Dataset Information

Thermal structure of the Venusian atmosphere from the sub-cloud region to the mesosphere as observed by radio occultation.

ABSTRACT: We present distributions of the zonal-mean temperature and static stability in the Venusian atmosphere obtained from Venus Express and Akatsuki radio occultation profiles penetrating down to an altitude of 40?km. At latitudes equatorward of 75°, static stability derived from the observed temperature profiles is consistent with previous in-situ measurements in that there is a low-stability layer at altitudes of 50-58?km and highly and moderately stratified layers above 58?km and below 50?km, respectively. Meanwhile, at latitudes poleward of 75°, a low-stability layer extends down to 42?km, which has been unreported in analyses of previous measurements. The deep low-stability layer in the polar region cannot be explained by vertical convection in the middle/lower cloud layer, and the present result thus introduces new constraints on the dynamics of the sub-cloud atmosphere. The Venusian atmosphere is in striking contrast to the Earth's troposphere, which generally has a deeper low-stability layer at low latitudes than at mid- and high latitudes.

SUBMITTER: Ando H

PROVIDER: S-EPMC7044293 | biostudies-literature | 2020 Feb

REPOSITORIES: biostudies-literature

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Thermal structure of the Venusian atmosphere from the sub-cloud region to the mesosphere as observed by radio occultation.

Ando Hiroki H Imamura Takeshi T Tellmann Silvia S Pätzold Martin M Häusler Bernd B Sugimoto Norihiko N Takagi Masahiro M Sagawa Hideo H Limaye Sanjay S Matsuda Yoshihisa Y Choudhary Raj Kumar RK Antonita Maria M

Scientific reports 20200226 1

We present distributions of the zonal-mean temperature and static stability in the Venusian atmosphere obtained from Venus Express and Akatsuki radio occultation profiles penetrating down to an altitude of 40 km. At latitudes equatorward of 75°, static stability derived from the observed temperature profiles is consistent with previous in-situ measurements in that there is a low-stability layer at altitudes of 50-58 km and highly and moderately stratified layers above 58 km and below 50 km, resp ...[more]

PMID: 32103048

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Project description:There is currently a gap in satellite observations of the moisture structure during heavy precipitation conditions, since infrared and microwave sounders cannot sense water-vapour structure near the surface in the presence of intense precipitation. Conversely, Global Navigation Satellite System (GNSS) radio occultations (RO) can profile the moisture structure with high precision and vertical resolution, but cannot indicate the presence of precipitation directly. Polarimetric RO (PRO) measurements have been proposed as a method to characterize heavy rain in GNSS RO, by measuring the polarimetric differential phase delay induced by large size hydrometeors. Previous studies have shown that the PRO polarimetric phase shift is sensitive to the path-integrated rain rate under intense precipitation scenarios, but there is no current method to invert PRO measurements into quantitative estimates of the path-averaged rain rate. In this manuscript, a probabilistic inversion approach to the GNSS PRO observables is proposed, where the GPM precipitation products are used for the construction of an a priori look-up table (LUT) database. The performance of the LUTs is assessed for use in the inversion of satellite-based GNSS PRO observations, based on synthetically generated PRO data of actual events, which correspond to co-locations between GNSS RO profiles and the TRMM observations. The synthetic data include end-to-end propagation effects of the polarimetric observables and a simple separation algorithm to isolate the hydrometeor component of the observation. The assessment results in agreement better than ±1 mm/hr between the reference LUT and the actual rain statistics of the synthetic data, proving the suitability of the GPM-based probabilistic inversion tool. These findings indicate that the GNSS PRO products are capable of extending the current GNSS RO ones by associating indications of rain-rate probabilities at different altitudes, at ?250 m vertical resolution and under intense precipitation scenarios with the standard vertical thermodynamic profiles.

Project description:Abstract A new model was recently introduced to correct for higher?order ionospheric residual biases in radio occultation (RO) data. The model depends on the ?1 and ?2 dual?frequency bending angle difference squared, and a factor ?, which varies with time, season, solar activity, and height, needing only the F10.7 solar radio flux index as additional background information. To date, this kappa?correction was analyzed in simulation studies. In this study, we test it on real observed Metop?A RO data. The goal is to improve the accuracy of monthly mean RO climate records, potentially raising the accuracy of RO data toward higher stratospheric altitudes. We performed a thorough analysis of the kappa?correction, evaluating its ionospheric sensitivity during the solar cycle for monthly RO climatologies and comparing the kappa?corrected RO stratospheric climatologies to three other data sets from reanalysis and passive infrared sounding. We find a clear dependence of the kappa?correction on solar activity, geographic location, and altitude; hence, it reduces systematic errors that vary with the solar cycle. From low to high solar activity conditions, the correction can increase from values of about 0.2 K to more than 2.0 K at altitudes between 40 to 45 km. The correction shifts RO climatologies toward warmer temperatures. With respect to other data sets, however, we found it difficult to draw firm conclusions, because the biases in the other data sets appear to be at similar magnitude as the size of the kappa?correction. Further validation with more accurate data will be useful. Key Points The kappa?correction model is tested for the impact of its correction of higher?order ionospheric biases in radio occultation data The magnitude of the kappa?correction varies over the solar cycle from 0.2 K to more than 2.0 K at about 40 km The correction shifts the stratospheric data toward warmer temperatures; firm validation based on other data sets was difficult

Dataset Information

Thermal structure of the Venusian atmosphere from the sub-cloud region to the mesosphere as observed by radio occultation.

Publications

Thermal structure of the Venusian atmosphere from the sub-cloud region to the mesosphere as observed by radio occultation.

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