Mesospheric ozone changes associated with 27 day solar ultraviolet flux variations

Aikin, A. C.; Smith, Henry J.

doi:10.1029/gl013i005p00427

Cited by 10 publications

(9 citation statements)

References 13 publications

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“…Another approach is to perform cross-spectral analysis Hood, 1986;Eckman, 1985;Aikin and Smith, 1986] of two of the data sets. However, this approach requires long time series for good spectral resolutions and is much more affected by the methods by which data gaps are filled.…”

Section: Satellite Data Analysismentioning

confidence: 99%

“…The method by which this can be accomplished is included in section 4.1. [Hood, 1986], Nimbus 4 BUV [Chandra, 1985], SME UV [Eckman, 1986], and SME IR [Aikin and Smith, 1986]. The response of ozone to 205-nm solar variability during the LIMS data interval was clearly detected when temperature effects were removed from the ozone data (see Figure 2 Table 2].…”

Section: Satellite Data Analysismentioning

confidence: 99%

“…Both SME ozone data sets give limited longitudinal coverage, and this can lead to misinterpretation of results if, for example, a transient wave passes through the band of longitudes where measurements are obtained. Aikin and Smith [1986] indicated inconsistencies between O3/UV results they obtained over various time intervals of the SME IR data. This is probably an indication of substantial noise as well as extraneous effects brought about by the limited longitudinal coverage.…”

Section: /Uv Relationmentioning

confidence: 99%

“…Thus we chose to analyze as large a set of SME IR data as was available. Aikin and Smith [1986] analyzed bands _+ 2.5 ø in latitude for 110 and 244-day cases. On the other hand, we analyze here a band extending between _+40 ø in latitude for over 655 days, which corresponds to a factor of 95 more data than an Aikin and Smith 110-day case.…”

Section: /Uv Relationmentioning

confidence: 99%

“…Ozone peaked many days before the solar UV maximized, and although a small negative lag can occur if temperatures are rising at the time of the solar UV peak, the magnitude of the lags that Eckman notes are in some cases inconsistent with theory as well as with other measurements. Aikin and Smith [1986] have attempted to use SME 1.27-/•m data to study mesospheric ozone and see some evidence of a 27-day signal, but two independent data sets give inconsistent results, probably due to the noise in the limited data sets. In this paper we use essentially the approach we developed for the LIMS data to study the Nimbus 7 SBUV and SME 1.27-/•m ozone data, in an effort to obtain a self-consistent picture of the response of ozone to solar UV variability.…”

Section: Introductionmentioning

confidence: 98%

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Response of middle atmosphere to short‐term solar ultraviolet variations: 1. Observations

Keating¹,

Pitts²,

Brasseur³

et al. 1987

J. Geophys. Res.

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A series of studies were performed concerning the response of low‐latitude ozone and temperature in the stratosphere and mesosphere to short‐term solar ultraviolet variability associated with the rotation of the sun. The studies are based on Nimbus 7 Limb Infrared Monitor of the Stratosphere (LIMS) stratospheric ozone and temperature data, Nimbus 7 solar backscattered ultraviolet (SBUV) stratospheric ozone and 205‐nm solar ultraviolet data, Solar Mesosphere Explorer (SME) 1.27‐μm mesospheric O3 data, SME 121.6‐nm solar ultraviolet data, and Nimbus 7 Stratosphere and Mesosphere Sounder (SAMS) stratospheric and mesospheric temperature data. Using a longer temperature time series than has been used in the past for such studies, response times of temperature to solar UV variability in the stratosphere are found to be unexpectedly long (6 days at 2 mbar) and to become much shorter in the mesosphere (1 day at 0.01 mbar). Maximum sensitivity of temperature to solar variability (0.3 K/percent 205‐nm radiation) is found to occur near 70 km. The coupling of the temperature and ozone response to solar UV variability has been isolated by studying ozone responses with and without temperature effects. Temperature effects tend to increase rather than decrease the amplitude and to shift the response time of stratospheric ozone to solar variability to an earlier time. Using a longer ozone time series than has been used in the past for such studies, the stratospheric ozone response with no correction for temperature effects is found to be approximately a 0.4% increase at 3 mbar for a 1.0% increase in 205‐nm solar radiation. In the mesosphere a major systematic ozone decrease has been detected near 0.05 mbar (∼70 km), with increased solar Lyman α (121.6 nm) radiation (−0.14% ozone decrease for a 1% increase in solar Lyman α). This may be caused by solar Lyman α photodissociating H2O vapor producing HOx, with subsequent destruction of Ox. Higher in the mesosphere, where H2O mixing ratios should be much lower, ozone is found to increase with increasing solar UV. Observed responses of HNO3 and NO2 to solar UV variability are also briefly discussed. The theoretical response of middle atmosphere species and temperature to solar UV variability is discussed in detail in a companion paper (Brasseur et al., this issue).

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Section: Satellite Data Analysismentioning

confidence: 99%

Section: Satellite Data Analysismentioning

confidence: 99%

Section: /Uv Relationmentioning

confidence: 99%

Section: /Uv Relationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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Response of middle atmosphere to short‐term solar ultraviolet variations: 1. Observations

Keating¹,

Pitts²,

Brasseur³

et al. 1987

J. Geophys. Res.

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Middle atmosphere change through solar forcing

Keating

Chen²

1991

Advances in Space Research

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Nighttime Mesospheric/Lower Thermospheric Tropical Ozone Response to the 27‐Day Solar Rotational Cycle: ENVISAT‐GOMOS Satellite Observations Versus HAMMONIA Idealized Chemistry‐Climate Model Simulations

et al. 2018

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Global Ozone Monitoring by Occultation of Stars (GOMOS) satellite data are analyzed to estimate the first observation‐based nighttime (22:00 median local time) ozone response to the 27‐day solar rotational cycle in the tropical mesosphere/lower thermosphere (50–110 km altitude). The ozone response to solar rotational variability is derived from linear correlation and regressions using Lyman‐α line (121.6 nm) as solar index that varies by about 10–15% over solar rotational cycles. In the lower mesosphere (50–70 km), the GOMOS ozone is found to be correlated with the solar fluctuations and exhibits a sensitivity of ~0.1 (expressed in percent change of ozone for 1% change in Lyman‐α). In the upper mesosphere/lower thermosphere (above 80 km), ozone variations become anticorrelated with solar rotational variations. In this region, the vertical profile of ozone sensitivity to the 27‐day solar cycle exhibits a maximum of 1.8 at 81 km, a minimum of 0.3 at 100 km, and a sharp increase above. Such high ozone sensitivities are observed for the first time. The observed ozone response is compared with chemistry‐climate simulations from the Hamburg model of the neutral and ionized atmosphere (HAMMONIA) that is forced with an idealized 27‐day solar spectral irradiance time series. Although observational and model results share some common features, substantial discrepancies are found. Namely, the altitude of transition from positive to negative solar ozone correlation signal in the model simulation is found about 10 km below the altitude of the observations and the amplitude of the ozone sensitivity is generally vastly underestimated by the model.

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Mesospheric ozone changes associated with 27 day solar ultraviolet flux variations

Cited by 10 publications

References 13 publications

Response of middle atmosphere to short‐term solar ultraviolet variations: 1. Observations

Response of middle atmosphere to short‐term solar ultraviolet variations: 1. Observations

Middle atmosphere change through solar forcing

Nighttime Mesospheric/Lower Thermospheric Tropical Ozone Response to the 27‐Day Solar Rotational Cycle: ENVISAT‐GOMOS Satellite Observations Versus HAMMONIA Idealized Chemistry‐Climate Model Simulations

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