Spectral evidence for hydrated salts in recurring slope lineae on Mars

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Determining whether liquid water exists on the Martian surface is central to understanding the hydrologic cycle and potential for extant life on Mars. Recurring slope lineae, narrow streaks of low reflectance compared to the surrounding terrain, appear and grow incrementally in the downslope direction during warm seasons when temperatures reach about 250–300 K, a pattern consistent with the transient flow of a volatile species1,2,3. Brine flows (or seeps) have been proposed to explain the formation of recurring slope lineae1,2,3, yet no direct evidence for either liquid water or hydrated salts has been found4. Here we analyse spectral data from the Compact Reconnaissance Imaging Spectrometer for Mars instrument onboard the Mars Reconnaissance Orbiter from four different locations where recurring slope lineae are present. We find evidence for hydrated salts at all four locations in the seasons when recurring slope lineae are most extensive, which suggests that the source of hydration is recurring slope lineae activity. The hydrated salts most consistent with the spectral absorption features we detect are magnesium perchlorate, magnesium chlorate and sodium perchlorate. Our findings strongly support the hypothesis that recurring slope lineae form as a result of contemporary water activity on Mars.

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Change history

  • Corrected online 14 October 2015

    In the version of this Letter originally published, the journal name in ref. 12 was incorrect, it should have been Nature Geoscience. This has been corrected in all versions of the Letter.


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L.O. and M.B.W. are funded by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1148903. The research was further supported by MDAP Grant No. NNX13AK01G. All original data described in this paper are reported in the SOM and archived by NASA’s Planetary Data System. We thank the MRO science and engineering team for returning such an incredible data set. The paper benefited from initial reviews by B. Schmidt and L. Liuzzo.

Author information


  1. School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia 30308, USA

    • Lujendra Ojha
    • , Mary Beth Wilhelm
    •  & James J. Wray
  2. Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, California 94035, USA

    • Mary Beth Wilhelm
  3. Applied Physics Laboratory, Laurel, Maryland 20723, USA

    • Scott L. Murchie
  4. Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721, USA

    • Alfred S. McEwen
    •  & Matt Chojnacki
  5. Department of Space Studies, Southwest Research Institute, Boulder, Colorado 80302, USA

    • Jennifer Hanley
  6. Laboratoire de Planétologie et Géodynamique, Nantes 44322, France

    • Marion Massé


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The methodology was conceived and designed by L.O. All data analysis was done by L.O. with significant feedback from S.L.M., J.J.W., A.S.M. and M.B.W. J.J.W., M.B.W., J.H. and M.M. provided all the laboratory spectra used in this paper. A.S.M., M.C. and S.L.M. planned many of the HiRISE–CRISM coordinated observations of the RSL sites. All authors contributed to discussion, interpretation and writing.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to Lujendra Ojha.

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