Hostname: page-component-8448b6f56d-m8qmq Total loading time: 0 Render date: 2024-04-19T15:01:23.424Z Has data issue: false hasContentIssue false
  • English
  • Français

Broadening of the Interplanetary Helium Cone Structure Due to Elastic Collisions of LISM Helium Atoms with Solar Wind Ions

Published online by Cambridge University Press:  12 April 2016

Hans J. Fahr ,
Hans U. Nass  and
Daniel Rucinski
Hans J. Fahr
Affiliation:
Institut für Astrophysik der Universität Bonn
Hans U. Nass
Affiliation:
Institut für Astrophysik der Universität Bonn
Daniel Rucinski
Affiliation:
Space Research Center of Polish Academy of Sciences, Warsaw

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Neutral interstellar particles penetrating into the heliosphere, besides being subject there to specific loss processes, suffer elastic collisions with KeV-solar wind ions. The momentum transfer to the neutrals connected with these collisions leads to a loss of angular momentum with respect to the sun and to a fractional compensation of the effective solar gravity. The dynamical particle trajectories hence are changed into non-Keplerians leading to density and temperature distributions differing from those calculated in the past. This is found from a solution of the Boltzmann equation that linearizes the effect of this additional force. It is shown here that the HeI-584A resonance glow of the heliospheric helium cone lead to substantially lower interstellar helium temperatures if re-interpreted on the basis of this revised theory. These temperatures now seem to be in accordance with the derived temperatures for interstellar hydrogen.

Type
Helium and Hydrogen Backscattering Results and the Very Local Interstellar Medium
Information
International Astronomical Union Colloquium , Volume 81: Local Interstellar Medium , 1984 , pp. 32 - 36
Copyright
Copyright © NASA 1984

References

Fahr, H.J. (1974). The extraterrestrial UV-background and the neerby inter-stellar medium. Space Sci. Rev. 15, 483 Google Scholar
Fahr, H.J. (1978). Change of interstellar gas parameters interstellar-wind-dominated astropheres. Astron. Astrophys. 66, 103 Google Scholar
Fahr, H.J., Lay, G. (1974). Solar radiation asymmetries and heliospheric gas heating influencing extraterrestrial UVdata. Space Research XIV, 567 Google Scholar
Fahr, H.J., Nass, H.U., Rucinski, D. (1984). Draglike effects on heliospheric neutrals due to elastic collisions with solar wind ions. Astron. Astrophys. (in press)Google Scholar
Feldman, W.C., Lange, J.J. Scherb, F., (1972). Interstellar helium in inter-planetary space. Solar Wind IV, NASA special publ. 308, ed: Sonnett, C.P. et. al., 684 Google Scholar
Hassan, M.H.A., Wallis, M.K. (1983) stochastic diffusion in inverse square fields: general formulation for interplanetary gas. Planet. Space Sci. 31, 1 Google Scholar
Holzer, T.E. (1977). Neutral hydrogen in interplanetary space. Rev. Geophys. Space Phys. 15, 467 Google Scholar
Kunc, J.A., Wu, F.M., Judge, D.C. (1983). Heating of the interstellar medium by the solar wind. Planet. Space Sci. 31, 1157 Google Scholar
Wallis, M.K. (1975). Collisional heating of interplanetary gas: Fokker-Planck treatment. Planet. Space Sci. 23, 419 CrossRefGoogle Scholar
Wu, F.M., Judge, D.L. (1978). Elektronheating of inflowing interstellar gas. Ap.J. 225, 1045 Google Scholar