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Late Tharsis formation and implications for early Mars

Abstract

The Tharsis region is the largest volcanic complex on Mars and in the Solar System. Young lava flows cover its surface (from the Amazonian period, less than 3 billion years ago) but its growth started during the Noachian era (more than 3.7 billion years ago). Its position has induced a reorientation of the planet with respect to its spin axis (true polar wander, TPW), which is responsible for the present equatorial position of the volcanic province. It has been suggested that the Tharsis load on the lithosphere influenced the orientation of the Noachian/Early Hesperian (more than 3.5 billion years ago) valley networks1 and therefore that most of the topography of Tharsis was completed before fluvial incision. Here we calculate the rotational figure of Mars (that is, its equilibrium shape) and its surface topography before Tharsis formed, when the spin axis of the planet was controlled by the difference in elevation between the northern and southern hemispheres (hemispheric dichotomy). We show that the observed directions of valley networks are also consistent with topographic gradients in this configuration and thus do not require the presence of the Tharsis load. Furthermore, the distribution of the valleys along a small circle tilted with respect to the equator is found to correspond to a southern-hemisphere latitudinal band in the pre-TPW geographical frame. Preferential accumulation of ice or water in a south tropical band is predicted by climate model simulations of early Mars applied to the pre-TPW topography. A late growth of Tharsis, contemporaneous with valley incision, has several implications for the early geological history of Mars, including the existence of glacial environments near the locations of the pre-TPW poles of rotation, and a possible link between volcanic outgassing from Tharsis and the stability of liquid water at the surface of Mars.

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Figure 1: Noachian/Early Hesperian valley networks distribution and density12 before and after TPW.
Figure 2: Permanent ice deposits predicted by the global climate model for early Mars, with obliquity 45°, a circular orbit and mean surface pressure ~0.2 bar.
Figure 3: Scenario for a TPW driven by a late growth of Tharsis contemporaneous with valley network incision.

References

  1. 1

    Phillips, R. J. et al. Ancient geodynamics and global-scale hydrology on mars. Science 291, 2587–2591 (2001)

    CAS  ADS  Article  Google Scholar 

  2. 2

    Anderson, R. C. et al. Primary centers and secondary concentrations of tectonic activity through time in the western hemisphere of Mars. J. Geophys. Res. 106, 20563–20586 (2001)

    ADS  Article  Google Scholar 

  3. 3

    Grott, M. et al. Long-term evolution of the martian crust-mantle system. Space Sci. Rev. 174, 49–111 (2013)

    CAS  ADS  Article  Google Scholar 

  4. 4

    Grott, M. Late crustal growth on Mars: evidence from lithospheric extension. Geophys. Res. Lett. 32, L23201 (2005)

    ADS  Article  Google Scholar 

  5. 5

    Nahm, A. L. & Schultz, R. A. Evaluation of the orogenic belt hypothesis for the formation of the Thaumasia highlands, Mars. J. Geophys. Res. 115, E04008 (2010)

    ADS  Article  Google Scholar 

  6. 6

    Roberts, J. H. & Zhong, S. The cause for the north south orientation of the crustal dichotomy and the equatorial location of Tharsis on Mars. Icarus 190, 24–31 (2007)

    ADS  Article  Google Scholar 

  7. 7

    Melosh, H. J. Tectonic patterns on a reoriented planet: Mars. Icarus 44, 745–751 (1980)

    ADS  Article  Google Scholar 

  8. 8

    Willemann, R. J. Reorientation of planets with elastic lithospheres. Icarus 60, 701–709 (1984)

    ADS  Article  Google Scholar 

  9. 9

    Rouby, H., Greff-Lefftz, M. & Besse, J. Rotational bulge and one plume convection pattern: influence on Martian true polar wander. Earth Planet. Sci. Lett. 272, 212–220 (2008)

    CAS  ADS  Article  Google Scholar 

  10. 10

    Matsuyama, I. & Manga, M. Mars without the equilibrium rotational figure, Tharsis, and the remnant rotational figure. J. Geophys. Res. 115, E12020 (2010)

    ADS  Article  Google Scholar 

  11. 11

    Carr, M. H. The Martian drainage system and the origin of valley networks and fretted channels. J. Geophys. Res. 100, 7479–7507 (1995)

    ADS  Article  Google Scholar 

  12. 12

    Hynek, B. M., Beach, M. & Hoke, M. R. T. Updated global map of Martian valley networks and implications for climate and hydrologic processes. J. Geophys. Res. 115, E09008 (2010)

    ADS  Article  Google Scholar 

  13. 13

    Irwin, R. P., III, Craddock, R. A., Howard, A. D. & Flemming, H. L. Topographic influences on development of Martian valley networks. J. Geophys. Res. 116, E02005 (2011)

    ADS  Article  Google Scholar 

  14. 14

    Fassett, C. I. & Head, J. W. III . The timing of Martian valley network activity: constraints from buffered crater counting. Icarus 195, 61–89 (2008)

    ADS  Article  Google Scholar 

  15. 15

    Bouley, S. & Craddock, R. A. Age dates of valley network drainage basins and subbasins within Sabae and Arabia Terrae, Mars. J. Geophys. Res. 119, 1302–1310 (2014)

    Article  Google Scholar 

  16. 16

    Forget, F. et al. 3D modelling of the early Martian climate under a denser CO2 atmosphere: temperatures and CO2 ice clouds. Icarus 222, 81–99 (2013)

    CAS  ADS  Article  Google Scholar 

  17. 17

    Wordsworth, R. et al. Global modelling of the early Martian climate under a denser CO2 atmosphere: water cycle and ice evolution. Icarus 222, 1–19 (2013)

    CAS  ADS  Article  Google Scholar 

  18. 18

    Wordsworth, R. D. et al. Comparison of “warm and wet” and “cold and icy” scenarios for early Mars in a 3D climate model. J. Geophys. Res. 120, 1201–1219 (2015)

    Article  Google Scholar 

  19. 19

    Tanaka, K. & Kolb, E. Geologic history of the polar regions of Mars based on Mars Global Surveyor data. I. Noachian and Hesperian Periods. Icarus 154, 3–21 (2001)

    CAS  Google Scholar 

  20. 20

    Fishbaugh, K. & Head, J. North polar region of Mars: topography of circumpolar deposits from Mars Orbiter Laser Altimeter (MOLA) data and evidence for asymmetric retreat of the polar cap. J. Geophys. Res. 105, 22455–22486 (2000)

    ADS  Article  Google Scholar 

  21. 21

    Tanaka, K. L. et al. History of plains resurfacing in the Scandia region of Mars. Planet. Space Sci. 59, 1128–1142 (2011)

    ADS  Article  Google Scholar 

  22. 22

    Putzig, N. E. et al. SHARAD soundings and surface roughness at past, present, and proposed landing sites on Mars: reflections at Phoenix may be attributable to deep ground ice. J. Geophys. Res. 119, 1936–1949 (2014)

    Article  Google Scholar 

  23. 23

    Kress, A. M. & Head, J. W. Late Noachian and early Hesperian ridge systems in the south circumpolar Dorsa Argentea Formation, Mars: evidence for two stages of melting of an extensive late Noachian ice sheet. Planet. Space Sci. 109–110, 1–20 (2015)

    ADS  Article  Google Scholar 

  24. 24

    Feldman, W. C. et al. Global distribution of near-surface hydrogen on Mars. J. Geophys. Res. 109, E09006 (2004)

    ADS  Article  Google Scholar 

  25. 25

    Head, J. W. & Pratt, S. Extensive Hesperian-aged south polar ice sheet on Mars: evidence for massive melting and retreat, and lateral flow and ponding of meltwater. J. Geophys. Res. Planets 106, 12275–12299 (2001)

    CAS  ADS  Article  Google Scholar 

  26. 26

    Kargel, J. S. & Strom, R. G. Ancient glaciation on Mars. Geology 20, 3–7 (1992)

    ADS  Article  Google Scholar 

  27. 27

    Leonard, G. J. & Tanaka, K. L. Geologic map of the Hellas region of Mars. USGS Surv. Misc. Invest. Ser. Map I–2694 (scale 1:4,336,000) http://pubs.usgs.gov/imap/i2694/ (USGS, 2001)

  28. 28

    Costard, F. The spatial distribution of volatiles in the martian hydrolithosphere. Earth Moon Planets 45, 265–290 (1989)

    ADS  Article  Google Scholar 

  29. 29

    Weiss, D. K. & Head, J. W. Formation of double-layered ejecta craters on Mars: a glacial substrate model. Geophys. Res. Lett. 40, 3819–3824 (2013)

    ADS  Article  Google Scholar 

  30. 30

    Grimm, R. E. & Solomon, S. C. Tectonic tests of proposed polar wander paths for Mars and the Moon. Icarus 65, 110–121 (1986)

    ADS  Article  Google Scholar 

  31. 31

    Tsai, V. C. & Stevenson, D. J. Theoretical constraints on true polar wander. J. Geophys. Res. 112, B05415 (2007)

    ADS  Article  Google Scholar 

  32. 32

    Chan, N. H. et al. Time-dependent rotational stability of dynamic planets with elastic lithospheres. J. Geophys. Res. 119, 169–188 (2014)

    Article  Google Scholar 

  33. 33

    Bibring, J. P. et al. Global mineralogical and aqueous Mars history derived from OMEGA/Mars Express data. Science 312, 400–404 (2006)

    CAS  ADS  Article  Google Scholar 

  34. 34

    Kaula, W. M. An Introduction to Planetary Physics: the Terrestrial Planets (John Wiley & Sons, 1968)

  35. 35

    Wieczorek, M. A. in Treatise on Geophysics 165–206 (2007)

  36. 36

    Arfken, G. & Weber, H. Mathematical Methods for Physicists 4th edn (Academic Press, 1995)

  37. 37

    Lemoine, F. G., Konopliv, M. & Zuber, M. T. MRO Derived Gravity Science Data Products, MRO-M-RSS-5-SDP-V1.0, NASA Planetary Data System, https://pds.nasa.gov/ds-view/pds/viewProfile.jsp?dsid=MRO-M-RSS-5-SDP-V1.0 (2008)

  38. 38

    Smith, D. E. MOLA initial experiment gridded data record, MGS-M-MOLA-5-IEGDR-L3-V1.0, NASA Planetary Data System, https://pds.nasa.gov/ds-view/pds/viewDataset.jsp?dsid=MGS-M-MOLA-5-IEGDR-L3-V1.0 (1999)

  39. 39

    Sabadini, R. & Vermeersen, B. Global Dynamics of the Earth: Applications of Normal Mode Relaxation Theory to Solid-Earth Geophysics (Kluwer Academic, 2004)

  40. 40

    ESRI. Arc Hydro Tools Overview http://downloads.esri.com/blogs/hydro/ah2/arc_hydro_tools_2_0_overview.pdf (Environmental Systems Research Institute, 2004)

  41. 41

    Jenness, J. S. Some thoughts on analyzing topographic habitat characteristics. In Remotely Wild http://www.jennessent.com/downloads/topographic_analysis_online.pdf (GIS, Remote Sensing, and Telemetry Working Group of The Wildlife Society, June 2005)

  42. 42

    Laskar, J. et al. Long term evolution and chaotic diffusion of the insolation quantities of Mars. Icarus 170, 343–364 (2004)

    ADS  Article  Google Scholar 

  43. 43

    Tanaka, K. L. et al. Geologic map of Mars: U.S. Geological Survey Scientific Investigations Map 3292, scale 1:20,000,000http://dx.doi.org/10.3133/sim3292 (2014)

Download references

Acknowledgements

This research was funded by the GEOPS laboratory, the Programme National de Planétologie of INSU-CNRS and the Centre National d’Etude Spatiale (CNES).

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Authors

Contributions

S.B. conceived the project. S.B and D.B. drafted the manuscript with contributions from all authors and performed calculations of palaeo poles from valley networks distribution. I.M. performed the calculation of the rotational figure of Mars and its surface topography before TPW and Tharsis. F.F. and M.T. performed early Mars climate model simulations applied to the pre-TPW topography. A.S. and S.B. performed calculations of stream network for a topography of Mars with and without Tharsis.

Corresponding author

Correspondence to Sylvain Bouley.

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The authors declare no competing financial interests.

Extended data figures and tables

Extended Data Figure 1 Map of Tharsis region with 0 m, 3,000 m and 6,000 m isoaltitude lines.

Noachian terrains are mapped in light red for terrains lower than 3,000 m and in dark red for terrains higher than 3,000 m. Hesperian and Amazonian terrains are in grey. Age units are taken from the most recent geological map of this region43. The black cross on Tharsis Montes is the location of the centre of mass of the Tharsis dome.

Extended Data Figure 2 Modelled stream network before and after Tharsis emplacement.

a, b, Digital Elevation Model (DEM) with 1° per pixel resolution without Tharsis (a) and with Tharsis (b). The stream network was modelled using the Arc Hydro tool in ArcGIS.

Extended Data Figure 3 Rose diagram of orientations of the modelled stream network.

a, Before Tharsis emplacement (N = 702). b, After Tharsis emplacement (N = 698). The orientation values are grouped into 45° sectors. N is the total number of orientation measurements.

Extended Data Figure 4 Geological map of the north polar region.

The red cross indicates the location of the palaeo north pole (PNP), inferred from the valley network distribution. Figure modified from ref. 43; US Geological Survey.

Extended Data Figure 5 Orthographic projection of lower-limit concentrations of water abundance at latitudes poleward of 50° N.

The red cross indicates the location of the palaeo north pole, inferred from the valley network distribution. Figure modified with permission from figure 5 of Feldman, W. C. et al.24, J. Geophys. Res., John Wiley and Sons, copyright 2004 by the American Geophysical Union.

Extended Data Figure 6 Predicted global-scale stress and tectonic patterns due to the Tharsis-driven TPW event.

Solid circles indicate the locations of the palaeo poles. In the stress pattern (a), crosses indicate directions and relative magnitudes of principal stresses, and orange and blue lines correspond to extensional and compressive stresses, respectively. In the tectonic pattern (b), the orange, blue, and light grey lines indicate the strike of the expected normal, thrust and strike–slip faults, respectively. Contours correspond to the deviator stress in units of MPa. Solid black lines mark the boundaries between different tectonic regions.

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Bouley, S., Baratoux, D., Matsuyama, I. et al. Late Tharsis formation and implications for early Mars. Nature 531, 344–347 (2016). https://doi.org/10.1038/nature17171

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