Wave signature in the Venus dayside cloud layer at 58–64 km observed by ground-based infrared spectroscopy

Hosouchi, M.; Kouyama, T.; Iwagami, N.; Ohtsuki, Shoko; Takagi, Masahiro

doi:10.1016/j.icarus.2012.04.027

Cited by 9 publications

(12 citation statements)

References 28 publications

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“…Kouyama et al (2012a) reported the existence of planetary-scale waves with a rotation period of about 4.4 days from the Galileo spacecraft observations at the cloud top. Hosouchi et al (2012) suggested the wave-like structure with its apparent rotation period of 3.5, 4.9, and 8.4 days found at 58-64 km in the cloud layer. Those apparent periods may be interpreted as superposition of the mean zonal flow and waves such as the Kelvin wave and Rossby wave.…”

Section: Introductionmentioning

confidence: 84%

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

Nakagawa

Hoshino

Sornig

et al. 2013

Icarus

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Section: Introductionmentioning

confidence: 84%

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

Nakagawa

Hoshino

Sornig

et al. 2013

Icarus

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“…However, GCM studies indicate the existence of barotropic or baroclinic waves with periods ranging from 6-23 days (Lebonnois et al 2016) in the cloud layer, which is another possibility for the 8 day signature. An ∼ 8 day period wave was observed a little deeper than cloud top level in nearinfrared observations (∼1.7 micron), and is also thought to result from the interaction of Kelvin and Rossby waves with the mean flow (Hosouchi et al 2012).…”

Section: Physical Interpretations Of the Oscillations At 283-nmmentioning

confidence: 99%

Principal components of short-term variability in the ultraviolet albedo of Venus

Kopparla

Lee

Imamura

et al. 2019

A&A

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We explore the dominant modes of variability in the observed albedo at the cloud tops of Venus using the Akatsuki UVI 283-nm and 365-nm observations, which are sensitive to SO 2 and unknown UV absorber distributions respectively, over the period Dec 2016 to May 2018. The observations consist of images of the dayside of Venus, most often observed at intervals of 2 hours, but interspersed with longer gaps. The orbit of the spacecraft does not allow for continuous observation of the full dayside, and the unobserved regions cause significant gaps in the datasets. Each dataset is subdivided into three subsets for three observing periods, the unobserved data are interpolated and each subset is then subjected to a principal component analysis (PCA) to find six oscillating patterns in the albedo. Principal components in all three periods show similar morphologies at 283-nm but are much more variable at 365-nm. Some spatial patterns and the time scales of these modes correspond to well-known physical processes in the atmosphere of Venus such as the ∼4 day Kelvin wave, 5 day Rossby waves and the overturning circulation, while others defy a simple explanation. We also a find a hemispheric mode that is not well understood and discuss its implications.

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“…In fact, Demory et al (2013) recently provided promising results of cloud contrasts on an exoplanet. In the case of Venus, a wide variety of periodicities has been detected with observations at different wavelengths through their effects on upper cloud patterns for reflected sunlight Hosouchi et al 2012), thermal emission (Apt & Leung 1982), and also winds Kouyama et al 2013;Khatuntsev et al 2013). The wave period T is given by the expression…”

Section: Classification Of Atmospheric Periodicitiesmentioning

confidence: 99%

“…Note that, in most cases, for a single period, several combinations of horizontal intrinsic phase velocity and wavelength are possible. Low-latitude periodicities detected on the dayside cloud brightness distribution , infrared absorption lines (Hosouchi et al 2012), and on the zonal winds (Kouyama et al 2013) are displayed in the top panels of Figure 4, while periodicities identified in thermal emission at polar latitudes (Apt & Leung 1982) are shown in the lower panels.…”

Section: Classification Of Atmospheric Periodicitiesmentioning

confidence: 99%

“…The presence of global-scale waves of a different nature has also been investigated with direct observations in Venus Rossow et al 1990;Kouyama et al 2012Kouyama et al , 2013 as well as the waves predicted by different atmospheric models (Yamamoto 2001;Imamura 2006;Lebonnois et al 2010). These global-scale waves have been usually interpreted as special cases of globalscale terrestrial analogs such as Kelvin waves Smith et al 1992;Kouyama et al 2012), Rossby waves (Imamura 2006;Hosouchi et al 2012;Kouyama et al 2013), or solar tides . In the first part of this work (Peralta et al 2014), we deduced a generic dispersion relation for the acoustic and the inertia-gravity waves for a planet with a cyclostrophic atmosphere, following a procedure similar to that of Schubert & Walterscheid (1984) for Venus but additionally accounting for the centrifugal force combined with the meridional shear of the background wind.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Analytical Solution for Waves in Planets With Atmospheric Superrotation. Ii. Lamb, Surface, and Centrifugal Waves

Peralta

Imamura

Read

et al. 2014

ApJS

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This paper is the second in a two-part study devoted to developing tools for a systematic classification of the wide variety of atmospheric waves expected on slowly rotating planets with atmospheric superrotation. Starting with the primitive equations for a cyclostrophic regime, we have deduced the analytical solution for the possible waves, simultaneously including the effect of the metric terms for the centrifugal force and the meridional shear of the background wind. In those cases where the conditions for the method of the multiple scales in height are met, these wave solutions are also valid when vertical shear of the background wind is present. A total of six types of waves have been found and their properties were characterized in terms of the corresponding dispersion relations and wave structures. In this second part, we study the waves' solutions when several atmospheric approximations are applied: Lamb, surface, and centrifugal waves. Lamb and surface waves are found to be quite similar to those in a geostrophic regime. By contrast, centrifugal waves turn out to be a special case of Rossby waves that arise in atmospheres in cyclostrophic balance. Finally, we use our results to identify the nature of the waves behind atmospheric periodicities found in polar and lower latitudes of Venus's atmosphere.

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Wave signature in the Venus dayside cloud layer at 58–64 km observed by ground-based infrared spectroscopy

Cited by 9 publications

References 28 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

Principal components of short-term variability in the ultraviolet albedo of Venus

Analytical Solution for Waves in Planets With Atmospheric Superrotation. Ii. Lamb, Surface, and Centrifugal Waves

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