Icarus 160, 172–182 (2002) doi:10.1006/icar.2002.6899 Analysis of the Time-Dependent Chemical Evolution of Titan Haze Tholin Bishun N. Khare Mail Stop 239-11, NASA Ames Research Center, Moffett Field, California 94035 E. L. O. Bakes SETI Institute, Mail Stop 245-3, NASA Ames Research Center, Moffett Field, California 94035 E-mail:
[email protected] Hiroshi Imanaka SETI Institute, Mail Stop 239-11, NASA Ames Research Center, Moffett Field, California 94035 Christopher P. McKay and Dale P. Cruikshank Space Sciences Division, Mail Stop 245-3, NASA Ames Research Center, Moffett Field, California 94035 and Edward T. Arakawa Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831 Received June 19, 2001; revised February 20, 2002 1. INTRODUCTION Haze particles exert a significant influence over the thermody- namics and radiation absorption properties of the Titan haze, as Observations of Titan’s haze by Voyager indicate a dense well as its complex organic chemistry. Characterization of both the layer of smog produced by ongoing charged particle photo- molecular and the submicrometer components of the haze is there- chemistry and ultraviolet (UV) radiation in Titan’s stratosphere fore vital for understanding the global properties of Titan. We have (Hanel et al. 1981). Titan’s atmospheric haze dominates its carried out a Titan tholin synthesis experiment and measured the temperature, atmospheric circulation, and climate control, and time variation of the infrared spectrum of the product as a thin film photochemistry plays a key role in the structure and evolu- developed. Also, to examine the possibility of oxygen contamina- tion of the haze.