Resonance line radiative transfer for hot atom coronae using Kappa distributions

摘要: Abstract Hot atomic populations are an important component of the planetary exospheres. Usually, radiative transfer models describing scattering light by moving atoms assume that these have a Maxwellian velocity distribution. However, distributions hot could actually some more extended wings. Popular often used in plasma physics and recently proposed to describe neutral environments Kappa function distributions. In this paper, following work Hummer [Non-coherent scattering: I The redistribution functions with Doppler broadening. R Astron. Soc Month Not 1962;125:21] Cranmer [Non-Maxwellian solar coronal Lyα emission. Astrophys J 1998;508:925–39], we calculate frequency radiation scattered We also present detailed study model taking into account distribution functions, for integer semi-integer values κ . apply theory Jupiter hydrogen corona containing 0.1% column density quantify spectroscopic imaging differences between bi-Maxwellian When assuming =2 population, intensity increases ∼40% occur at bright limb ∼15% on disk compared same calculations done using line profile differs slightly from limb, but difference is larger above limb. Jovian atmosphere speculative further studies needed link formation exospheric