Simulating the 3.4-Micron Feature of Titan’s Haze 


Vol. 34,  No. 3, pp. 759-762, Mar.  2013
10.5012/bkcs.2013.34.3.759


PDF
  Tumbnail

  Abstract

Four prominent features of Titan’s haze are found within the ‘3.4-μm’ absorption to be uniform with recent vertically resolved Cassini/VIMS spectra.1 These are absorptions at 2998 cm−1 (3.34 μm), 2968 cm−1 (3.37 μm), 2927 cm−1 (3.42 μm), and 2882 cm−1 (3.47 μm). A detailed fitting suggests that the 2998 cm−1 feature could originate from amorphous acetonitrile (CH3CN) 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 (CH4), significantly constraining the chemical composition of organic haze layers under Titan’s active radiation field.

  Statistics
Cumulative Counts from November, 2022
Multiple requests among the same browser session are counted as one view. If you mouse over a chart, the values of data points will be shown.


  Cite this article

[IEEE Style]

Y. S. Kim, C. Ennis, S. J. Kim, "Simulating the 3.4-Micron Feature of Titan’s Haze," Bulletin of the Korean Chemical Society, vol. 34, no. 3, pp. 759-762, 2013. DOI: 10.5012/bkcs.2013.34.3.759.

[ACM Style]

Y. S. Kim, C. Ennis, and Sang Joon Kim. 2013. Simulating the 3.4-Micron Feature of Titan’s Haze. Bulletin of the Korean Chemical Society, 34, 3, (2013), 759-762. DOI: 10.5012/bkcs.2013.34.3.759.

Search
(IN TITLE, AUTHOR, ABSTRACT,KEYWORDS)

Advanced Search ▼

POPULAR KEYWORDS
(TOP 10 KEYWORDS)

Recent Publications
(LAST 3 YEARS)

ISSN(Print) 0253-2964
ISSN(Online) 1229-5949