Simultaneous in situ measurements of small-scale structures in neutral, plasma, and atomic oxygen densities during the WADIS sounding rocket project

Strelnikov, Boris; Eberhart, Martin; Friedrich, Martin; Hedin, Jonas; Khaplanov, Mikhail; Baumgarten, Gerd; Williams, B. P.; Staszak, Tristan; Asmus, Heiner; Strelnikova, Irina; Latteck, R.; Grygalashvyly, M.; Lübken, Franz‐Josef; Höffner, J.; Wörl, Raimund; Gumbel, J.; Löhle, Stefan; Fasoulas, Stefanos; Rapp, Markus; Barjatya, Aroh; Taylor, Michael J.; Pautet, Pierre-Dominique

doi:10.5194/acp-19-11443-2019

Cited by 11 publications

(9 citation statements)

References 90 publications

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“…(2012, 2013) and Strelnikov et al. (2019) at ∼69°N above Andøya, Norway. The (thin) blue dashed line was calculated for H' = 77 km and β = 0.7 km −1 for comparison with the slope of the H' = 77 km and β = 0.6 km −1 mean winter solid blue line and the slopes of the rocket observations.…”

Section: Comparisons With Others and Electron Number Densitiesmentioning

confidence: 88%

“…(2013) (F13), and Strelnikov et al. (2019) (S19). The straight red dashed line is a ( H ′, β ) best fit to the rocket profile of December 4, 2010.…”

Section: Comparisons With Others and Electron Number Densitiesmentioning

confidence: 99%

“…The solid lines are the mean values, from the VLF observations reported here, for equinox (green) and winter (blue) while the dashed green lines are for the equinoctial upper and lower 10-percentile values determined in Section 2.2 and illustrated in Figures 3a and 3b. The dated dotted curves are from the rocket MF/HF radio wave propagation measurements of Friedrich et al (2012Friedrich et al ( , 2013 and Strelnikov et al (2019) at ∼69°N above Andøya, Norway. The (thin) blue dashed line was calculated for H' = 77 km and β = 0.7 km −1 for comparison with the slope of the H' = 77 km and β = 0.6 km −1 mean winter solid blue line and the slopes of the rocket observations.…”

Section: Electron Number Densitiesmentioning

confidence: 99%

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Quiet Night Arctic Ionospheric D Region Characteristics

et al. 2021

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The lowest region of the Earth's ionosphere (containing free electrons) is the D region with its lower edge at heights generally around 70 km by day and 85 km by night. These heights are too low for satellite measurements (too much drag) and too high for aircraft or balloons. Rocket measurements (e.g., Friedrich & Torkar, 2001;Friedrich et al., 2018) have proved very useful but tend to be too transient and expensive to fully explore the significant diurnal, seasonal, and latitudinal variations around the Earth. Ground-based, high frequency radars (e.g., Singer et al., 2011) have also proved useful when available but are quite rare and are very limited in their geographical coverage. In contrast, very low frequency (VLF) radio waves, particularly from single-frequency, ground-based, man-made transmitters, have good geographical coverage and very good (often continuous) diurnal and seasonal coverage. These waves readily partially reflect from the lower edge of the D region with the resulting amplitude and phase changes being rather sensitive to its height and sharpness. The VLF waves also reflect very well from the Earth's surface, particularly the conducting oceans, enabling them to travel up to large distances (thousands of km) in the Earth-ionosphere waveguide bounded above by the D region.VLF radio subionospheric propagation has been used to refine our knowledge of the daytime D region by taking amplitude and phase measurements along radio paths both near (∼100 km from) the transmitter, where the direct ground wave signal dominates, and at greater distances (from ∼300 km up to several thousand km away) where the waves reflected from the D region dominate. The resulting phase and amplitude changes along the paths were then compared with calculations from VLF subionospheric modeling codes enabling the latitude-dependent characteristics (height and sharpness) of the daytime D region to be inferred, e.g., Thomson (2010) and Thomson et al. (2012Thomson et al. ( , 2014 at low latitudes, Thomson et al. ( , 2017 at midlatitudes, and Thomson et al. (2018) at high latitudes in the Arctic. The current study builds on these earlier studies to examine the nighttime Arctic D region.Diurnal VLF radio propagation recordings have been used to find the characteristics of the nighttime D region of the ionosphere at lower latitudes on a variety of long paths by comparing the observed changes in phase and amplitude between day and night with calculations from VLF propagation codes (Thomson & McRae, 2009;Thomson et al., 2007). For these comparisons the daytime results of Thomson (1993) and McRae and Thomson (2000) were used. In the present paper, we again use single-frequency, diurnal

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Section: Comparisons With Others and Electron Number Densitiesmentioning

confidence: 88%

“…(2013) (F13), and Strelnikov et al. (2019) (S19). The straight red dashed line is a ( H ′, β ) best fit to the rocket profile of December 4, 2010.…”

Section: Comparisons With Others and Electron Number Densitiesmentioning

confidence: 99%

Section: Electron Number Densitiesmentioning

confidence: 99%

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Quiet Night Arctic Ionospheric D Region Characteristics

et al. 2021

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“…The main reason for that was the relative simplicity of implementation and numerical stability of the Heisenberg (1948) model. Staszak et al (2021) and Strelnikov et al (2017Strelnikov et al ( , 2019) applied Lübken's technique utilizing both Heisenberg (1948) and Tatarskii (1971) models and showed that the results can reveal considerable discrepancies as far as absolute ɛ-values are concerned, however yielding very similar relative vertical structure and variability.…”

Section: Spectral Model Techniquementioning

confidence: 99%

Assessment of the Precision of Spectral Model Turbulence Analysis Techniques Using Direct Numerical Simulation Data

Strelnikov

Rapp²,

Fritts

et al. 2022

JGR Atmospheres

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Turbulence measurements in the atmosphere and ocean comprise remote sensing techniques and vast in situ methods. The most detailed picture of turbulence dissipation or intensity fields can only be acquired by in situ measurements. In situ measurement techniques, in turn, utilize different principles depending on altitude (depth) region and consequently its accessibility means.Different physical quantities inside turbulent flows when measured with sufficient precision reveal fluctuations around a mean background value. Spectral analysis of these fluctuations shows that they are distributed in a continuous wavenumber space and might obey a mathematical law called spectrum function. In the case of the velocity fluctuations, one may find spectrum functions which are the Fourier transform of correlation functions (see e.g., Hinze, 1975). Similar functions can also be applied to describe the spectral distribution of other, scalar quantities ϑ, also referred to as tracers. In the general case, these functions are three-dimensional (3D) in space and include time dependency. Most measurement techniques, however, do measure a quasi-instant one-dimensional (1D) cross-section of this 3D spectrum. This technical limitation can normally be circumvented by assuming isotropy of the spectral distribution of the measured fluctuations allowing for 3D-to-1D transform of

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“…While not fully resolvable by models, these subgrid‐scale processes can be observed by various observational techniques, including radar, lidar and rocket measurements (Le Pichon et al., 2015; Rapp & Lübken, 2004; Schäfer et al., 2020; Strelnikov et al., 2019). One such subgrid‐scale phenomenon is atmospheric gravity waves (GWs).…”

Section: Introductionmentioning

confidence: 99%

Probing Gravity Waves in the Middle Atmosphere Using Infrasound From Explosions

et al. 2023

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This study uses low‐frequency, inaudible acoustic waves (infrasound) to probe wind and temperature fluctuations associated with breaking gravity waves (GWs) in the middle atmosphere. Building on an approach introduced by Chunchuzov et al., infrasound recordings are used to retrieve effective sound‐speed fluctuations in an inhomogeneous atmospheric layer that causes infrasound backscattering. The infrasound was generated by controlled blasts at Hukkakero, Finland, and recorded at the IS37 infrasound station, Norway in the late summers 2014–2017. Our findings indicate that the analyzed infrasound scattering occurs at mesospheric altitudes of 50–75 km, a region where GWs interact under non‐linearity, forming thin layers of strong wind shear. The retrieved fluctuations were analyzed in terms of vertical wave number spectra, resulting in an approximate kz−3 ${k}_{z}^{-3}$ power law that corresponds to the “universal” saturated spectrum of atmospheric GWs. The kz−3 ${k}_{z}^{-3}$ power law wavenumber range corresponds to vertical atmospheric scales of 33–625 m. The fluctuation spectra were compared to theoretical GW saturation theories as well as to independent wind measurements by the Saura medium‐frequency radar near Andøya Space Center around 100 km west of IS37, yielding a good agreement in terms of vertical wavenumber spectrum amplitudes and slopes. This suggests that the radar and infrasound‐based effective sound‐speed profiles represent low‐ and high‐wavenumber regimes of the same “universal” GW spectrum. The results illustrate that infrasound allows for probing fine‐scale dynamics not well captured by other techniques, suggesting that infrasound can provide a complementary technique to probe atmospheric GWs.

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Simultaneous in situ measurements of small-scale structures in neutral, plasma, and atomic oxygen densities during the WADIS sounding rocket project

Cited by 11 publications

References 90 publications

Quiet Night Arctic Ionospheric D Region Characteristics

Quiet Night Arctic Ionospheric D Region Characteristics

Assessment of the Precision of Spectral Model Turbulence Analysis Techniques Using Direct Numerical Simulation Data

Probing Gravity Waves in the Middle Atmosphere Using Infrasound From Explosions

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