Characteristics of planetary-scale waves simulated by a new venusian mesosphere and thermosphere general circulation model

Hoshino, N.; Fujiwara, Hitoshi; Takagi, Masahiro; Takahashi, Yukihiro; Kasaba, Yasumasa

doi:10.1016/j.icarus.2011.06.039

Cited by 25 publications

(52 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The wave imposed at the lower boundary would change the structure by the interaction with the background winds as the wave propagates upward. Here it should be noted that Hoshino et al (2012) showed the dominance of the Kelvin wave in the venusian mesosphere. The diurnal and semidiurnal tides given at 80 km lower boundary hardly propagate upward.…”

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 71%

“…We recently developed a novel GCM for the venusian mesosphere and thermosphere including the altitude region of 80-180 km (Hoshino et al, 2012). We performed two GCM simulations in order to investigate effects of the planetary-scale wave and mesoscale gravity wave on the temporal variations of mesospheric winds.…”

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 99%

“…We adopt an O-CO 2 collision energy transfer rate coefficient of 0.9 Â 10 À12 cm 3 /s (Bougher et al, 1986). The Rayleigh friction coefficient at turbopause was set to be 5.0 Â 10 À5 /s in Hoshino et al (2012). Previous simulation studies set the values to be 5.0 Â 10 À5 /s in Brecht and Bougher (2012) and 2.0 Â 10 À4 /s in Mengel et al (1989).…”

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 99%

“…Although various GCMs around the world evolved and improved significantly over recent years, it is noted that several GCMs are limited up to an altitude around 80-100 km (Parish et al, 2011;Lebonnois et al, 2010). Models simulating exclusively the upper atmosphere (Bougher et al, 2006;Brecht and Bougher, 2012;Hoshino et al, 2012;Tingle and Mueller-Wodarg, 2009) have addressed the mesospheric region. Bougher et al (2006) mentioned that GCMs could not reproduce the observed density, temperature, and nightglow variations by using a unique set of wind fields and eddy/wave-drag parameters.…”

Section: Introductionmentioning

confidence: 99%

“…Forbes and Konopliv (2007) suggested the upward propagation of planetary-scale waves in the thermosphere. Hoshino et al (2012) performed GCM simulations considering these planetaryscale waves (thermal tides, Rossby waves, and Kelvin waves) in the venusian mesosphere and thermosphere, and investigated vertical propagation of these planetary-scale waves from 80 km toward 180 km altitude range. They suggested that Kelvin waves, which transport the westward momentum upward, caused the westward atmospheric acceleration but could not reproduce the observed RSZ strength.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

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

Nakagawa

Hoshino

Sornig

et al. 2013

Icarus

View full text Add to dashboard Cite

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 71%

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 99%

Section: Gcm Atmospheric Wave Simulationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

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

Nakagawa

Hoshino

Sornig

et al. 2013

Icarus

View full text Add to dashboard Cite

Modeling VIRTIS/VEX O₂(a1∆g) nightglow profiles affected by the propagation of gravity waves in the Venus upper mesosphere

et al. 2014

View full text Add to dashboard Cite

In this work we describe a model of the perturbation of the O 2 (a 1 Δ g ) nightglow limb profiles by the action of gravity waves (GWs) propagating in the Venus' upper atmosphere. Data have been acquired by the Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS) on board the European Space Agency mission Venus Express (VEX). The high variability observed in the shape of the O 2 (a 1 Δ g ) nightglow limb profiles between 80 and 120 km, often characterized by the presence of a double peak, suggests the occurrence of GWs at the considered altitudes. In order to model and derive the GWs properties, we apply to Venus a well-known theory used to study terrestrial density fluctuations induced by the GWs propagation. The retrieved vertical wavelengths and amplitudes of the waves at the O 2 (a 1 Δ g ) layer altitude (~100 km) are of the order of 7-16 km and 3-14% respectively, complying with wave amplitude threshold for dynamical instability in the majority of the fitted cases. Temperature fluctuations would exceed 40% at higher altitudes (115-120 km) thus inducing either wave breaking or dissipation. Intrinsic horizontal phase velocities are expected to vary in the range 32 m/s and 85 m/s. GWs are detected in a wide range of latitudes from the midlatitudes up to the polar regions, and we cannot exclude existence of the sources of different nature. This study also confirms the high variability induced by the action of GW propagation in the airglow profiles of the terrestrial planets and points out the need for future missions to couple simultaneous complementary GW detection techniques in order to better constrain GW properties and understand their impact on the Venus general circulation.

show abstract

Periodic variations of oxygen EUV dayglow in the upper atmosphere of Venus: Hisaki/EXCEED observations

et al. 2015

View full text Add to dashboard Cite

International audienceUsing the Extreme Ultraviolet Spectroscope for Exospheric Dynamics (EXCEED) aboard Hisaki and the Solar Extreme Ultraviolet Monitor on the Solar and Heliospheric Observatory, we investigate variations of the extreme ultraviolet (EUV) dayglow brightness for OII 83.4 nm, OI 130.4 nm, and OI 135.6 nm in the Venusian upper atmosphere observed in March–April (period 1), April–May (period 2), and June–July (period 3) in 2014. The result shows that characteristic periodicities exist in the dayglow variations other than the ~27 day solar rotational effect of the solar EUV flux: 1.8, 2.8, 3.1, 4.5, and 9.9 day in period 1; 1.1 day in period 2; and 1.0 and 11 day in period 3. Many of these periodicities are consistent with previous observations and theory. We suggest these periodicities are related to density oscillations of oxygen atoms or photoelectrons in the thermosphere. The cause of these periodicities is still uncertain, but planetary-scale waves and/or gravity waves propagating from the middle atmosphere, and/or minor periodic variations of the solar EUV radiation flux may play a role. Effects of the solar wind parameters (velocity, dynamic pressure, and interplanetary magnetic field's intensity) on the dayglow variations are also investigated using the Analyser of Space Plasma and Energetic Atoms (ASPERA-4) and magnetometer aboard Venus Express. Although clear correlation with the dayglow variations is not found, their minor periodicities are similar to the dayglow periodicities. Contribution of the solar wind to the dayglow remains still unknown, but the solar wind parameters might affect the dayglow variations

show abstract

Characteristics of planetary-scale waves simulated by a new venusian mesosphere and thermosphere general circulation model

Cited by 25 publications

References 53 publications

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

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

Modeling VIRTIS/VEX O₂(a1∆g) nightglow profiles affected by the propagation of gravity waves in the Venus upper mesosphere

Periodic variations of oxygen EUV dayglow in the upper atmosphere of Venus: Hisaki/EXCEED observations

Contact Info

Product

Resources

About

Characteristics of planetary-scale waves simulated by a new venusian mesosphere and thermosphere general circulation model

Cited by 25 publications

References 53 publications

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

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

Modeling VIRTIS/VEX O2(a1∆g) nightglow profiles affected by the propagation of gravity waves in the Venus upper mesosphere

Periodic variations of oxygen EUV dayglow in the upper atmosphere of Venus: Hisaki/EXCEED observations

Contact Info

Product

Resources

About

Modeling VIRTIS/VEX O₂(a1∆g) nightglow profiles affected by the propagation of gravity waves in the Venus upper mesosphere