Detection of arsine in Saturn

Journal Article · Wed Nov 01 04:00:00 EST 1989 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/168032· OSTI ID:7274230

Bezard, B; Drossart, P; Lellouch, E; Tarrago, G; Maillard, J P ^[1]

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1. Paris Observatoire, Meudon (France) Paris XI Universite, Orsay (France) CNRS, Institut d'Astrophysique, Paris (France)

The detection of arsine (AsH3) in Saturn's atmosphere using high-resolution observations near 4.7 microns is reported. A strong broad absorption at the position of the nu3 Q-branch of AsH3 and weaker features where the R(1) lines of the nu1 and nu3 bands occur are noted in this high-resolution spectral range. Comparison with synthetic spectra derived from a model atmosphere indicates the following: both the thermal emission and the reflected solar radiation contribute to Saturn's 5 micron flux; the mole fraction of arsine is (2.4 + 1.4 or - 1.2) x 10 to the -9th in the approx. 4 bar region (T about 200 K) from which the thermal emission originates; AsH3 is 2.5 to 10 times less abundant in the upper troposphere (0.2-0.4 bar), a possible consequence of UV photolysis. The current observation of arsine implies upward transport from the 360 K region that is sufficiently rapid to inhibit conversion reactions. A reanalysis of 5-micron spectroscopic observations of Jupiter by Bjoraker, Larson, and Kunde (1986) indicated that arsine is much less abundant on Jupiter (AsH3/H2 less than or roughly equal to 3 x 10 to the -10th) than on Saturn. 27 refs.

• OSTI ID: 7274230
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 346; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640107* -- Astrophysics & Cosmology-- Planetary Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ABSORPTION SPECTRA
ABUNDANCE
ARSENIC COMPOUNDS
ATMOSPHERES
CHEMICAL COMPOSITION
CHEMISTRY
COSMOCHEMISTRY
HYDRIDES
HYDROGEN COMPOUNDS
MATHEMATICAL MODELS
PLANETARY ATMOSPHERES
PLANETS
SATURN PLANET
SPECTRA