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Simulation of Titan haze formation using a photochemical flow reactor: The optical constants of the polymer by Buu N. Tran; Jeffrey C. Joseph; James P. Ferris; Peter D. Persans; John J. Chera is a Physics and Astronomy article available to read on EtoBox.

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Solar UV is the principal energy source impinging the atmosphere of Titan while the energy from the electrons in Saturn's magnetosphere is less than 0.5% of the UV light. Titan haze analogs were prepared by the photolysis of a mixture of gases that simulate the composition of its atmosphere (nitrogen, methane, hydrogen, acetylene, ethylene, and cyanoacetylene). The real (n) and imaginary (k) parts of the complex refractive index of haze analogs formed from four different gas mixtures were calculated from the spectral properties of the solid polymer in UV-visible, near infrared and infrared wavelength spectral regions. The value of n was constant at 1.6 ± 0.1 throughout the 0.2-2.5 μm region. The variation of k with wavelength for the values derived for Titan has a lower error than the absolute values of k so the more significant comparisons are with the slopes of the k(λ) plots in the UV-VIS region. Three of the photochemical Titan haze analogs had slopes comparable to those derived for Titan from the Voyager data (Rages and Pollack, 1980, Icarus 41, 119-130;McKay and Toon, 1992, in: Proceedings of the Symposium on Titan, in: ESA SP, Vol. 338,. The slopes of the k(λ) plots for haze

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Author

Buu N. Tran; Jeffrey C. Joseph; James P. Ferris; Peter D. Persans; John J. Chera

Publisher

Elsevier Science; Elsevier ; Elsevier Inc.; Elsevier BV; Oxford University Press (OUP) (ISSN 0019-1035)

Published

2003

Language

EN

Field

Physics and Astronomy (Physical Sciences)