S2 in planetary atmospheres: a coupled-channel Schrödinger equation calculation of the B 3Σ u^- - X 3Σ g^- transition

Details S2 in planetary atmospheres: a coupled-channel Schrödinger equation calculation of the B 3Σ u^- - X 3Σ g^- transition S2 in planetary atmospheres: a coupled-channel Schrödinger equation calculation of the B 3Σ u^- - X 3Σ g^- transition

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.1603g&link_type=abstract

American Astronomical Society, DPS meeting #35, #16.03; Bulletin of the American Astronomical Society, Vol. 35, p.940

Astronomy and Astrophysics

Astronomy

Scientific paper

Diatomic sulfur (S2) has been observed in absorption, via the strong ultraviolet B 3Σu^- - X 3Σg^- system, in the atmospheres of Jupiter and Io. The determinations of S2 abundances and temperatures from its ultraviolet absorption signature are hindered by the very large uncertainties associated with the fundamental spectroscopic parameters of the molecule. Oscillator strengths, line widths and line shapes are, to date, poorly determined. As part of a combined program of calculations and laboratory measurements, we present preliminary model calculations of the S2 B - X absorption spectrum. From limited spectroscopic information, it is known that the B 3Σ u^- state is heavily perturbed by B'' 3Πu, 1Πu and 5Σu^-(5Πu) predissociating states (Wheeler et al. 1998) which yield an apparently complex spectrum. In contrast, the analogous B - X transition in molecular oxygen (O2), responsible for the Schumann-Runge bands, has been studied extensively in the laboratory. The apparent complexities of this spectrum are readily understood, in terms of a coupled-channel Schrödinger equation (CSE) model (Lewis et al. 2001). We apply a CSE model developed for the B 3Σ u^- - X 3Σg^- transition of O2 to the analogous S2 spectrum, employing the potential energy curves and coupling scheme of Wheeler et al., as a starting point.The CSE calculations provide valuable insight into the photodissociation spectrum, demonstrating complex interference effects that are more pronounced than for O2 and hence of significance to planetary photochemical models. These calculations will guide planned measurements of the strengths and lineshapes of the B-X system. References: M. D. Wheeler, S. M. Newman, and A. J. Orr-Ewing, J. Chem. Phys. 108, 6594-6605 (1998); B. R. Lewis, S. T. Gibson, F. T. Hawes, and L. W. Torop, Phys. Chem. Earth (C) 26, 519-526 (2001).

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