Comparison of general circulation model atmospheric wave simulations with wind observations of venusian mesosphere

Nakagawa, Hiromu; Hoshino, N.; Sornig, M.; Kasaba, Yasumasa; Sonnabend, G.; Stupar, D.; Aoki, Shohei; Murata, Isao

doi:10.1016/j.icarus.2013.02.029

Cited by 11 publications

(15 citation statements)

References 65 publications

(85 reference statements)

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“…Forbes and Konopliv (2007) suggested that planetary scale waves originating in the cloud layer would propagate to the thermosphere, based on an analysis of data obtained by Magellan. Recent GCM calculations by Hoshino et al (2012) and Nakagawa et al (2013) further suggest that only Kelvin waves propagate up to thermospheric altitudes (up to ∼130 km) with significant amplitudes, and not tides. Rossby waves have small amplitudes at ∼130 km.…”

Section: Gravity Waves: Airglow and Other Signaturesmentioning

confidence: 99%

Aeronomy of the Venus Upper Atmosphere

et al. 2017

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We present aeronomical observations collected using remote sensing instruments on board Venus Express, complemented with ground-based observations and numerical modeling. They are mostly based on VIRTIS and SPICAV measurements of airglow obtained in the nadir mode and at the limb above 90 km. They complement our understanding of the behavior of Venus' upper atmosphere that was largely based on Pioneer Venus observations mostly performed over thirty years earlier. Following a summary of recent spectral data from the EUV to the infrared, we examine how these observations have improved our knowledge of the composition, thermal structure, dynamics and transport of the Venus upper atmosphere. We then synthesize progress in three-dimensional modeling of the upper atmosphere which is largely based on global mapping and observations of time variations of the nitric oxide and O 2 nightglow emissions. Processes controlling the escape flux of atoms to space are described. Results based on the VeRA radio propagation experiment are summarized and compared to ionospheric measurements collected during earlier space missions. Finally, we point out some unsolved and open questions generated by these recent datasets and model comparisons.

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Section: Gravity Waves: Airglow and Other Signaturesmentioning

confidence: 99%

Aeronomy of the Venus Upper Atmosphere

et al. 2017

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“…The realistic amplitude of gravity waves can be obtained for all altitude regions considering the information of gravity waves near the cloud layer, which has recently been obtained from VEX observations. Nakagawa et al [] reported the initial simulation results with the MK scheme, which were used to estimate the amplitude of the wind variations caused by gravity waves. They suggested that gravity waves caused wind variation with an amplitude of ∼15 m/s at the evening terminator in the 110 km altitude region.…”

Section: Introductionmentioning

confidence: 99%

Effects of gravity waves on the day‐night difference of the general circulation in the Venusian lower thermosphere

et al. 2013

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[1] We investigated generation mechanisms of the local time variation of the wind velocity in the Venusian mesosphere and thermosphere, which has been suggested from recent ground-based CO millimeter/submillimeter and CO 2 10 m observations, using our general circulation model. Our model considers the momentum transport caused by gravity waves with the gravity wave parameterization developed by Medvedev and Klaassen (2000). Our results show that atmospheric circulation distinctly changes from the dayside to the nightside. The subsolar-to-antisolar (SSAS) wind is predominant in the dayside. On the other hand, the retrograde superrotating zonal (RSZ) wind is superposed on the SSAS wind in the nightside. These characteristics are consistent with the previous observations. The westward momentum, which drives the RSZ wind in the nightside at an altitude of 110 km, is supplied by gravity waves in the 115-130 km altitude region. The downward flow that originates in the SSAS wind transports the westward momentum downward in the nightside.

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“…For this altitude range, the numerical simulations showed that atmospheric circulation distinctly changes due to the momentum transport from lower atmosphere by an upward propagating gravity wave (GW) (Hoshino et al 2013;Nakagawa et al 2013). An improved version of a ground-to-thermosphere Venus general circulation model (GCM) including a non-orographic GW parameterization developed at Institut Pierre Simon Laplace/ Laboratoire de Météorologie Dynamique (IPSL/LMD) (Gilli et al 2017) provides a better representation of temperature profiles at altitudes above 100 km, such as those observed by the SPICAV (Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Venus) and SOIR (Solar Ocultation at Infrared) instruments on Venus Express.…”

Section: Introductionmentioning

confidence: 98%

“…Goldstein et al (1991) performed the first measurement at this altitude range with heterodyne spectroscopy and obtained a global circulation including SS-AS flow. The dayside non-LTE CO 2 emission lines have been used for the retrieval of wind velocity and temperature profiles in the lower thermosphere at the altitude of 110 ± 10 km (e.g., Krause et al 2018;Nakagawa et al 2013;Sonnabend et al 2008Sonnabend et al , 2010Sonnabend et al , 2012Sornig et al 2008Sornig et al , 2012Sornig et al , 2013.…”

Section: Introductionmentioning

confidence: 99%

Evaluation of a method to retrieve temperature and wind velocity profiles of the Venusian nightside mesosphere from mid-infrared CO2 absorption line observed by heterodyne spectroscopy

Takami

Nakagawa

Sagawa

et al. 2020

Earth Planets Space

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We evaluated a method for retrieving vertical temperature and Doppler wind velocity profiles of the Venusian nightside mesosphere from the CO 2 absorption line resolved by mid-infrared heterodyne spectroscopy. The achievable sensitive altitude and retrieval accuracy were derived with multiple model spectra generated from various temperature and wind velocity profiles with several noise levels. The temperature profiles were retrieved at altitudes of 70-100 km with a vertical resolution of 5 km and a retrieval accuracy of ± 15 K. The wind velocity was also retrieved at an altitude of approximately 85 km with a vertical resolution of 10 km and a retrieval accuracy of ± 25-50 m/s. In addition, we studied an event and applied our method to spectra obtained by the HIPWAC instrument attached to the NASA/IRTF 3-m telescope on May 19-22, 2012. Retrieved wind velocities in a latitude of 33° S at 3:00 LT were interpreted as subsolar-to-antisolar (SS-AS) flows at altitudes of 84 ± 6 km and 94 ± 7 km, and they were stronger than expected. This result suggested that the transition between the retrograde superrotational zonal (RSZ) wind and SS-AS flow may occur at altitudes below 90 km which previously was predicted to be the transition region. This work provides a basis for our analysis of further observations obtained by a mid-infrared heterodyne spectrometer MILAHI attached to the Tohoku University 60-cm telescope at Haleakalā, Hawaii.

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Comparison of general circulation model atmospheric wave simulations with wind observations of venusian mesosphere

Cited by 11 publications

References 65 publications

Aeronomy of the Venus Upper Atmosphere

Aeronomy of the Venus Upper Atmosphere

Effects of gravity waves on the day‐night difference of the general circulation in the Venusian lower thermosphere

Evaluation of a method to retrieve temperature and wind velocity profiles of the Venusian nightside mesosphere from mid-infrared CO2 absorption line observed by heterodyne spectroscopy

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