Heliospheric interface filtration of the interstellar hydrogen

Details Heliospheric interface filtration of the interstellar hydrogen Heliospheric interface filtration of the interstellar hydrogen

Jun 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aipc..471..803i&link_type=abstract

The solar wind nine conference. AIP Conference Proceedings, Volume 471, pp. 803-806 (1999).

Physics

Interplanetary Physics, Atomic, Molecular, And Chemical, And Grain Processes

Scientific paper

In this paper we have used a kinetic model of the flow of interstellar atoms with updated values of velocity, temperature and density of the circumsolar interstellar cloud, and calculated how quantities which are directly associated to the observations vary as a function of the interstellar proton number density np,LIC. These quantities are the degree of filtration, the temperature and the velocity of the interstellar H-atoms in the inner heliosphere, the distances to the bow shock (BS), heliopause (HP) and termination shock (TS), and the plasma frequencies in the LIC, at the BS and in the maximum compression region around the heliosphere which constitutes the ``barrier'' for radio waves formed in the interstellar medium. Comparing the model results with pick up ion data, Ly-α measurements, and low-frequencies radio emissions, we have searched for a number density of protons in the LIC compartible with all observations. We find it difficult in the frame of this model without interstellar magnetic field to reconcile the distance to the shock and the heliopause deduced from time-delay of the radio emissions with other diagnostics and discuss possible explanations for these discrepancies. We also conclude that, on the basis of this model, the most likely value for the proton density in the LIC is in the range 0.04 cm-3

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