Asymmetry in the Jovian auroral Lyman-α line profile due to thermospheric high-speed flow

Details Asymmetry in the Jovian auroral Lyman-α line profile due to thermospheric high-speed flow Asymmetry in the Jovian auroral Lyman-α line profile due to thermospheric high-speed flow

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jgre..11505002c&link_type=abstract

Journal of Geophysical Research, Volume 115, Issue E5, CiteID E05002

Astronomy and Astrophysics

Astrophysics

2

Planetary Sciences: Fluid Planets: Aurorae, Planetary Sciences: Solar System Objects: Jupiter, Solar Physics, Astrophysics, And Astronomy: Ultraviolet Emissions

Scientific paper

The presence of a fast wind in the auroral region atmosphere of Jupiter has been detected from the Doppler shift in near-IR observations of H3+ emissions. The Doppler effect also modifies auroral resonance emission line shapes. We present a new radiative transfer equation for the hydrogen Lyman-α line in the presence of a horizontal wind and solve it numerically using the Feautrier method. This model allows us to derive the theoretical profile of the Lyman-α emission line. We apply this code to long slit echelle spectra of Jupiter's auroral Lyman-α emission obtained by HST-STIS which exhibit a self-reversed and asymmetric profile. Using a simple expression for the vertical variation of the horizontal wind velocity, we find the HST-STIS observations are well reproduced by a velocity profile reaching ˜4-8 km/s near ˜10-5 μbar pressure altitude (˜1500 km above the 1 bar level). The velocity is much higher than velocity derived from H3+ emission peaking at ˜550 km and consistent with an increase of the velocity with regards to altitude but reaching larger values than predicted by circulation models at ˜10-5 μbar.

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