DOI QR코드

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Simulating the 3.4-Micron Feature of Titan's Haze

  • Kim, Y.S. (Department of Chemistry, University of Hawaii at Manoa) ;
  • Ennis, C. (Department of Chemistry, University of Hawaii at Manoa) ;
  • Kim, Sang Joon (School of Space Research, Kyung Hee University)
  • 투고 : 2012.10.03
  • 심사 : 2012.12.08
  • 발행 : 2013.03.20

초록

Four prominent features of Titan's haze are found within the '3.4-${\mu}m$' absorption to be uniform with recent vertically resolved Cassini/VIMS spectra. These are absorptions at 2998 $cm^{-1}$ (3.34 ${\mu}m$), 2968 $cm^{-1}$ (3.37 ${\mu}m$), 2927 $cm^{-1}$ (3.42 ${\mu}m$), and 2882 $cm^{-1}$ (3.47 ${\mu}m$). A detailed fitting suggests that the 2998 $cm^{-1}$ feature could originate from amorphous acetonitrile ($CH_3CN$) carrying about 25% of integrated optical depth; the remaining features, which account for 75% of the integrated optical depth, could arise from a distinct triplet (C-H stretching) structure of radiolyzed hydrocarbons. An additional feature was possibly evidenced at altitudes higher than 300 km and attributable to 'polymer-capped' methane ($CH_4$), significantly constraining the chemical composition of organic haze layers under Titan's active radiation field.

키워드

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