Ozone Measurements in the Mesosphere During The Solar Proton Event of 2 November 1969

Weeks, L. H.; Cuikay, R. S.; Corbin, J. R.

doi:10.1175/1520-0469(1972)029<1138:omitmd>2.0.co;2

Cited by 110 publications

(57 citation statements)

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“…Jackman and McPeters, 1987). 03 depletions during SPEs have even been measured in the mesosphere (Weeks et al, 1972;Thomas et al, 1983;McPeters and Jackman, 1985). The 03 depletions observed for the July 13, 1982 SPE were modeled from HO, enhancements by Solomon et al (1983).…”

Section: Model Description and Resultsmentioning

confidence: 99%

Mesospheric Heating during Highly Relativistic Electron Precipitation Events.

Goldberg

Baker

Herrero

et al. 1995

J. geomagn. geoelec

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Highly relativistic electron precipitation (HRE) events which occur in the mid-latitude and auroral regions last 2.5 days on the average, peaking in the magnetosphere daily near local noon. Furthermore, they can recur every 27 days for several synodic solar rotation periods, and become most intense and frequent during the minimum of the solar cycle. These events are described in terms of their spatial and temporal extent and their spectral characteristics. A detailed sounding rocket study of a relatively weak event in May, 1990 at Poker Flat, Alaska gave energy depositions from which modeling calculations have yielded 03 depletion estimates in excess of 25% near 75 km altitude. These depletions would hardly affect the UV flux reaching the stratosphere below, but could alter the thermal balance in the 60-75 km altitude region in the mesosphere. Further analysis for that HRE has shown the possibility of Joule heating effects near the polar cusp of up to 3°/day depending on the magnitude of the electric field. The mesospheric heating caused by more intense events studied with SAMPEX (Solar Anomalous Magnetospheric Particle Explorer) is compared with the earlier May 1990 event to demonstrate the global impact of HRE events on the chemical and thermal characteristics of the neutral atmosphere.

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Section: Model Description and Resultsmentioning

confidence: 99%

Mesospheric Heating during Highly Relativistic Electron Precipitation Events.

Goldberg

Baker

Herrero

et al. 1995

J. geomagn. geoelec

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“…Here a decrease of [O 3 ] by about an order of magnitude (O 3 -profiles 1-4) causes enhancement of the electron density by a factor ∼1.5-2. The maximum deviations in [O 3 ], between our hypothetical O 3 -profile 4 and the O 3 -profile 5 taken from the neutral chemistry model by Swider and Keneshea (1973) and the O 3 -profile 6 from Weeks et al (1972), are about a factor 2 and a factor ∼4.5, respectively. It is seen that they do not lead to such large differences in the value of N e .…”

Section: Ion Composition and Electron Density For Different Concentramentioning

confidence: 87%

“…Figure 1 presents examples of the height distribution of the O 3 concentration in the mesosphere during daytime, obtained from measurements and as a result of theoretical studies. Measurements show substantial diurnal variations at mesospheric altitudes with maximum concentrations at nighttime and a secondary peak above 80 km (Llewellyn and Witt, 1977;Weeks et al, 1972Weeks et al, , 1978Wilson and Schwartz, 1981;Ulwick et al, 1987;Zommerfields et al, 1989;Zhou et al, 1998;Sandor et al, 1997;Gumbel et al, 1998;Fussen et al, 2000;Kaufmann et al, 2003;Polyakov et al, 2005;Kyrölä et al, 2006).…”

Section: Height Profiles Of Ozone In the Mesospherementioning

confidence: 99%

“…1 represents the height distribution of ozone decreased below 80 km altitude by a factor 2 compared with the minimum model O 3 -concentrations for quiet conditions (Swider and Keneshea, 1973;Rodrigo et al, 1986). The O 3 -profiles 5 and 6 represent O 3 concentrations in the mesosphere obtained in a neutral chemistry model for the SPE-disturbed D-region (Swider and Keneshea, 1973;Swider et al, 1978) and measured by Weeks et al (1972) during the SPE in November 1969.…”

Section: Height Profiles Of Ozone In the Mesospherementioning

confidence: 99%

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The influence of ozone concentration on the lower ionosphere – modelling and measurements during the 29–30 October 2003 solar proton event

2009

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Abstract.A numerical model of D-region ion chemistry is used to study the influence of the ozone concentration in the mesosphere on ion-composition and electron density during solar proton events (SPE). We find a strong sensitivity in the lower part of the D-region, where negative ions play a major role in the ionization balance. We have chosen the strong SPE on 29-30 October 2003 when very intense proton fluxes with a hard energetic spectrum were observed. Deep penetration into the atmosphere by the proton fluxes and strong ionisation allows us to use measurements of electron density, made by the EISCAT 224 MHz radar, starting from as low as 55 km. We compare the electron density profiles with model results to determine which ozone concentration profiles are the most appropriate for mesospheric altitudes under SPE conditions. We show that, during daytime, an ozone profile corresponding to depletion by a factor of 2 compared to minimum model concentrations for quiet conditions (Rodrigo et al., 1986), is needed to give model electron density profiles consistent with observations. Simple incorporation of minor neutral constituent profiles (NO, O and O 3 ) appropriate for SPE conditions into ion-chemistry models will allow more accurate modeling of electron and ion densities during such events, without the need to apply a complete chemical model calculating all neutral species.

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“…These protons can impact the neutral middle atmosphere (stratosphere and mesosphere) and produce both HO, (H, OH, HOz) and NO, (N, NO, NOz, N03, NzO~, HNO3, HOzN02, CIONO2, BrONOZ) constituents either directly or through a photochemical sequence (e.g., Swider and Keneshea, 1973;Crutzen et al, 1975;Jackman et al, 1980;McPeters, 1986;Zadorozhny et al, 1992). Ozone is also impacted by the solar protons through direct photochemical destruction forced by the HO, and NO, enhancements (e.g., Weeks et al, 1972;Heath et al, 1977;Solomon et al, 1983;Jackman et al, 1990).…”

Section: Introductionmentioning

confidence: 99%