Scattered UV solar radiation within the clouds of Venus

Ekonomov, A. P.; Мороз, В. І.; Moshkin, B. E.; Gnedykh, V. I.; Golovin, Yu. M.; Crigoryev, A. V.

doi:10.1038/307345a0

Cited by 23 publications

(18 citation statements)

References 12 publications

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“…Measurements of scattered solar radiation below the clouds Ekonomov et al 1984) indicate that the atmosphere at these levels is only slightly heated by absorption of sunlight in the weak near-IR CO 2 and H 2 O bands and by additional UV absorption. Thermal infrared fluxes and cooling rates in the lower atmosphere are very poorly constrained by the observations and the models.…”

Section: Global Radiative Energy Balancementioning

confidence: 99%

“…The solar flux radiometer (LSFR) aboard the Pioneer Venus Large Probe measured solar fluxes during descent in a series of channels covering a broad range from 0.4 through 1.8 μm (Tomasko et al 1980a). The Venera-13 and 14 descent probes also carried a photometric experiment to measure the distribution of UV radiation (Ekonomov et al 1984). The measurements of the vertical profiles of downward solar fluxes by the Venera and Pioneer-Venus descent probes showed that UV and blue radiation are strongly absorbed in the upper cloud layer above 57 km.…”

Section: Radiation Field Inside the Atmospherementioning

confidence: 99%

“…The solar radiation field inside the atmosphere was measured by spectrophotometers on several Venera descent probes (Ekonomov et al 1984;). These observations provided a unique data set for characterizing the angular and spectral distribution of solar scattered light between 0.4 and 1.2 μm from ∼ 65 km down to the surface.…”

Section: Radiation Field Inside the Atmospherementioning

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: Global Radiative Energy Balancementioning

confidence: 99%

Section: Radiation Field Inside the Atmospherementioning

confidence: 99%

Section: Radiation Field Inside the Atmospherementioning

confidence: 99%

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Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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“…Fecl 3 in aerosol particles was observed by X-ray fluorescent spectroscopy from the VEnErA 14 and VEGA landers [Petryanov et al, 1981;Krasnopolsky, 1989]. The transition from Fecl 3 to colorless ferric sulfate predicted to occur at 58 km is close to the lower boundary of absorption observed by Ekonomov et al [1983Ekonomov et al [ , 1984 on VEnErA 14. SCl 2 .…”

Section: Unidentified Uv and Blue Absorptionmentioning

confidence: 99%

Atmospheric composition, chemistry, and clouds

Mills¹,

Esposito²,

Yung³

2007

Geophysical Monograph Series

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“…The mixing ratios of these absorbers are considered to increase precipitously with decreasing the altitude below the cloud top (Pollack et al, 1980). Identification of the absorber is important not only for atmospheric chemistry but also for the radiative energy budget, since the absorption makes a nonnegligible contribution to the heating profile in the cloud layer (Ekonomov et al, 1984).…”

Section: Clouds and Lightningmentioning

confidence: 99%

Overview of Venus orbiter, Akatsuki

et al. 2011

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The Akatsuki spacecraft of Japan was launched on May 21, 2010. The spacecraft planned to enter a Venusencircling near-equatorial orbit in December 7, 2010; however, the Venus orbit insertion maneuver has failed, and at present the spacecraft is orbiting the Sun. There is a possibility of conducting an orbit insertion maneuver again several years later. The main goal of the mission is to understand the Venusian atmospheric dynamics and cloud physics, with the explorations of the ground surface and the interplanetary dust also being the themes. The angular motion of the spacecraft is roughly synchronized with the zonal flow near the cloud base for roughly 20 hours centered at the apoapsis. Seen from this portion of the orbit, cloud features below the spacecraft continue to be observed over 20 hours, and thus the precise determination of atmospheric motions is possible. The onboard science instruments sense multiple height levels of the atmosphere to model the three-dimensional structure and dynamics. The lower clouds, the lower atmosphere and the surface are imaged by utilizing nearinfrared windows. The cloud top structure is mapped by using scattered ultraviolet radiation and thermal infrared radiation. Lightning discharge is searched for by high speed sampling of lightning flashes. Night airglow is observed at visible wavelengths. Radio occultation complements the imaging observations principally by determining the vertical temperature structure.

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Scattered UV solar radiation within the clouds of Venus

Cited by 23 publications

References 12 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

Atmospheric composition, chemistry, and clouds

Overview of Venus orbiter, Akatsuki

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