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- W129252052 abstract "The powerful greenhouse effect on Venus exists because pressure-broadened CO2 absorption bands, interlaced with water absorption features, effectively block most of the upwelling thermal radiation coming from the surface. The sulfuric acid clouds and small amounts of SO2, OCS, CO, HCl and HF are responsible for some absorption of radiation at wavelengths greater than 2 m. In particular, these constituents of Venus' atmosphere absorb thermal radiation in a crucial part of the spectrum -the 2.1 to 2.6 m range where the CO2-H2O thermal absorption conspiracy is weak. Much of the radiation on the short-wavelength side of Venus' surface blackbody curve (which has a peak at 4 m), leaves the planet through this window. Variations in the abundance of the trace atmospheric species have a large effect on the efficacy of this window, both directly through their infrared absorption, and indirectly through their effect on clouds. Increased atmospheric absorption, say through an increase in atmospheric water abundance, can heat the surface. However, as the surface of Venus heats up, the peak of its Planck function moves towards the 2.1 to 2.6 m window, allowing more direct thermal radiation loss to space. This high temperature shift of radiative loss into the window will act as a thermostat. For moderate perturbations in atmospheric trace species therefore, such as those expected from volcanism or large impacts, there is a limit to how hot the surface of Venus can get." @default.
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- W129252052 modified "2023-09-27" @default.
- W129252052 title "How Hot Can Venus Get" @default.
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