Interplanetary Lyman-alpha spectra as a diagnostic of the local interstellar plasma density - The Baranov two-shocks heliosphere case

Details Interplanetary Lyman-alpha spectra as a diagnostic of the local interstellar plasma density - The Baranov two-shocks heliosphere case Interplanetary Lyman-alpha spectra as a diagnostic of the local interstellar plasma density - The Baranov two-shocks heliosphere case

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...396..696l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 396, no. 2, Sept. 10, 1992, p. 696-703. Research supported by CNES.

Astronomy and Astrophysics

Astrophysics

12

Heliosphere, Interplanetary Medium, Interstellar Matter, Lyman Alpha Radiation, Plasma Density, Plasma Diagnostics, Backscattering, Line Spectra, Monte Carlo Method, Proton Density (Concentration), Shock Waves, Solar Wind

Scientific paper

Due to coupling with protons through charge exchange, neutral H atoms from the interstellar medium (ISM) are perturbed when they enter the heliosphere, and flow through the interface between the expanding solar wind and the inflowing ionized component of the ISM. Line profiles of the solar Ly-alpha backscattered emission, reflecting neutral atoms velocity distribution, contain information on the amount of interaction with the plasma. In particular, through the partial differentiation between atoms coming from the stagnation line and the 'sidewind' atoms the 'umbrella effect', if there are variations of the neutral flow velocity and temperature when moving out from the stagnation line, due to the coupling, these variations should be reflected in the line profile directional pattern. This effect is investigated in a quantitative way in the case of the two-shocks heliospheric interface of Baranov et al. (1971, 1982). Neutral velocities and line profiles are calculated by using a Monte Carlo simulation of the H flow through the interface. It is shown that the resulting line-profile upwind/downwind evolution cannot be reproduced by any simple homogeneous model with no interface, and that these measurable differences depend on the ISM proton density.

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