New Ground-based Measurements of the Venus Nightglow

Details New Ground-based Measurements of the Venus Nightglow New Ground-based Measurements of the Venus Nightglow

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsa41a..17s&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SA41A-17

Astronomy and Astrophysics

Astronomy

5405 Atmospheres: Composition And Chemistry, 6295 Venus

Scientific paper

In 1999 it was demonstrated that the oxygen green line is a significant component of the Venus nightglow, using the Keck I telescope and the associated HIRES echelle spectrometer [1]. In February 2001 Venus was viewed again, this time using the 3.5-meter APO telescope in New Mexico. Four evenings were available, and longer integration times were used than the eight minutes of the Keck run. However, this time the green line was weak in comparison to the terrestrial line - possibly absent altogether. In contrast, the 0-10 O2(c-X) Herzberg II band was strong and distinct. These bands appear to be more persistent features than the green line, which was also absent in the original measurements of Krasnopolsky et al. from Venera 9/10 [2]. To understand the Venus nightglow processes it is desirable to have repeated coordinated measurements of the planet for the known emitters observable from the ground - O(1S - 1D), O2(c1Σ u- - X3Σ g-), and the 1.27 μ O2(a1Δ g - X3Σ g-) 0-0 band, also known to be quite variable [3]. [1] T. G. Slanger, P. C. Cosby, D. L. Huestis, and T. A. Bida, Science 291, 463 (2001). [2] V. A. Krasnopolsky, A. A. Krysko, V. N. Rogachev, and V. A. Parshev, Cosmic Research 14, 789 (1976). [3] D. Crisp et al., J. Geophys. Res. 101, 4577 (1996). This work was supported by a grant from the NASA Planetary Astronomy program.

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