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<p>Understanding the interaction of Martian rocks and the environment is conducive to Mars <i>in situ</i> resource utilization (ISRU) and the search for natural H<sub>2</sub> reservoirs. Here, we report an interesting finding: using a real Martian meteorite (NWA13190) and within Mars’ temperature range (25°C), we confirmed spontaneous hydrogen generation from the reaction of water, CO<sub>2</sub>, and Martian rock—no external energy or catalysts required. The reaction produced hydrogen at ∼4 ppm/day, stabilizing after 9 days, alongside newly formed carbonate and sulfate minerals absent in the original meteorite. Mechanistic analyses using XPS (X-ray photoelectron spectroscopy), Mössbauer spectroscopy, and FTIR (Fourier transform infrared spectroscopy) revealed that Fe<sup>2+</sup> in FeTiO<sub>3</sub> and FeS<sub>2</sub> (not pyroxene) oxidized to Fe<sup>3+</sup>, driving water reduction to hydrogen. The buffer effect of CO<sub>2</sub> sustained acidic conditions, enhancing Fe<sup>2+</sup> release and H<sub>2</sub> production. These results align with <i>in situ</i> Mars detections (e.g., Ca-sulfate veins by Curiosity). Compared with energy-intensive electrolysis-based ISRU, this geological process offers a more efficient H<sub>2</sub> production pathway. It also provides theoretical support for natural hydrogen reservoirs on Mars and simultaneously advances understanding of Mars’ early atmospheric evolution and potential life-supporting environments.</p>

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Hydrogen generation from the spontaneous reaction of water, CO2, and Martian meteorites

  • 期刊论文

  • 发表日期：

    2026年2月10日

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  • Xuhai Tang,
  • Yiheng Zhang,
  • Jiangmei Qiao,
  • Yuyan Sara Zhao,
  • Lizhi Huang,
  • Yiwei Liu

摘要

Understanding the interaction of Martian rocks and the environment is conducive to Mars in situ resource utilization (ISRU) and the search for natural H2 reservoirs. Here, we report an interesting finding: using a real Martian meteorite (NWA13190) and within Mars’ temperature range (25°C), we confirmed spontaneous hydrogen generation from the reaction of water, CO2, and Martian rock—no external energy or catalysts required. The reaction produced hydrogen at ∼4 ppm/day, stabilizing after 9 days, alongside newly formed carbonate and sulfate minerals absent in the original meteorite. Mechanistic analyses using XPS (X-ray photoelectron spectroscopy), Mössbauer spectroscopy, and FTIR (Fourier transform infrared spectroscopy) revealed that Fe2+ in FeTiO3 and FeS2 (not pyroxene) oxidized to Fe3+, driving water reduction to hydrogen. The buffer effect of CO2 sustained acidic conditions, enhancing Fe2+ release and H2 production. These results align with in situ Mars detections (e.g., Ca-sulfate veins by Curiosity). Compared with energy-intensive electrolysis-based ISRU, this geological process offers a more efficient H2 production pathway. It also provides theoretical support for natural hydrogen reservoirs on Mars and simultaneously advances understanding of Mars’ early atmospheric evolution and potential life-supporting environments.