract

TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 547-550 (2010).

Other

Solar Wind, Interstellar Matter, Flow Instability, Particle Emission, Solar Wind, Interstellar Dust Grains, Diffuse Emission, Infrared Cirrus, Instability Of Shear Flows

Scientific paper

We study the flow in the vicinity of the heliopause stagnation point. The medium is considered as two-component, with one component being plasma and the other the H atoms. The plasma and H atoms interact through charge exchange. It is assumed that the H atom flow has constant velocity, density and temperature, so that the back reaction of the plasma flow on the H atom flow is neglected. The solution is obtained in the form of power series expansions with respect to the radial distance from the symmetry axis. The main result obtained in our analysis is that the heliopause is not a surface of discontinuity, at least in a vicinity of the stagnation point. Rather it is the surface separating the flows of the solar wind and interstellar medium with all flow parameters continuous at this surface.

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