A visible and near-infrared spectroscopic investigation of Triton's two faces

Details A visible and near-infrared spectroscopic investigation of Triton's two faces A visible and near-infrared spectroscopic investigation of Triton's two faces

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....1084m&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #1084

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Scientific paper

Triton is one of the most peculiar satellites of the Solar System, for several reasons. First of all, for its retrograde orbit that makes of Triton a plausible captured satellite. Moreover, Triton is synchronously rotating, so we can speak of leading and trailing sides. The Voyager had shown huge differences between the two hemispheres, being the leading side much more cratered that the trailing one. The origin of this huge asymmetry is still not clearly understood. We think that some hints could arise from a spectral investigation of Triton's double face. We present here the results of new observations of Triton performed with the ESO telescope NTT (La Silla, Chile) in October 2002. Using the high quality of NTT instrumentation (EMMI for the visible and SOFI for the Infrared), we were able to cover the entire 0.4--2.5 μm spectral range in a single night. We applied this procedure for two nights, well selected along the orbit of Triton, in order to cover essentially the trailing side one night, and the leading one the other night, obtaining the first face-resolved 0.4--2.4 μm spectra of Triton. We discuss here the spectra and the differences between the two faces, and the implications of this findings for a better understanding of the surface composition of Triton.

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