Computer Science
Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7769p&link_type=abstract
HST Proposal ID #7769
Computer Science
Hst Proposal Id #7769 Solar System
Scientific paper
Our primary interest is the diagnostic of the Lyman alpha emission in several particular regions of the Jovian auroral region, together with records of the H2 Lyman and Werner emission which is necessary for its interpretation. High resolution spectra around the Lyman alpha line with STIS and grating E140H will give access to atmospheric parameters at and above the auroral source, along the slit centered on the region of interest {[H] from radiative transfer modeling of the reversed Lyman alpha profile, T from temperature sensitive H2 lines}, and to information concerning the precipitating particles responsible for the excitation {search for an extended red-shifted wing typical of energetic proton precipitation, and for Doppler shifts and line asymmetries indicative of superthermal proton inflows or outflows}. Low resolution spectra taken at the same place with STIS and grating G140L will provide complementary information, in particular on the hydrocarbon column density abov e the source, required to establish the local vertical structure of the auroral atmosphere and fully interpret the spectra in terms of preciptating particle diagnostics. Previous HST observations with GHRS and FOC have shown that a wide variety of auroral processes takes place in a series of localized specific features. Consequently, we will target with particular care a few specific areas: {1, 2} the so-called 'main oval' at the footprint of the magnetic shell 30 RJ both sides of longitude 150 deg. { 120 and 200 deg.}, {3} the polar emission along the meridian 160 deg., {4} the 'low-latitude' spot magnetically conjugate of the outer Io torus at about the same longitude, and {5} the neighborhood of the Io flux tube footprint whenever possible. Since the spectra must not be contaminated by signatures of different processes acting in nearby areas, particular attention will be paid to good pointing of the aperture, which will be checked at high accuracy by taking images of bot h h emispheres in the same visit. In addition, the general auroral morphology at the time of the observations must be recorded during the previous or the next Jovian rotation in the wavelength ranges of major importance for the interpretation of the spectra {especially to estimate the contribution of various orders in the Echelle spectra}. Finally, the experience gained in the last two years has confirmed that the scientific return of the observations will be increase by orders of magnitude if the are taken while Galileo is taking in-situ particle and field measurements in the Jovian magnetosphere.
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