The H Lyman-α emission line from the upper atmosphere of Jupiter: Parametric radiative transfer study and comparison with data

摘要: This study uses the adding-doubling radiative transfer method in which we take into account curvature effect of planetary atmosphere order to test sensitivity jovian Ly-α emission line relation H column density, eddy diffusion coefficient, frequency redistribution function for photon scattering, temperature vertical profile, and an added hot atomic layer on top atmosphere. We also focus here developing new diagnostic tools that will help us obtain more confidently underlying thermospheric structure Jupiter. First, using brightness distribution specific wavelength bands as proposed by Ben Jaffel et al. [Ben Jaffel, L., Magnan, C., Vidal-Madjar, A., 1988. Astron. Astrophys. 204, 319–326], show spatial thickness above homopause level can be measured directly separation between positions respectively core wing optical limbs. constrains [H] value KH coefficient at disc location under consideration. propose refine [H], respectively, a latitude, Q ratio limb peak intensity from other regions over disc. Finally, relationship gradient thermosphere is demonstrated, thus providing accurate tool access this key information high resolution observations. Quick, preliminary comparisons with some existing HTS/STIS data auroral latitudes (∼1700 km) much smaller than equatorial (∼3900 km). These results strongly support existence both density versus higher values regions. Such small consistent mixing brings hydrocarbons upwards, reducing consequently hydrogen scatters photons. strength approach open horizons use strong resonant lines state upper atmospheres.