Oxygen Atom Rydberg Emissions at 394-927 NM in the Nightglow, as Measured Near Solar Maximum at Mauna Kea

Details Oxygen Atom Rydberg Emissions at 394-927 NM in the Nightglow, as Measured Near Solar Maximum at Mauna Kea Oxygen Atom Rydberg Emissions at 394-927 NM in the Nightglow, as Measured Near Solar Maximum at Mauna Kea

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sa61a02s&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SA61A-02

Astronomy and Astrophysics

Astronomy

0310 Airglow And Aurora

Scientific paper

Nightglow emissions from oxygen atom Rydberg levels were detected from astronomical sky spectra taken from Mauna Kea, Hawai'i. The spectra were obtained at the Keck I telescope with the HIRES spectrometer (R~37,000) in 1993-1997 near solar minimum, and at the Keck II telescope with the ESI spectrometer (R~7,000) in 2000, near solar maximum. In 1993-97, only the quintet 772-775 nm and the triplet 844.6 nm features were seen, while in 2000 we were able to detect twenty groups of multiplets, at 394-927 nm, with quintet transitions being more conspicuous than triplets. In some of the ESI spectra, emission at 772-775 nm is very high, approximately two orders of magnitude more intense relative to nearby OH features than in the 1994-97 period. The expected source of the oxygen excited states is the radiative recombination of O+ with an electron. The ESI data show strong N(2D) 520 nm emission, comparable to that from the 589 nm sodium doublet, when the oxygen emission is intense. N(2D) is also generated from an ion/electron recombination reaction, dissociative recombination of NO+. We are greatly indebted to Professor Wallace Sargent and Dr. Thomas Barlow of Caltech for providing us with the ESI spectra, and to the NSF Aeronomy program for support.

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