Search for ionospheric winds in Jupiter from the H_3^+ emissions

Details Search for ionospheric winds in Jupiter from the H_3^+ emissions Search for ionospheric winds in Jupiter from the H_3^+ emissions

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dps....31.7307m&link_type=abstract

American Astronomical Society, DPS meeting #31, #73.07

Astronomy and Astrophysics

Astronomy

Scientific paper

Between October 8 and 11, 1998, we observed the Northern and Southern auror= al regions of Jupiter in the \nu_2 fundamental band of H_3^{+} with the Fourier Transform Spectrometer at CFHT. In total, 15 spectra were recorded.= The spectra, which covered the 2465--2580 cm^{-1} domain, were all acquired at a resolving power in the range 55000 to 75000. This high= resolution, which corresponds to a 4--5.5 km s^{-1} velocity resolution, = was aimed at searching for ionospheric winds from measurements of Doppler shifts in the H_3^+ lines. In the brightest regions, up to 20 H_3^{+} lines were detectable, but in practice, about ten lines were usable, including the strongest ones at 2509.075 and 2529.724 cm^{-1}. The S/N ratio on these lines in the spectra set varies= from 140 to 15, depending on the observed auroral regions. The spectra were= acquired with a 2.5'' aperture successively centered on specific high latit= ude (57^{\circ}--82^{\circ}) points, either near central meridian or on the= limbs. Systematic corrections include the topocentric velocity of Jupiter, = the rotational velocity of the target emitting regions, and known instrumental= effects. The estimated accuracy is on the order of 1 km s^{-1}, one major source o= f uncertainty coming from the pointing precision. Current results marginally = indicate the presence of \sim 2 km ^{-1} retrograde winds on the Jupite= r North and South Eastern limbs, and possibly a radial component of comparable amplitude on the central meridian. From this first analysis, the order of magnitude of the measured winds is= consistent with the results of Rego et al. (Nature, 1999), hence excluding= ionospheric Jovian winds at the altitude of H_3^{+} formation faster than 3 km s^{-1}.

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