ETON 1: A data base pertinent to the study of energy transfer in the oxygen nightglow

Greer, R.G.H.; Murtagh, Donal; McDade, I. C.; Dickinson, P.H.G.; Thomas, L.; Jenkins, D. B.; Stegman, J.; Llewellyn, E. J.; Witt, G.; Mackinnon, D. J.; Williams, E. R.

doi:10.1016/0032-0633(86)90074-7

Cited by 132 publications

(84 citation statements)

References 11 publications

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“…Neglecting quenching effects make the profile roughly proportional to the product of [O] 2 and O 2 . Thus the altitude and shape of the profile are dominated by the constituent profiles of atomic and molecule oxygen with a typical peak altitude of 95 km as observed from rocket measurements by Witt et al (1979Witt et al ( , 1984 and Greer et al (1986). The OH emission is produced by the reaction of ozone and atomic hydrogen, but the ozone is produced by the reaction of atomic oxygen with O 2 , so that the OH emission is roughly proportional to [O], locating it below the O 2 emission normally at 87 km, as observed by rocket measurements by Baker and Stair (1988).…”

Section: -Daymentioning

confidence: 83%

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O2 atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

et al. 2009

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Abstract. The presence of planetary wave type oscillations at mid-latitudes in the mesosphere/lower thermosphere region has been investigated using airglow observations. The observations were taken with a Spectral Airglow Temperature Imager (SATI) installed at Sierra Nevada Observatory (37.06 • N, 3.38 • W) at 2900 m height. Airglow data of the column emission rate of the O 2 Atmospheric (0-1) band and of the OH Meinel (6-2) band and deduced rotational temperatures from 1998 to 2007 have been used in this study. From these observations a climatology of planetary wave type oscillations at this location is inferred. It has been found that the planetary wave type oscillations of 5-day period is predominant in our data throughout the year, with activity greater than 50% during March/April and October/November months. The planetary wave type oscillations of 2-day period is predominant during both solstices, being predominant during winter solstice in O 2 while a 10-day oscillation appears throughout the year with activity around 20% and with maximum activity during spring and autumn equinoxes. The 16-day oscillation has maximum occurrence during autumn-winter while its activity is almost disappeared during spring-summer. No clear seasonal dependence of the amplitude of the planetary wave type oscillations was observed in the cases considered in this study.The waves simultaneously detected in the rotational temperatures deduced from both OH and O 2 emissions usually Correspondence to: M. J. López-González (mariajose@iaa.es) show an upward energy propagation and are affected by dissipation processes.

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Section: -Daymentioning

confidence: 83%

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O2 atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

et al. 2009

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“…where A (Greer et al, 1986;McDade et al, 1986b). The values of the rate coefficients and excitation parameters to be used in Eq.…”

Section: No From the Photometric Measurementsmentioning

confidence: 99%

Observations of NO in the upper mesosphere and lower thermosphere during ECOMA 2010

et al. 2012

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Abstract. In December 2010 the last campaign of the German-Norwegian sounding rocket project ECOMA (Existence and Charge state Of Meteoric smoke particles in the middle Atmosphere) was conducted from Andøya Rocket Range in northern Norway (69 • N, 16 • E) in connection with the Geminid meteor shower. The main instrument on board the rocket payloads was the ECOMA detector for studying meteoric smoke particles (MSPs) by active photoionization and subsequent detection of the produced charges (particles and photoelectrons). In addition to photoionizing MSPs, the energy of the emitted photons from the ECOMA flash-lamp is high enough to also photoionize nitric oxide (NO). Thus, around the peak of the NO layer, at and above the main MSP layer, photoelectrons produced by the photoionization of NO are expected to contribute to, or even dominate above the main MSP-layer, the total measured photoelectron current. Among the other instruments on board was a set of two photometers to study the O 2 (b 1 + g − X 3 − g ) Atmospheric band and NO 2 continuum nightglow emissions. In the absence of auroral emissions, these two nightglow features can be used together to infer NO number densities. This will provide a way to quantify the contribution of NO photoelectrons to the photoelectron current measured by the ECOMA instrument and, above the MSP layer, a simultaneous measurement of NO with two different and independent techniques. This work is still on-going due to the uncertainties, especially in the effort to quantitatively infer NO densities from the ECOMA photoelectron current, and the lack of simultaneous measurements of temperature and density for the photometric study. In this paper we describe these two techniques to infer NO densities and discuss the uncertainties. The peak NO number density inferred from the two photometers on ascent was 3.9 × 10 8 cm −3 at an altitude of about 99 km, while the concentration inferred from the ECOMA photoelectron measurement at this altitude was a factor of 5 smaller.

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“…Rocket and satellite measurements have shown that the peak of maximum emission rate of the O 2 atmospheric emission is placed at about 95 km (e.g. Witt et al, 1979Witt et al, , 1984Greer et al, 1986). So, rotational temperatures from the O 2 (0-1) atmospheric band are good indicators of the atmospheric temperature at around 95 km height.…”

Section: Introductionmentioning

confidence: 99%

Seasonal variations of O2 atmospheric and OH(6−2) airglowand temperature at mid-latitudes from SATI observations

et al. 2004

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Abstract. More than 3 years of airglow observations with a Spectral Airglow Temperature Imager (SATI) installed at the Sierra Nevada Observatory (37.06 • N, 3.38 • W) at 2900 m height have been analyzed. Values of the column emission rate and vertically averaged temperature of the O 2 atmospheric (0-1) band and of the OH Meinel (6-2) band from 1998 to 2002 have been presented. From these observations a clear seasonal variation of both emission rates and rotational temperatures is inferred at this latitude. It is found that the annual variation of the temperatures is larger than the semiannual variation, while for the emission rates the amplitudes are comparable.

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ETON 1: A data base pertinent to the study of energy transfer in the oxygen nightglow

Cited by 132 publications

References 11 publications

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O<sub>2</sub> atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O<sub>2</sub> atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Observations of NO in the upper mesosphere and lower thermosphere during ECOMA 2010

Seasonal variations of O<sub>2</sub> atmospheric and OH(6−2) airglowand temperature at mid-latitudes from SATI observations

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ETON 1: A data base pertinent to the study of energy transfer in the oxygen nightglow

Cited by 132 publications

References 11 publications

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O&lt;sub&gt;2&lt;/sub&gt; atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O&lt;sub&gt;2&lt;/sub&gt; atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Observations of NO in the upper mesosphere and lower thermosphere during ECOMA 2010

Seasonal variations of O&lt;sub&gt;2&lt;/sub&gt; atmospheric and OH(6−2) airglowand temperature at mid-latitudes from SATI observations

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Product

Resources

About

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O<sub>2</sub> atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Climatology of planetary wave type oscillations with periods of 2–20 days derived from O<sub>2</sub> atmospheric and OH(6-2) airglow observations at mid-latitude with SATI

Seasonal variations of O<sub>2</sub> atmospheric and OH(6−2) airglowand temperature at mid-latitudes from SATI observations