With recent progress of observational astronomy, the next generation of space telescopes (JWST, ARIEL, OST, HabEx, LUVOIR) will be able to determine the composition of exoplanetary atmospheres in the next decades. The discovery of rocky exoplanets, as potentially favorable harbors for life, finds a particularly strong echo in the scientific community and in the general audience. The interaction of the surface of a planetary body with its atmosphere is key to understanding the composition of the latter and hence to determine whether the planet may host life or not. In an effort to describe surface–atmosphere interactions on rocky planets and the heterogeneous reactions occurring on solid surfaces, in particular mineral dust grains, in such systems it is necessary to develop a systematic approach to this family of reactions. Such an approach is proposed in this Perspective on three very distinct examples of rocky planets: Earth, Mars, and Venus. These bodies have experienced very different evolutions, although they likely started from similar initial conditions; the pressure and temperature of their atmospheres cover a broad range of values, offering an invaluable set of planet-size laboratories to study the impact of physical and chemical parameters on the evolution of atmospheres. Systems that should be investigated in priority with relevance for Earth, Mars, and Venus are discussed. It is shown that a better knowledge of mineral dust supporting heterogeneous reactivity is crucial and that the impact of environmental parameters on these reactions needs to be carefully investigated. Current and future missions to Mars and Venus will require such work to better model and understand the observations. In particular, a strong effort is needed to study Venus, which has only few dedicated laboratory setups although it will be the target of exploration missions in the next decades. These studies will pave the way to build robust models of exoplanetary atmospheres, which will be crucial to account for the observations of their composition by space telescopes in the near future.

中文翻译：

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地球，火星和金星大气中的异质物理化学：岩石系外行星的前景

随着观测天文学的最新进展，下一代太空望远镜（JWST，ARIEL，OST，HabEx，LUVOIR）将能够确定未来几十年的系外行星大气的组成。岩石系外行星的发现，可能是生命的潜在庇护所，在科学界和普通大众中发现了特别强烈的回声。行星表面与大气的相互作用是理解行星的组成并因此确定行星是否可以生存的关键。为了描述岩石行星上的表面-大气相互作用以及在固体表面上发生的非均相反应，特别是矿物尘埃颗粒，在此类系统中，有必要为这种反应家族开发一种系统的方法。本文在“透视”中针对岩石行星的三个非常不同的示例提出了这种方法：地球，火星和金星。尽管它们可能是从相似的初始条件开始的，但它们经历了截然不同的演变。它们大气层的压力和温度涵盖了广泛的数值范围，提供了一组宝贵的行星级实验室，用于研究物理和化学参数对大气层演变的影响。讨论了应优先研究与地球，火星和金星有关的系统。结果表明，对支持异质反应性的矿物粉尘的更好了解至关重要，并且需要仔细研究环境参数对这些反应的影响。当前和将来前往火星和金星的任务将需要进行此类工作，以更好地建模和理解观测结果。特别是，研究金星需要付出很大的努力，尽管只有未来几十年的探索任务，金星只有很少的专用实验室设置。这些研究将为建立稳固的系外行星模型铺平道路，这对于在不久的将来用太空望远镜解释其组成至关重要。