Planetary wave trends in the lower thermosphere—Evidence for 22-year solar modulation of the quasi 5-day wave

Jarvis, M. J.

doi:10.1016/j.jastp.2006.02.014

Cited by 26 publications

(18 citation statements)

References 38 publications

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“…6a as a blue curve; the orange curve marks the solar F10.7 cm flux). Our finding is supported through the work of Jarvis (2006) who recently analyzed geomagnetic data from five northern hemisphere observatories extending back over eight 11-year solar cycles. He found an evidence for a 22-year solar modulation of the quasi 5-day wave.…”

Section: Article In Presssupporting

confidence: 83%

Evidence for solar signals in the mesopause temperature variability?

Höppner

Bittner

2007

Journal of Atmospheric and Solar-Terrestrial Physics

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Section: Article In Presssupporting

confidence: 83%

Evidence for solar signals in the mesopause temperature variability?

Höppner

Bittner

2007

Journal of Atmospheric and Solar-Terrestrial Physics

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“…It is now well accepted that the geomagnetic activity variations play an important role in the generation of the PWS in the ionosphere. Recent investigations have shown that geomagnetic activity can drive PWS in the ionospheric F-region (Xiong et al, 2006;Jarvis, 2006), supporting previous results which indicate that geomagnetic activity variations can be one of the main sources of the PWS in the ionosphere Apostolov, 2001, 2003).…”

Section: Introductionsupporting

confidence: 76%

Upper ionosphere variability over Alma-Ata and Observatorio Del Ebro using the ΔfoF2 data obtained during the winter/spring period of 2003–2004

Gordienko

Fedulina

Altadill

et al. 2007

Journal of Atmospheric and Solar-Terrestrial Physics

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“…Such oscillations were recently discovered by Offermann et al (2015). An oscillation with a period of about 20 to 25 years is found in various atmospheric parameters such as temperature (Qu et al, 2012;Wei et al, 2015), geopotential height (Coughlin and Tung, 2004a, b), and planetary wave activity (Jarvis, 2006;Höppner and Bittner, 2007). It is also seen in two atmospheric models (HAMMONIA, WACCM).…”

Section: Long-term Oscillationmentioning

confidence: 83%

Long-term dynamics of OH * temperatures over central Europe: trends and solar correlations

et al. 2016

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Abstract. We present the analysis of annual average OH * temperatures in the mesopause region derived from measurements of the Ground-based Infrared P-branch Spectrometer (GRIPS) at Wuppertal (51 • N, 7 • E) in the time interval 1988 to 2015. The new study uses a temperature time series which is 7 years longer than that used for the latest analysis regarding the long-term dynamics. This additional observation time leads to a change in characterisation of the observed longterm dynamics.We perform a multiple linear regression using the solar radio flux F10.7 cm (11-year cycle of solar activity) and time to describe the temperature evolution. The analysis leads to a linear trend of (−0.089 ± 0.055) K year −1 and a sensitivity to the solar activity of (4.2 ± 0.9) K (100 SFU) −1 (r 2 of fit 0.6). However, one linear trend in combination with the 11-year solar cycle is not sufficient to explain all observed long-term dynamics. In fact, we find a clear trend break in the temperature time series in the middle of 2008. Before this break point there is an explicit negative linear trend of (−0.24 ± 0.07) K year −1 , and after 2008 the linear trend turns positive with a value of (0.64 ± 0.33) K year −1 . This apparent trend break can also be described using a long periodic oscillation. One possibility is to use the 22-year solar cycle that describes the reversal of the solar magnetic field (Hale cycle). A multiple linear regression using the solar radio flux and the solar polar magnetic field as parameters leads to the regression coefficients C solar = (5.0 ± 0.7) K (100 SFU) −1 and C hale = (1.8 ± 0.5) K (100 µT) −1 (r 2 = 0.71). The second way of describing the OH * temperature time series is to use the solar radio flux and an oscillation. A leastsquare fit leads to a sensitivity to the solar activity of (4.1 ± 0.8) K (100 SFU) −1 , a period P = (24.8 ± 3.3) years, and an amplitude C sin = (1.95 ± 0.44) K of the oscillation (r 2 = 0.78). The most important finding here is that using this description an additional linear trend is no longer needed. Moreover, with the knowledge of this 25-year oscillation the linear trends derived in this and in a former study of the Wuppertal data series can be reproduced by just fitting a line to the corresponding part (time interval) of the oscillation. This actually means that, depending on the analysed time interval, completely different linear trends with respect to magnitude and sign can be observed. This fact is of essential importance for any comparison between different observations and model simulations.

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Planetary wave trends in the lower thermosphere—Evidence for 22-year solar modulation of the quasi 5-day wave

Cited by 26 publications

References 38 publications

Evidence for solar signals in the mesopause temperature variability?

Evidence for solar signals in the mesopause temperature variability?

Upper ionosphere variability over Alma-Ata and Observatorio Del Ebro using the ΔfoF2 data obtained during the winter/spring period of 2003–2004

Long-term dynamics of OH * temperatures over central Europe: trends and solar correlations

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