Diurnal variations of mesospheric ozone obtained by ground‐based microwave radiometry

Zommerfelds, W. C.; Künzi, K.; Summers, M. E.; Bevilacqua, R. M.; Strobel, D. F.; Allen, Mark; Sawchuck, W. J.

doi:10.1029/jd094id10p12819

Cited by 69 publications

(78 citation statements)

References 20 publications

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“…The mean diurnal variation for April (Fig. 4b) is in agreement with Zommerfelds et al (1989), who also see a daytime decrease in ozone of −30 % (compared to nighttime ozone) for April 1987 at 56 km above Bern. Ricaud et al (1996) used data from the MLS instrument onboard the UARS satellite and compared the results to two photochemical models and ground-based microwave measurements from Bordeaux observatory (44.8 • N, France) and Table Mountain (34.4 • N, California).…”

Section: Gromossupporting

confidence: 87%

A climatology of the diurnal variations in stratospheric and mesospheric ozone over Bern, Switzerland

et al. 2014

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Abstract. The ground-based radiometer GROMOS, stationed in Bern (47.95 • N, 7.44 • E), Switzerland, has a unique data set: it obtains ozone profiles from November 1994 to present with a time resolution of 30 min and equivalent quality during night-and daytime. Here, we derive a monthly climatology of the daily ozone cycle from 17 years of GRO-MOS observation. We present the diurnal ozone variation of the stratosphere and mesosphere. Characterizing the diurnal cycle of stratospheric ozone is important for correct trend estimates of the ozone layer derived from satellite observations. The diurnal ozone cycle from GROMOS is compared to two models: the Whole Atmosphere Community Climate Model (WACCM) and the Hamburg Model of Neutral and Ionized Atmosphere (HAMMONIA). Generally, observation and models show a good agreement: in the lower mesosphere, daytime ozone is for both GROMOS and models around 25 % less than midnight ozone. In the stratosphere, ozone reaches its maximum in the afternoon showing values several percent larger than the midnight value. Further, GROMOS and models indicate a seasonal behaviour of the diurnal ozone variations in the stratosphere with a larger afternoon maximum during daytime in summer than in winter. Using the 17 years of ozone profiles from GROMOS, we find strong interannual variations in the diurnal ozone cycle for both the stratosphere and the mesosphere. Interannual variability in temperature, atmospheric circulation and composition may explain the observed interannual variability of the diurnal ozone cycle above Bern.

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Section: Gromossupporting

confidence: 87%

A climatology of the diurnal variations in stratospheric and mesospheric ozone over Bern, Switzerland

et al. 2014

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“…Measurements (Zommerfields et al, 1989;Fussen et al, 2000;Kaufmann et al, 2003;Polyakov et al, 2005) and theoretical investigations Laird, 1970, 1972;Thomas and Bowman, 1972;Zadorozhny, 1982;Rodrigo et al, 1986;Sandor et al, 1997) show substantial diurnal variations of ozone concentration with maximum values at nighttime. Theoretical values of ozone numerical density are rather close to experimental values.…”

Section: Fig 1amentioning

confidence: 94%

Electron density profiles in the quiet lower ionosphere based on the results of modeling and experimental data

et al. 2012

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Abstract. The theoretical PGI (Polar Geophysical Institute) model for the quiet lower ionosphere has been applied for computing the ionization rate and electron density profiles in the summer and winter D-region at solar zenith angles less than 80 • and larger than 99 • under steady state conditions. In order to minimize possible errors in estimation of ionization rates provided by solar electromagnetic radiation and to obtain the most exact values of electron density, each wavelength range of the solar spectrum has been divided into several intervals and the relations between the solar radiation intensity at these wavelengths and the solar activity index F 10.7 have been incorporated into the model. Influence of minor neutral species (NO, H 2 O, O, O 3 ) concentrations on the electron number density at different altitudes of the sunlit quiet D-region has been examined. The results demonstrate that at altitudes above 70 km, the modeled electron density is most sensitive to variations of nitric oxide concentration. Changes of water vapor concentration in the whole altitude range of the mesosphere influence the electron density only in the narrow height interval 73-85 km. The effect of the change of atomic oxygen and ozone concentration is the least significant and takes place only below 70 km.Model responses to changes of the solar zenith angle, solar activity (low-high) and season (summer-winter) have been considered. Modeled electron density profiles have been evaluated by comparison with experimental profiles available from the rocket measurements for the same conditions. It is demonstrated that the theoretical model for the quiet lower ionosphere is quite effective in describing variations in ionization rate, electron number density and effective recombination coefficient as functions of solar zenith angle, solar activity and season. The model may be used for solving inverse tasks, in particular, for estimations of nitric oxide concentration in the mesosphere.

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“…Comparing Figure 5d with Figure 7a shows that the diurnal ozone variations are very similar to those of O x below 48 km (i.e., O x % O 3 ). Above this level, diurnal variations in ozone are predominantly caused by partitioning between O and O 3 [Vaughan, 1982;Zommerfelds et al, 1989], as outlined in section 1.…”

Section: Photochemical and Dynamical Contributions To Diurnal Ozone Vmentioning

confidence: 99%

“…[3] Diurnal variations in the upper stratosphere and mesosphere have been extensively studied because of their large amplitude (>10% to the daily mean) [Vaughan, 1982;Zommerfelds et al, 1989;Ricaud et al, 1996;Marsh et al, 2002;Schneider et al, 2005;Huang et al, 2008;Dikty et al, 2010]. At these altitudes, ozone levels show a strong depletion during the daytime but then recover at night.…”

Section: Introductionmentioning

confidence: 99%

Diurnal ozone variations in the stratosphere revealed in observations from the Superconducting Submillimeter‐Wave Limb‐Emission Sounder (SMILES) on board the International Space Station (ISS)

et al. 2013

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[1] Considerable uncertainties remain in the global pattern of diurnal variation in stratospheric ozone, particularly lower to middle stratospheric ozone, which is the principal contributor to total column ozone. The Superconducting Submillimeter-Wave LimbEmission Sounder (SMILES) attached to the Japanese Experiment Module (JEM) on board the International Space Station (ISS) was developed to gather high-quality global measurements of stratospheric ozone at various local times, with the aid of superconducting mixers cooled to 4K by a compact mechanical cooler. Using the SMILES dataset, as well as data from nudged chemistry-climate models (MIROC3.2-CTM and SD-WACCM), we show that the SMILES observational data have revealed the global pattern of diurnal ozone variations throughout the stratosphere. We also found that these variations can be explained by both photochemistry and dynamics. The peak-to-peak difference in the stratospheric ozone mixing ratio (total column ozone) reached 8% (1%) over the course of a day. This variation needs to be considered when merging ozone data from different satellite measurements and even from measurements made using one specific instrument at different local times.

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Diurnal variations of mesospheric ozone obtained by ground‐based microwave radiometry

Cited by 69 publications

References 20 publications

A climatology of the diurnal variations in stratospheric and mesospheric ozone over Bern, Switzerland

A climatology of the diurnal variations in stratospheric and mesospheric ozone over Bern, Switzerland

Electron density profiles in the quiet lower ionosphere based on the results of modeling and experimental data

Diurnal ozone variations in the stratosphere revealed in observations from the Superconducting Submillimeter‐Wave Limb‐Emission Sounder (SMILES) on board the International Space Station (ISS)

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