Stabilization of Venus’ climate by a chemical-albedo feedback

Hashimoto, George L.; Abe, Yutaka

doi:10.1186/bf03351628

Cited by 15 publications

(9 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The high surface temperature of Venus enhances the importance of the gas‐solid reactions on the planetary surface in controlling the atmospheric composition, including infrared‐active species which control the greenhouse effect. Venus climate models that combine chemical reaction and radiative transfer in the atmosphere have demonstrated that such a coupling between surface chemical reactions and greenhouse effect will play an important role in controlling the surface environment [e.g., Hashimoto and Abe , 2000; Bullock and Grinspoon , 2001].…”

Section: Introductionmentioning

confidence: 99%

Felsic highland crust on Venus suggested by Galileo Near‐Infrared Mapping Spectrometer data

Hashimoto¹,

Roos-Serote²,

Sugita³

et al. 2008

J. Geophys. Res.

107

View full text Add to dashboard Cite

[1] We evaluated the spatial variation of Venusian surface emissivity at 1.18 mm wavelength and that of near-surface atmospheric temperature using multispectral images obtained by the Near-Infrared Mapping Spectrometer (NIMS) on board the Galileo spacecraft. The Galileo NIMS observed the nightside thermal emission from the surface and the deep atmosphere of Venus, which is attenuated by scattering from the overlying clouds. To analyze the NIMS data, we used a radiative transfer model based on the adding method. Although there is still an uncertainty in the results owing to the not well known parameters of the atmosphere, our analysis revealed that the horizontal temperature variation in the near-surface atmosphere is no more than ±2 K on the Venusian nightside and also suggests that the majority of lowlands likely has higher emissivity compared to the majority of highlands. One interpretation for the latter result is that highland materials are generally composed of felsic rocks. Since formation of a large body of granitic magmas requires water, the presence of granitic terrains would imply that Venus may have had an ocean and a mechanism to recycle water into the mantle in the past.

show abstract

Section: Introductionmentioning

confidence: 99%

Felsic highland crust on Venus suggested by Galileo Near‐Infrared Mapping Spectrometer data

Hashimoto¹,

Roos-Serote²,

Sugita³

et al. 2008

J. Geophys. Res.

107

View full text Add to dashboard Cite

show abstract

“…The climate and surface environment are also controlled by volcanism in that the associated degassing affects the atmospheric composition producing climate variations Grinspoon 1998, Hashimoto andAbe 2000). The dominant climate change is caused by changes in the H 2 SO 4 cloud cover above 48 km altitude, being induced by the increase in atmospheric sulfur produced by Venusian volcanos.…”

Section: Introductionmentioning

confidence: 98%

Elucidating the Rate of Volcanism on Venus: Detection of Lava Eruptions Using Near-Infrared Observations

Hashimoto

Imamura

2001

Icarus

View full text Add to dashboard Cite

“…It has also been pro-posed that the atmospheric SO 2 mixing ratio is in equilibrium with a pyrite-magnetite assemblage. This chemical coupling would stabilize the climate through a cloud-albedo feedback (Hashimoto and Abe, 2000). Anomalous radar reflectivity areas observed at Venusian highlands might be attributed to pyrite produced by the atmosphere-surface interaction above, although heavy metal frost may also explain the reflectivity (Schaefer and Fegley, 2004).…”

Section: Surface Processesmentioning

confidence: 99%

“…Its climate and surface environment are also controlled by volcanism in that the associated degassing affects the atmospheric composition producing climate variations (Hashimoto and Abe, 2000). The current rate of volcanism, which is a key parameter determining the present chemical state of the atmosphere, is uncertain (Basilevsky et al, 1997).…”

Section: Surface Processesmentioning

confidence: 99%

Overview of Venus orbiter, Akatsuki

et al. 2011

Self Cite

View full text Add to dashboard Cite

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.

show abstract

Stabilization of Venus’ climate by a chemical-albedo feedback

Cited by 15 publications

References 24 publications

Felsic highland crust on Venus suggested by Galileo Near‐Infrared Mapping Spectrometer data

Felsic highland crust on Venus suggested by Galileo Near‐Infrared Mapping Spectrometer data

Elucidating the Rate of Volcanism on Venus: Detection of Lava Eruptions Using Near-Infrared Observations

Overview of Venus orbiter, Akatsuki

Contact Info

Product

Resources

About