Fluvial Systems (2018, updated Valley Networks)

External link.

“This dataset represents an update of previous global maps of Martian fluvial systems. We included all the valleys longer than 20 km.”

Each polyline is classified into these categories: Long valley, Single valley, Valley network. The db also contains age.

This db is based on the Hynek et al (2010) database and contains additions, removals and course corrections.

This dataset is hosted at this location:


If you use this data set in your own work, please cite this DOI: 10.5281/zenodo.1051038

Please also cite these works:

  • Alemanno et al.: 2018, Global Map of Martian Fluvial Systems: Age and Total Eroded Volume Estimations, Earth and Space Science Journal, 5, 560-577, doi:https://doi.org/10.1029/2018EA000362
  • Orofino et al.: 2018, Estimate of the water flow duration in large Martian fluvial systems. Planetary and Space Science Journal, 163, 83-96. doi: 10.1016/j.pss.2018.06.001
  • Alemanno G.: 2018, Study of the fluvial activity on Mars through mapping, sediment transport modelling and spectroscopic analyses. PhD dissertation thesis, arXiv:1805.02208 [astro-ph.EP].
This figure shows the additions to the previous valley network database (Hynek et al. 2010) in a sample region. Blue lines represent valley networks mapped by Hynek et al. 2010 and red lines represent additions by Alemanno et al. 2018.



Reference: Portyankina, G., 2005. Atmosphere-surface vapor exchange and ices in the Martian polar regions. PhD thesis, ISBN 3-936586-47-0

Database: Excel

Method: Search limited to latitudes south of 75◦S. All MOC NA images in the PDS archive that cover regions inside this area were checked visually for the presence of spider patterns. Images that contain single spiders, spider arrays, or spider ravines were selected for further analysis. Each of such images was counted as one entry. The archive covers the period from September 1997 to March 2004. We found 326 images that contain spider patterns.

Feature: The name ”martian spiders” was introduced by the MOC team to describe structures that show several branches diverging from one common center. Soon after the first detection they were discovered to be negative topographical features (depressions) – i.e. radial troughs or channels.



Polygonal ridges (boxwork or reticulate ridges)

Description Global map of polygonal ridge networks on Mars
Links http://www.sciencedirect.com/science/article/pii/S0019103516305000#bib0041
Citation Kerber L, Dickson JL, Head JW, Grosfils EB (2016) Polygonal ridge networks on Mars: Diversity of morphologies and the special case of the Eastern Medusae Fossae Formation. Icarus http://dx.doi.org/10.1016/j.icarus.2016.08.020


Reference figure Fig. 1

Datapoints published? No

Methods Using the Mars version of Google Earth (earth.google.com/mars/), we surveyed Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and Mars Express High Resolution Stereo Camera (HRSC) images near previously documented ridge occurrences. We then reviewed the 887 MRO High Resolution Imaging Science Experiment (HiRISE) images in the HiRISE catalog that were tagged with the keyword “ridges” by the HiRISE team (www.uahirise.org; as of 5/30/16). Where polygonal ridge networks were present, we mapped their regional extents using the broader spatial coverage of CTX data within the geographic information system software ArcGIS. The entire area of the Medusae Fossae Formation and the Hellas Basin floor deposits were separately surveyed at CTX scale to find additional ridge networks where HiRISE data were sparse.

Significance The diversity of the ridge networks implies a variety of formational mechanisms.

Shapefile YES. Original shapefile

Volcanoes on Mars (composite catalog)

Shapefile https://www.dropbox.com/s/554yilypb5sx0cs/volcano.zip?dl=0
Notes All data were re-drawn as ellipses that best fit the feature in THEMIS Day imagery and/or MOLA relief. All values were calculated from the re-drawn ellipses.
Lat/Lon are calculated as the centers of ellipses, not Lat/Lon values in the source papers
Diameter, area, perimeter are calculated from the ellipses, and are not taken from the source papers. Diameter is an average, calculated from perimeter.
Height (Max. elev, range of elevation) data are calculated from within the ellipses, and are not taken from the source papers. Heigh data is from MOLA gridded data. MAX=max elevation point within the ellipse, MIN: min. elevation value point within the ellipse
Type/interpretations are taken from the source papers. For small cones and mounds, interpretations vary (pingo/volcano/mud volcano). All features that have at least one volcanic interpretation in a recent (ca. last two decades) paper are included. Features previously (Viking) identified as volcanic but recently reclassified are not included.

Confidence. Major and minor shields, calderas, fissure/small/low shields and lava domes can be considered as confirmed, while all others are candidate volcanic features.

Group: a single ellipse is one example showing actual size, which is part of a group of similar sized features. These are typically interpreted as pseudocraters (rootless cones) or pingos or mud volcanoes.
Type: Caldera: size/range values represent caldera, not volcanic construct (if any). These are caldera volcanoes without substantial construct. (negative relief forms)
Database Editor Henrik Hargitai, with the help of P. Broz



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