The Heliopause: Structure, Stability, and Temporal Response to Disturbances

Details The Heliopause: Structure, Stability, and Temporal Response to Disturbances The Heliopause: Structure, Stability, and Temporal Response to Disturbances

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh14a..04z&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH14A-04

Physics

[2124] Interplanetary Physics / Heliopause And Solar Wind Termination

Scientific paper

The next major boundary to be discovered by the Voyager 1 and 2 spacecraft is probably the heliopause. From a continuum fluid perspective, the existence of a boundary separating interplanetary and interstellar gas is a necessary structure, and in the classical magnetized fluid description, the heliopause should be a contact or tangential discontinuity with no flow across the boundary. Such structures are commonly studied at magnetized planets in the form of planetary magnetopauses. Related structures exist at non-magnetized bodies such as Mars and comets. The heliopause however is complicated by the presence of magnetic fields and interstellar neutral hydrogen (H), which traverses the boundary between interplanetary and interstellar plasma. The back-reaction of neutral H undoubtedly modifies the boundary regions and there are suggestions based on simulations and theory that the heliopause may itself be modified by such charge-exchange couplings. We shall discuss the structure of the heliopause based on expectations from simulations. We shall consider the stability of the heliopause, and its response to interplanetary disturbances.

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