Radiative fluxes in the atmosphere of Venus

金星的主要云层从大约50 - 70公里的高度延伸，主要由硫酸和水混合而成。这些云对大气中的太阳辐射通量和热辐射通量都有巨大的影响，在温室变暖和强迫大气环流方面发挥着重要作用;因此，测量和了解这些通量对于了解大气动力学至关重要。大气层内的辐射通量已经由先锋金星、金星和织女星下降探测器测量，并将由未来的下降探测器和金星大气层中的气球测量，例如美国宇航局金星旗舰使命研究中提出的探测器。这项工作的主题将是使用牛津大学的现代辐射传输代码NEMESIS，结合金星快车等飞行任务的云约束，重新分析先锋金星和金星/Vega下降剖面，以检索云丰度和水蒸气剖面作为高度的函数。这将提高我们对金星大气层的理解，并为未来的任务提供重要的新约束和背景。特别是，将进行计算，以优化未来探测器或球载辐射计的潜在可见光/红外光谱通道的位置和宽度，并根据研究优先事项和项目进展中的使命机会，对与表面成像和/或太阳能发电有关的近地表辐射通量进行模拟。

The main cloud deck of Venus extends from about 50 - 70 km altitude and is composed primarily of sulphuric acid mixed with water. These clouds have a huge effect on both solar and thermal radiative fluxes in the atmosphere, playing a major part in greenhouse warming and in forcing the atmospheric circulation; hence, measuring and understanding these fluxes is critical for understanding the dynamics of the atmosphere. Radiative fluxes within the atmosphere have been measured by the Pioneer Venus, Venera, and VeGa descent probes, and will be measured from future descent probes and balloons in the atmosphere of Venus, such as the ones proposed in the NASA Venus Flagship Mission Study. The theme of this work will be to use Oxford's modern radiative transfer code, NEMESIS, combined with cloud constraints from missions such as Venus Express, to reanalyse Pioneer Venus and Venera/VeGa descent profiles to retrieve cloud abundances and water vapour profiles as a function of altitude. This will improve our understanding of Venus' atmosphere and also provide important new constraints and context for future missions. In particular, calculations will be made to optimise the position and widths of potential visible/infrared spectral channels for future probe- or balloon-borne radiometers and also simulations made of the near-surface radiative fluxes, relevant to surface imaging and/or solar power generation depending on research priorities and mission opportunities as the project progresses.