The response of the temperature of cold‐point mesopause to solar activity based on SABER data set

Tang, Chaoli; Liu, Dong; Wei, Heli; Wang, Yingjian; Dai, Congming; Wu, Pengfei; Zhu, Wenyue; Rao, Ruizhong

doi:10.1002/2016ja022538

Cited by 17 publications

(33 citation statements)

References 24 publications

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“…is smaller than the seasonal and daily variations. The OH equivalent temperature solar response is in agreement with that derived by Tang et al (2016) and Kalicinsky et al (2016) (4.89 K per 100 s.f.u. and 4.2 K per 100 s.f.u., respectively) but larger than that of Kim et al (2017) (1.2 K per 100 s.f.u.…”

Section: Sabersupporting

confidence: 89%

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

García‐Comas¹,

López-González²,

González‐Galindo³

et al. 2017

Ann. Geophys.

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Abstract. The mesospheric OH layer varies on several timescales, primarily driven by variations in atomic oxygen, temperature, density and transport (advection). Vibrationally excited OH airglow intensity, rotational temperature and altitude are closely interrelated and thus accompany each other through these changes. A correct interpretation of the OH layer variability from airglow measurements requires the study of the three variables simultaneously. Ground-based instruments measure excited OH intensities and temperatures with high temporal resolution, but they do not generally observe altitude directly. Information on the layer height is crucial in order to identify the sources of its variability and the causes of discrepancies in measurements and models. We have used SABER space-based 2002-2015 data to infer an empirical function for predicting the altitude of the layer at midlatitudes from ground-based measurements of OH intensity and rotational temperature. In the course of the analysis, we found that the SABER altitude (weighted by the OH volume emission rate) at midlatitudes decreases at a rate of 40 m decade −1 , accompanying an increase of 0.7 % decade −1 in OH intensity and a decrease of 0.6 K decade −1 in OH equivalent temperature. SABER OH altitude barely changes with the solar cycle, whereas OH intensity and temperature vary by 7.8 % per 100 s.f.u. and 3.9 K per 100 s.f.u., respectively. For application of the empirical function to Sierra Nevada Observatory SATI data, we have calculated OH intensity and temperature SATI-to-SABER transfer functions, which point to relative instrumental drifts of −1.3 % yr −1 and 0.8 K yr −1 , respectively, and a temperature bias of 5.6 K. The SATI predicted altitude using the empirical function shows significant short-term variability caused by overlapping waves, which often produce changes of more than 3-4 km in a few hours, going along with 100 % and 40 K changes in intensity and temperature, respectively. SATI OH layer wave effects are smallest in summer and largest around New Year's Day. Moreover, those waves vary significantly from day to day. Our estimations suggest that peak-to-peak OH nocturnal variability, mainly due to wave variability, changes within 60 days at least 0.8 km for altitude in autumn, 45 % for intensity in early winter and 6 K for temperature in midwinter. Plausible upper limit ranges of those variabilities are 0.3-0.9 km, 40-55 % and 4-7 K, with the exact values depending on the season.

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Section: Sabersupporting

confidence: 89%

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

García‐Comas¹,

López-González²,

González‐Galindo³

et al. 2017

Ann. Geophys.

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“…The differences are apparently due to the different altitudes, since the correlation between ozone and temperature increases with increasing altitude in the middle to upper atmosphere (~70 to ~100 km; Huang et al, , ). The ozone density data we analyzed in this paper are located at the mesopause, which has a global average altitude of 95.4 ± 0.5 km (Tang et al, ).…”

Section: Discussionmentioning

confidence: 99%

“…As can be seen from Figures a and b, the 95‐km altitude layer is not only the kinetic temperature minimum region in the middle atmosphere but also the maximum region of ozone VMR in the altitude range from ~25 to ~105 km, circled in blue in Figures a and b. Because the global average altitude of mesopause is around 95.4 ± 0.5 km (Tang et al, ), the blue circle symbols shown in Figures a and b are just around the mesopause region, in which the radiative, chemical, and dynamical processes are vigorous (Beig et al, , ). We have investigated the response of T‐CPM to solar activity in previous paper.…”

Section: Methods Of Data Processing and Analysismentioning

confidence: 99%

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The Responses of Ozone Density to Solar Activity in the Mesopause Region and the Mutual Relationship Based on SABER Measurements During 2002–2016

Tang

Wei

et al. 2018

JGR Space Physics

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This paper is aimed to investigate the mutual relationship between ozone‐density at cold‐point mesopause (O3‐CPM) and solar activity globally using Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) measurements and the 10.7 cm‐solar‐radio‐flux (F10.7) data set. For this purpose, the global latitude regions are divided into 16 latitude bins. The global changes of O3‐CPM are presented in mesopause region during 2002–2016. SABER has documented dramatic variability in O3‐CPM on time scale of the 11‐year solar cycle. The observed changes in the global O3‐CPM correlate well with the changes in solar activity during 2002–2016 with correlation coefficient of 0.92, and the global solar response of O3‐CPM is (20.18 ± 2.24)%/100 solar flux units in mesopause. Then, the latitudinal distribution of O3‐CPM and its solar cycle dependence are presented for 16 latitude bins. The latitudinal correlation analysis shows that the O3‐CPM is significantly correlated to the solar cycle at or above the 95% confidence level for each latitude bin from 84°S to 70°N, and the correlation coefficients are remarkably higher in the southern hemisphere than for corresponding latitudes in the northern hemisphere. The latitudinal distribution of O3‐CPM takes on a W shape on a global scale, and the distribution of solar response of O3‐CPM is seen in a strong south‐north asymmetry between the two hemispheres. The solar response of O3‐CPM in latitudinal distribution decreases gradually from the southern hemisphere to the northern hemisphere, and the standard deviation of solar response increases gradually from the equator to the pole in each hemisphere.

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“…In their review, Beig et al (2008) list numerous studies showing that the response of the mesospherelow thermosphere temperature to the change in solar activity reaches 4-5 K / 100 SFU, where SFU is the solar radio flux at a wavelength of 10.7 cm in 10 −22 W M −2 Hz −1 (F10.7). Tang et al (2016) estimated the change in the temperature of the mesopause from 2002 to 2015 using the measurements of the SABER radiometer on board the TIMED satellite. They showed that the average global response is about 5 K/100 SFU, in agreement with the results given in the review of Beig et al (2008).…”

Section: Introductionmentioning

confidence: 99%

Influence of geomagnetic activity on mesopause temperature over Yakutia

Gavrilyeva

Аммосов

2018

Atmos. Chem. Phys.

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Abstract. The long-term temperature changes of the mesopause region at the hydroxyl molecule OH (6-2) nighttime height and its connection with the geomagnetic activity during the 23rd and beginning of the 24th solar cycles are presented. Measurements were conducted with an infrared digital spectrograph at the Maimaga station (63 • N, 129.5 • E). The hydroxyl rotational temperature (TOH) is assumed to be equal to the neutral atmosphere temperature at the altitude of ∼ 87 km. The average temperatures obtained for the period 1999 to 2015 are considered. The season of observations starts at the beginning of August and lasts until the middle of May. The maximum of the seasonally averaged temperatures is delayed by 2 years relative to the maximum of the solar radio emission flux (wavelength of 10.7 cm), and correlates with a change in geomagnetic activity (Ap index). Temperature grouping in accordance with the geomagnetic activity level showed that in years with high activity (Ap > 8), the mesopause temperature from October to February is about 10 K higher than in years with low activity (Ap < = 8). Cross-correlation analysis showed no temporal shift between geomagnetic activity and temperature. The correlation coefficient is equal to 0.51 at the 95 % level.

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The response of the temperature of cold‐point mesopause to solar activity based on SABER data set

Cited by 17 publications

References 24 publications

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

The Responses of Ozone Density to Solar Activity in the Mesopause Region and the Mutual Relationship Based on SABER Measurements During 2002–2016

Influence of geomagnetic activity on mesopause temperature over Yakutia

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The response of the temperature of cold‐point mesopause to solar activity based on SABER data set

Cited by 17 publications

References 24 publications

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

The Responses of Ozone Density to Solar Activity in the Mesopause Region and the Mutual Relationship Based on SABER Measurements During 2002–2016

Influence of geomagnetic activity on mesopause temperature over Yakutia

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Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)

Mesospheric OH layer altitude at midlatitudes: variability over the Sierra Nevada Observatory in Granada, Spain (37° N, 3° W)