Simultaneous observations of the phase‐locked 2 day wave at Adelaide, Cerro Pachon, and Darwin

Walterscheid, R. L.; Hecht, J. H.; Gelinas, L. J.; MacKinnon, Andrew D.; Vincent, R. A.; Franke, Steven; Zhao, Yucheng; Taylor, Michael J.; Pautet, Pierre-Dominique

doi:10.1002/2014jd022016

Cited by 9 publications

(8 citation statements)

References 49 publications

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“…Craig and Elford (1981) explored phase locking relative to the sun and suggested nonlinear interactions with diurnal tides. This is also supported by recent studies (e.g., Huang et al, 2013a;Moudden and Forbes, 2014;Walterscheid et al, 2015). A possible correlation of QTDW amplitudes with the 11-year solar cycle has been found by Jacobi et al (1997), who explained this finding by a stronger mesospheric wind shear during solar maximum.…”

supporting

confidence: 75%

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Meteor radar quasi 2-day wave observations over 10 years at Collm (51.3° N, 13.0° E)

Lilienthal

Jacobi

2015

Atmos. Chem. Phys.

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Abstract. The quasi 2-day wave (QTDW) at 82-97 km altitude over Collm (51 • N, 13 • E) has been observed using a VHF meteor radar. The long-term mean amplitudes calculated using data between September 2004 and August 2014 show a strong summer maximum and a much weaker winter maximum. In summer, the meridional amplitude is slightly larger than the zonal one with about 15 m s −1 at 91 km height. Phase differences are slightly greater than 90 • on an average. The periods of the summer QTDW vary between 43 and 52 h during strong bursts, while in winter the periods tend to be more diffuse. On average, the summer QTDW is amplified after a maximum of zonal wind shear which is connected with the summer mesospheric jet and there is a possible correlation of the summer mean amplitudes with the background wind shear. QTDW amplitudes exhibit considerable inter-annual variability; however, a relationship between the 11-year solar cycle and the QTDW is not found.

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supporting

confidence: 75%

“…The last group covers periods longer than 48 h and peaks at 52 h with wave numbers 2 and 3. In the SH these three groups could not be observed and periods are close to 48 h with wave number 3 (Wu et al, 1996;Walterscheid et al, 2015). Craig and Elford (1981) explored phase locking relative to the sun and suggested nonlinear interactions with diurnal tides.…”

mentioning

confidence: 99%

Meteor radar quasi 2-day wave observations over 10 years at Collm (51.3° N, 13.0° E)

Lilienthal

Jacobi

2015

Atmos. Chem. Phys.

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“…Nonlinear interaction with especially the diurnal and semidiurnal tides (e.g., Palo et al, 1999) could explain this behavior. In this context, phase locking, which would significantly weaken the diurnal tide (Walterscheid & Vincent, 1996;Hecht et al, 2010;Walterscheid et al, 2015), did not seem to be active at Cerro Paranal during the considered time interval as periods very close to 48 h cannot explain the time series. The LT dependence of the Q2DW amplitude in OH emission might also be affected by the negative nocturnal trend of atomic oxygen (produced at daytime) that would always be present without vertical dynamics especially at the lowest OH emission altitudes (Marsh et al, 2006).…”

Section: Oh Linesmentioning

confidence: 90%

“…The so-called quasi-2-day wave (Q2DW) can achieve very high amplitudes in the mesopause region at low to middle latitudes. In particular, strong Q2DWs occur in the Southern Hemisphere for several weeks in the summer months January and February (e.g., Ern et al, 2013;Gu et al, 2019;Tunbridge et al, 2011;Walterscheid et al, 2015). The period is close to 2 days but can vary from 42 to 54 h (Gu et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

Vertical layering of OH line emission from X-shooter and SABER observations of a passing quasi-2-day wave

Noll

Kausch

Schmidt

et al. 2022

Preprint

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<p>The nighttime near-infrared radiation of the Earth's atmosphere is mainly produced in the mesopause region between 80 and 100 km by chemiluminescent emission of the OH radical. The line radiation of various vibrational and rotational states is therefore a valuable indicator of the chemistry and dynamics in the upper atmosphere. The vertical emission distribution can significantly change with time. It is also expected that the time-averaged effective emission height depends on the studied OH line due to differences in the radiative lifetimes, the collision-related transition probabilities, and the initial level population after the production of the radical. Although the knowledge of the OH emission layering is important for the interpretation of passing perturbations, the line-specific details are still uncertain.&#160;</p><p>We have studied the effective emission heights of about 300 OH lines based on near-infrared spectroscopic data from the X-shooter spectrograph at the Very Large Telescope at Cerro Paranal in Chile. The line intensities showed very strong variations due to a rising quasi-two day wave during eight nights at the beginning of 2017. With complementary vertically resolved broad-band observations of OH emission from the limb-sounder SABER on the TIMED satellite, we could link the line-dependent wave phases from the fitting of the X-shooter data with emission altitudes. With a period of about 44 h and a vertical wavelength of about 32 km, the observed wave turned out to be an excellent indicator of line-dependent altitude differences, which reached up to 8 km for the investigated lines. In general, the effective emission altitude increases with increasing vibrational and rotational level. Moreover, the derived wave amplitudes imply the presence of a cold thermalised and a hot non-thermalised population for each vibrational level. As the wave amplitudes also showed a strong dependence on local time, significant interactions between the quasi-two-day wave and other perturbations such as tides are likely.</p>

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“…Due to their relatively low phase speeds, PWs are prone to filtering by the background wind field before reaching the MLT region. Nonetheless, mesospheric PWs have been observed utilizing satellite and ground‐based measurements at all latitudes in mesospheric wind and temperature data (e.g., Lieberman & Riggin, ; Luo et al, ; Murphy et al, ; Riggin et al, ; Sivjee et al, ; Walterscheid et al, ; Wu et al, ).…”

Section: Introductionmentioning

confidence: 99%

Investigating an Unusually Large 28‐Day Oscillation in Mesospheric Temperature Over Antarctica Using Ground‐Based and Satellite Measurements

et al. 2019

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The Utah State University Advanced Mesospheric Temperature Mapper was deployed at the Amundsen-Scott South Pole Station in 2010 to measure OH temperature at~87 km as part of an international network to study the mesospheric dynamics over Antarctica. During the austral winter of 2014, an unusually large amplitude~28-day oscillation in mesospheric temperature was observed for~100 days from the South Pole Station. This study investigates the characteristics and global structure of this exceptional planetary-scale wave event utilizing ground-based mesospheric OH temperature measurements from two Antarctic stations (South Pole and Rothera) together with satellite temperature measurements from the Microwave Limb Sounder on the Aura satellite and the Solar Occultation For Ice Experiment on the Aeronomy of Ice in the Mesosphere satellite. Our analyses have revealed that this large oscillation is a wintertime, high-latitude phenomenon, exhibiting a coherent zonal wave #1 structure below 80-km altitude. At higher altitudes, the wave was confined in longitude between 180°E and 360°E. The amplitude of this oscillation reached~15 K at 85 km, and it was observed to grow with altitude as it extended from the stratosphere into the lower thermosphere in the Southern Hemisphere. The satellite data further established the existence of this oscillation in the Northern Hemisphere during the boreal wintertime. The main characteristics and global structure of this event as observed in temperature are consistent with the predicted 28-day Rossby Wave (1,4) mode.

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Simultaneous observations of the phase‐locked 2 day wave at Adelaide, Cerro Pachon, and Darwin

Cited by 9 publications

References 49 publications

Meteor radar quasi 2-day wave observations over 10 years at Collm (51.3° N, 13.0° E)

Meteor radar quasi 2-day wave observations over 10 years at Collm (51.3° N, 13.0° E)

Vertical layering of OH line emission from X-shooter and SABER observations of a passing quasi-2-day wave

Investigating an Unusually Large 28‐Day Oscillation in Mesospheric Temperature Over Antarctica Using Ground‐Based and Satellite Measurements

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