近日，美国得克萨斯大学奥斯汀分校Chenguang Sun团队报道了火山释放出的硫化物形成了早期火星的气候。2025年9月5日出版的《科学进展》杂志发表了这项成果。
硫和其他挥发物可以通过岩浆过程从火星内部运输到地表，包括地幔熔化、岩浆分化和脱气。然而，由于具有多组分挥发物的化学和动态演化的岩浆系统中气体-熔体相互作用的复杂性，这些过程在过去的硫循环模型中并没有完全集成。
研究组结合这些过程来模拟硫、碳和氢从火星上融化的过程。结果发现，还原的硫化物，H2S和S2，主要是通过在沸点到地表压力下脱气释放的。这些硫化物可以凝结成硫化物和单质硫，可能通过二次氧化产生在火星表面观察到的硫酸盐沉积物。该模型还表明，演化的岩浆在火山口压力下达到石墨和硫化物的饱和，它们可能在火星火山口中建立硫和碳储集层。脱气的H2S和S2可能与SF6（一种强效的温室气体）形成一层朦胧的大气，从而塑造火星的古气候。
附：英文原文
Title: Volcanic emission of reduced sulfur species shaped the climate of early Mars
Author: Lucia G. Bellino, Chenguang Sun
Issue&Volume: 2025-09-05
Abstract: Sulfur and other volatiles could be transported from the martian interior to surface through magmatic processes, including mantle melting, magma differentiation, and degassing. However, these processes were not fully integrated in past sulfur cycling models because of complexity from the gas-melt interactions in chemically and dynamically evolving magmatic systems with multicomponent volatiles. Here, we incorporate these processes to simulate how sulfur, carbon, and hydrogen degas from martian melts. We find that reduced sulfur species, H2S and S2, are dominantly emitted through degassing at crustal to surficial pressures. These sulfur species could condense as sulfide and elemental sulfur, potentially yielding the sulfate deposits observed on the martian surface through secondary oxidation. Our models also show that evolved magmas reach graphite and sulfide saturation at crustal pressures and thus may establish sulfur and carbon reservoirs in the martian crust. The degassed H2S and S2 may form a hazy atmosphere with SF6, a potent greenhouse gas, to shape the paleoclimate of Mars.
DOI: adr9635
Source: https://www.science.org/doi/10.1126/sciadv.adr9635