Acidic weathering of basalt and basaltic glass: 1. Near‐infrared spectra, thermal infrared spectra, and implications for Mars. Issue 1 (24th January 2017)

• Record Type: Journal Article
• Authors: Horgan, Briony H. N.; Smith, Rebecca J.; Cloutis, Edward A.; Mann, Paul; Christensen, Philip R.
• Is Part Of: Journal of geophysical research. Volume 122:Issue 1(2017:Jan.)
• Page Start: 172
• Page End: 202
• Publication Date: 2017-01-24
• Subjects: spectroscopy -- Mars -- weathering -- acid -- alteration; Planets -- Periodicals; Geophysics -- Periodicals; 559.9
• DOI: 10.1002/2016JE005111
• Languages: English
• ISSNs: 2169-9097

Abstract

Abstract: Acid‐leached rinds and coatings occur in volcanic environments on Earth and have been identified using orbital spectroscopy on Mars, but their development is poorly understood. We simulated long‐term open‐system acidic weathering in a laboratory by repeatedly rinsing and submerging crystalline and glassy basalts in pH ~ 1 and pH ~ 3 acidic solutions for 213 days and compared their visible/near‐infrared (0.3–2.5 µm) and thermal infrared (5–50 µm) spectral characteristics to their microscopic physical and chemical properties from scanning electron microscopy (SEM). We find that while alteration at moderately low pH (~3) can produce mineral precipitates from solution, it has very little spectral or physical effect on the underlying parent material. In contrast, alteration at very low pH (~1) results in clear silica spectral signatures for all crystalline samples while glasses exhibit strong blue concave‐up near‐infrared slopes. SEM indicates that these spectral differences correspond to different modes of alteration. In glass, alteration occurs only at the surface and produces a silica‐enriched leached rind, while in more crystalline samples, alteration penetrates the interior to cause dissolution and replacement by silica. We confirm that glass is more stable than crystalline basalt under long‐term acidic leaching, suggesting that glass could be enriched and common in terrains on Mars that have been exposed to acidic weathering. Leached glasses are consistent with both OMEGA and Thermal Emission Spectrometer (TES) spectra of the Martian northern lowlands and may contribute to the high‐silica phases detected globally in TES Surface Type 2. Thus, both glass‐rich deposits and acidic weathering may have been widespread on Mars. Key Points: Acid alteration at moderate pH produces mineral precipitates but has little to no physical or spectral effect on the underlying basalt Acid alteration at low pH causes significant leaching, but altered basalt and glass exhibit different near‐infrared and thermal infrared spectra The spectral difference is due to different weathering mechanisms and may allow us to uniquely detect leached glasses on Mars