Abstract
Four rocket-borne photometers measured nightglow emissions near λ 6300, λ 5893, λ 5577, and λ 5335. The emitting region of the oxygen green line, λ 5577, was entirely between 90 and 118 km, and had a very sharp lower boundary. The sodium D-lines were encountered primarily between 85 and 110 km, with a maximum intensity at 93 km. The upper boundary of D-line emission was not definite, due to tailing off of the distribution and low total intensity, but D-line emission extending into the 130- to 150-km region is indicated. The λ 6300 photometer showed two distinct features: an emitting region from 56 to 100 km, and a large signal still present at the peak of flight, 163 km. We attribute the 56- to 100-km emission to the (9–3) Meinel OH band, and conclude that the region of oxygen red line emission must lie above 163 km. On the basis of relative band intensities for the Meinel OH bands and the dissimilarity of the signal-νs-altitude curves for the λ 5335 and λ 6300 photometers, we conclude that practically all atmospheric emission near λ 5335 is due to an atmospheric “continuum” and not due to OH band emission. This atmospheric “continuum” has a maximum intensity between 100 and 110 km, and is at least as bright as the stellar background. During descent of the rocket through the E-region, the photometers recorded a bright glow in the rocket's wake. Energy for creating the glow had to come from atmospheric gases and not the rocket. Its spectra and other features are discussed.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Disclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.