Photochemistry of Ozone-Water Ices

被引：2

作者：

Johnson, Paul V. ^{[1
,2
]}

Markus, Charles R. ^{[1
,3
]}

Hodyss, Robert ^{[1
,2
]}

机构：

[1] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[2] NASA Astrobiol Inst, Mountain View, CA 94035 USA

[3] Univ Illinois, Dept Chem, Urbana, IL 61801 USA

来源：

ACS EARTH AND SPACE CHEMISTRY | 2019年 / 3卷 / 11期

关键词：

ultraviolet; photochemistry; spectroscopy; ozone; Ganymede; Rhea; Dione; AMINO-ACIDS; ULTRAVIOLET PHOTOLYSIS; SOLID OXYGEN; SATELLITES; PHOTODISSOCIATION; INTERSTELLAR; MATRIX; ATLAS;

D O I：

10.1021/acsearthspacechem.9b00189

中图分类号：

O6 [化学];

学科分类号：

0703 ;

摘要：

Ozone is known to be present within the surface ice of Jupiter's moon Ganymede as well as Saturn's moons Dione and Rhea. Given the ubiquity of solar photons incident on these water-ice-dominated surfaces, experiments were conducted to better understand the photochemistry of ozone-water ice mixtures. Samples were deposited as thin films in a vacuum chamber under temperature and pressure conditions relevant to satellites in the outer solar system. Chemical changes in the ices were monitored with infrared spectroscopy as they were exposed to ultraviolet light at 116.5/123.6, 147, and 254 nm emitted from Kr, Xe, and Hg resonant lamps, respectively. In all instances, hydrogen peroxide formed after ultraviolet irradiation, while the amount of ozone present decreased. Of the wavelengths tested, irradiation at 254 rim induced the most rapid change both in terms of irradiation time and number of incident photons. This work emphasizes the importance of wavelengths longer than the vacuum ultraviolet in the chemical evolution of ozone on Ganymede, Dione, and Rhea.

引用

页码：2430 / 2436

页数：13

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