Abstract
Infrared spectroscopy is an essential tool for analyzing the chemical composition of planets, satellites and comets. Observations with the ISO satellite have been performed on all classes of solar-system objects. Several important discoveries have been achieved, in particular with the Short-Wavelength Spectrometer. In spite of difficult observability constraints, spectra of Mars have been recorded with SWS and LWS. They have been used for a retrieval of the water vapor vertical distribution and a determination of the surface emissivity at long wavelengths. After removal of the atmospheric contribution in the 7–13 μm range, the emissivity spectrum of the surface shows distinct features due to solid signatures. In the case of the giant planets, the D/H ratio has been determined from the analysis of infrared HD transitions. An external source of oxygen has been discovered in the stratospheres of the giant planets and Titan through the detection of H2O emission lines; CO2 has also been detected on Jupiter, Saturn and Neptune. The origin of the oxygen flux, of comparable intensity on all giant planets and on Titan, might be interplanetary (micrometeorites) and/or local (rings, satellites). Several new hydrocarbons have been detected in the stratospheres of the giant planets, including C6H6 in Jupiter and Saturn, C4H2 and CH3C2H in Saturn, CH3 in Saturn and Neptune. These results provide new constraints on photochemical models of these planets. H2O has been also detected in Saturn’s troposphere with a very low abundance, as in the case of Jupiter; this suggests a possible similarity in the circulation mechanisms of both planets. In the case of Jupiter and Saturn, CAM images have been obtained in the CVF mode. These data will be used to retrieve information about the temperature field and (in the case of Jupiter) the spatial properties of the NH3 cloud; the Saturn data have been used to separate the ring and disk contributions. Comet Hale-Bopp was observed by ISO at several heliocentric distances, pre and post perihelion. The main spectroscopic results of these observations are the first detection of CO2 at large heliocentric distances (4.6 AU), the discovery of forsterite (Mg2SiO4) in the coma dust, and the determination of the formation temperature (25 K) from the analysis of the ortho and para H2O lines at 2.6 μm. A similar measurement with ISO in comet Hartley 2 led to a value of 35 K. Far-infrared photometry with PHT was used to retrieve brightness temperatures at various heliocentric distances and, in complement to CAM images in various filters, to constrain the composition and size distribution of the grains. ISO also observed Galilean satellites, Pluto, asteroids, other comets and cometary nuclei, cometary trails and zodiacal light. In particular, the far-infrared light-curve of Pluto, obtained with PHT, provided information about the nature of Pluto’s surface. Systematic observations of the zodiacal light have been performed with CAM and PHT to investigate its spatial variations and the properties of interplanetary dust.
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Encrenaz, T. (2000). ISO Observations of Solar-System Objects. In: Casoli, F., Lequeux, J., David, F. (eds) Astronomie spatiale infrarouge, aujourd’hui et demain Infrared space astronomy, today and tomorrow. Les Houches - Ecole d’Ete de Physique Theorique, vol 70. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-45573-6_4
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