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| Reference : The distribution of hot hydrogen atoms produced by electron and proton precipitation in ... |
| Scientific journals : Article | |||
| Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics | |||
| http://hdl.handle.net/2268/27467 | |||
| The distribution of hot hydrogen atoms produced by electron and proton precipitation in the Jovian aurora | |
| English | |
| Bisikalo, D. V. [> > > >] | |
| Shematovich, V. I. [> > > >] | |
Gérard, Jean-Claude  [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Labo de physique atmosphérique et planétaire (LPAP) >] | |
| Gladstone, G. R. [> > > >] | |
| Waite, J. H. [> > > >] | |
| 1-Sep-1996 | |
| Journal of Geophysical Research | |
| American Geophysical Union (AGU) | |
| 101 | |
| 21157-21168 | |
| International | |
| 0148-0227 | |
| Washington | |
| DC | |
| [en] Planetology: Fluid Planets: Atmospheres-composition and chemistry ; Atmospheric Composition and Structure: Airglow and aurora ; Atmospheric Composition and Structure: Thermosphere-composition and chemistry ; Planetology: Fluid Planets: Interactions with particles and fields | |
| [en] The energy distribution functions of nonthermal thermospheric hydrogen atoms are calculated for electron and proton precipitation in the Jovian aurora. A numerical model taking into account the production, elastic and inelastic relaxation and transport processes for hot H atoms is developed. This model is based on a Monte Carlo solution of the nonlinear Boltzmann equation for hot H atoms produced by electron and proton impact on H and H[SUB]2[/SUB] and exothermic chemical reactions. The distribution functions show a much higher energy tail for proton than electron precipitation. It is shown that the steady state flux of hot atoms (E>=2 eV) is essentially isotropic. The peak and column hot H densities are about 3×10[SUP]5[/SUP] cm[SUP]-3[/SUP] and 1×10[SUP]14[/SUP] cm[SUP]-3[/SUP] for a 100 erg cm[SUP]-2[/SUP]s[SUP]-1[/SUP] precipitation combining hard (22 keV) and soft (0.2 keV) electrons mixed with a 10 erg cm[SUP]-2[/SUP]s[SUP]-1[/SUP] flux of soft (0.3 keV) protons. These column densities, coupled with the wide range of hot H atom energies, may play an important role in the formation of the Lyman alpha line profile. Multiple scattering in the wings of the Ly alpha line by the fast H atoms is shown to partly account for the broad Ly alpha profile observed in the Jovian aurora with the Hubble space telescope. | |
| Researchers ; Professionals ; Students | |
| http://hdl.handle.net/2268/27467 | |
| 10.1029/96JE01952 | |
| http://adsabs.harvard.edu/abs/1996JGR...10121157B |
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