Models of the structure of the atmosphere of Venus from the surface to 100 kilometers altitude

Seiff, A.; Schofield, J. T.; Kliore, A. J.; Taylor, F. W.; Limaye, S. S.; Revercomb, H. E.; Sromovsky, Lawrence A.; Kerzhanovich, V. V.; Moroz, V.I.; Marov, M. Ya.

doi:10.1016/0273-1177(85)90197-8

Cited by 402 publications

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“…The measured latitudinal thermal structure shows that the pole-equator temperature differences at altitudes up to 65 km are relatively small, ∼ 10 K (Kliore 1985, Seiff et al 1985. Longitudinal differences from surface to the cloud tops (∼ 70 km) are < 5 K in low latitudes (Seiff et al 1980;Kliore 1985) and can be ∼ 20 K in higher latitudes (> 60°).…”

Section: Introductionmentioning

confidence: 91%

“…The results of thermal structure investigations available until early 1980s were reviewed by Seiff (1983) and used in the Venus International Reference Model (VIRA) described by Seiff et al (1985). Radio occultations from Magellan (Jenkins et al 1994) and Venera 15 and 16 orbiters (Yakovlev et al 1987) and retrievals from the Fourier Spectrometer infrared observations from Venera 15 have been incorporated by in an interim update of the VIRA model (Seiff et al 1985).…”

Section: Introductionmentioning

confidence: 99%

“…Radio occultations from Magellan (Jenkins et al 1994) and Venera 15 and 16 orbiters (Yakovlev et al 1987) and retrievals from the Fourier Spectrometer infrared observations from Venera 15 have been incorporated by in an interim update of the VIRA model (Seiff et al 1985). These and ground based results were summarized by Lellouch et al (1997).…”

Section: Introductionmentioning

confidence: 99%

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Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet's extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in [1411][1412][1413][1414] 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595-4622, 1996) from 1 μm observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.

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Section: Introductionmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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“…Overall, DYASTIMA is an easy to use application providing several pieces of output information that can be fitted to a variety of external applications. The most indicative input parameters that should be managed, combined and transformed in order to be inserted in the application, are the structure of the atmosphere (density, mixing ratios of different components), the magnetic field, the spectra of the incoming particles, the physical interactions that are considered, the energy channels that are predefined in order to accelerate the simulation, and the altitudes in which the in- Kliore et al (1985); Seiff et al (1985); Keating et al (1985) formation about the cascade will be registered. The physics list used in DYASTIMA contains all standard electromagnetic processes (see Table 1).…”

Section: Introductionmentioning

confidence: 99%

“…The atmospheric description is based on the Venus International Reference Atmosphere and on the estimations by Seiff et al (1985) for the middle and lower atmosphere (100-0 km) at low latitudes (u< 30 • ) and on those by Keating et al (1985) for the daytime upper atmosphere between 100-150 km at low latitude (u = 16 • ). We note that the considered atmospheric composition and densities are the same as in .…”

Section: Introductionmentioning

confidence: 99%

Solar energetic particle interactions with the Venusian atmosphere

et al. 2016

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Abstract. In the context of planetary space weather, we estimate the ion production rates in the Venusian atmosphere due to the interactions of solar energetic particles (SEPs) with gas. The assumed concept for our estimations is based on two cases of SEP events, previously observed in near-Earth space: the event in October 1989 and the event in May 2012. For both cases, we assume that the directional properties of the flux and the interplanetary magnetic field configuration would have allowed the SEPs' arrival at Venus and their penetration to the planet's atmosphere. For the event in May 2012, we consider the solar particle properties (integrated flux and rigidity spectrum) obtained by the Neutron Monitor Based Anisotropic GLE Pure Power Law (NMBANGLE PPOLA) model (Plainaki et al., 2010) applied previously for the Earth case and scaled to the distance of Venus from the Sun. For the simulation of the actual cascade in the Venusian atmosphere initiated by the incoming particle fluxes, we apply the DYASTIMA code, a Monte Carlo (MC) application based on the Geant4 software (Paschalis et al., 2014). Our predictions are afterwards compared to other estimations derived from previous studies and discussed. Finally, we discuss the differences between the nominal ionization profile due to galactic cosmic-ray-atmosphere interactions and the profile during periods of intense solar activity, and we show the importance of understanding space weather conditions on Venus in the context of future mission preparation and data interpretation.

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Venus's major cloud feature as an equatorially trapped wave distorted by the wind

Peralta

Sánchez‐Lavega

López‐Valverde

et al. 2015

Geophysical Research Letters

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The superrotation of the atmospheres of slowly rotating bodies is a long‐standing problem yet unsolved in atmospheric dynamics. On Venus, the most extreme case known of superrotation, this is accompanied and influenced by a recurrent planetary‐scale cloud structure, known as the Y feature. So far, no model has simultaneously reproduced its shape, temporal evolution, related wind field, nor the relation between its dynamics and the unknown UV‐absorbing aerosol that produces its dark morphology. In this paper we present an analytical model for a Kelvin‐like wave that offers an explanation of these peculiarities. Under Venus cyclostrophic conditions, this wave is equatorially and vertically trapped where zonal winds peak and extends 7 km in altitude, and its vertical wind perturbations are shown to produce upwelling of the UV absorber. The Y‐feature morphology and its 30 day evolution are reproduced as distortions of the wave structure by the Venus winds.

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Models of the structure of the atmosphere of Venus from the surface to 100 kilometers altitude

Cited by 402 publications

References 0 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

Solar energetic particle interactions with the Venusian atmosphere

Venus's major cloud feature as an equatorially trapped wave distorted by the wind

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