Colin Dundas, Ph.D.
Colin Dundas is a Research Geologist with the Astrogeology Science Center. He studies planetary geomorphology and surface processes using spacecraft imagery and topography data as well as numerical modeling, with a particular focus on active processes and change detection. He is a Co-Investigator and Science Theme Lead for Mass Wasting on the HiRISE camera team.
Past and current research areas include:
- Current activity on Martian slopes, including Recurring Slope Lineae and changes in gullies
- Martian ground ice, ice-exposing impact craters and scarps, and sublimation-thermokarst landforms
- Large lava flows and lava-volatile interactions on Mars, Io, and Earth
- Effects of target properties and secondary craters on crater chronology
- Floods in Martian outflow channels
- Volatile-loss landforms in the Solar System
Professional Experience
2009-2011: Postdoctoral researcher at the University of Arizona.
2011 - Present: Research Geologist at the USGS Astrogeology Science Center
Education and Certifications
Ph.D., Planetary Science (Geoscience minor), The University of Arizona, 2009
B.S., Planetary Science, California Institute of Technology, 2004
Science and Products
Filter Total Items: 77
An aeolian grainflow model for Martian Recurring Slope Lineae
Recurring Slope Lineae (RSL) on Mars have been enigmatic since their discovery; their behavior resembles a seeping liquid but sources of water remain puzzling. This work demonstrates that the properties of RSL are consistent with observed behaviors of Martian and terrestrial aeolian processes. Specifically, RSL are well-explained as flows of sand that remove a thin coating of dust. Observed RSL pr
Authors
Colin M. Dundas
Present-day mass wasting in sulfate-rich sediments in the equatorial regions of Mars
Present-day topographic changes are observed on steep slopes in equatorial regions of Mars that are associated with sulfate-rich sediments. Hydrated sulfates are known to be present in many sedimentary deposits on Mars. We document volume changes in the form of mass movements and gullies over these regions. We have estimated erosion rates of ~12 mm/yr (or ~1.2–120 mm/yr with uncertainties) over st
Authors
Melissa F Thomas, Alfred S. McEwen, Colin M. Dundas
Report from the Ice and Climate Evolution Science Analysis group (ICE-SAG)
This document is the final report of the Ice and Climate Evolution Science Analysis Group (ICESAG) that was formed by the Mars Exploration Program Analysis Group (MEPAG) as part of its preparations for the upcoming NASA Planetary Science Decadal Survey for 2023 through 2032 (see §1). Through telecons, one face-to-face meeting, and discussions with experts in relevant topics, ICE-SAG has identified
Authors
Than Putzig, Serina Diniega, Colin M. Dundas, Timothy N. Titus
Active boulder movement at high Martian latitudes
Lobate stony landforms occur on steep slopes at high latitudes on Mars. We demonstrate active boulder movement at seven such sites. Sub-meter-scale boulders frequently move distances of a few meters. The movement is concentrated in the vicinity of the lobate landforms but also occurs on other slopes. This provides evidence for a new, common style of activity on Mars, which may play an important ro
Authors
Colin M. Dundas, Michael T. Mellon, Susan J. Conway, Renaldo Gastineau
Dark halos produced by current impact cratering on Mars
Hundreds of new impact craters have been observed to form on Mars since spacecraft began imaging that planet. New impact craters produced visible ejecta deposits and many of them also have visible rays, similar to lunar and mercurian craters. However, some of the new martian impact craters have a circular feature of relatively low reflectance that we call a “halo.” This feature is distinct from th
Authors
Gwendolyn D. Bart, Ingrid J. Daubar, Boris A Ivanov, Colin M. Dundas, Alfred S. McEwen
The formation of gullies on Mars today
A decade of high-resolution monitoring has revealed extensive activity in fresh Martian gullies. Flows within the gullies are diverse: they can be relatively light, neutral or dark, colourful or bland, and range from superficial deposits to 10 m-scale topographic changes. We observed erosion and transport of material within gullies, new terraces, freshly eroded channel segments, migrating sinuous
Authors
Colin M. Dundas, Alfred S. McEwen, Serina Diniega, Candice J. Hansen, Jim N. McElwaince
The flood lavas of Kasei Valles, Mars
Both the northern and southern arms of Kasei Valles are occupied by platy-ridged flood lavas. We have mapped these flows and examined their morphology to better understand their emplacement. The lavas were emplaced as high-flux, turbulent flows (exceeding 106 m3 s−1). Lava in southern Kasei Valles can be traced back up onto the Tharsis rise, which is also the likely source of lavas in the northern
Authors
Colin M. Dundas, Glen E. Cushing, Laszlo P. Kestay
Exposed subsurface ice sheets in the Martian mid-latitudes
Thick deposits cover broad regions of the Martian mid-latitudes with a smooth mantle; erosion
in these regions creates scarps that expose the internal structure of the mantle.We
investigated eight of these locations and found that they expose deposits of water ice that
can be >100 meters thick, extending downward from depths as shallow as 1 to 2 meters below
the surface.The scarps are actively ret
Authors
Colin M. Dundas, Ali M Bramson, Lujendra Ojha, James J. Wray, Michael T. Mellon, Shane Byrne, Alfred S. McEwen, N. E. Putzig, Donna Viola, Sarah Sutton, E. Clark, J.W. Holt
Image simulation and assessment of the colour and spatial capabilities of the Colour and Stereo Surface Imaging System (CaSSIS) on the ExoMars Trace Gas Orbiter
This study aims to assess the spatial and visible/near-infrared (VNIR) colour/spectral capabilities of the 4-band Colour and Stereo Surface Imaging System (CaSSIS) aboard the ExoMars 2016 Trace Grace Orbiter (TGO). The instrument response functions for the CaSSIS imager was used to resample spectral libraries, modelled spectra and to construct spectrally (i.e., in I/F space) and spatially consiste
Authors
Livio L. Tornabene, Frank P. Seelos, Antoine Pommerol, Nicolas Thomas, Christy M. Caudill, Patricio Becerra, John C. Bridges, Shane Byrne, Marco Cardinale, Matthew Chojnacki, Susan J. Conway, Gabriele Cremonese, Colin M. Dundas, M. R. El-Maarry, Jennifer Fernando, Candice J. Hansen, Kayle Hansen, Tanya N. Harrison, Rachel Henson, Lucia Marinangeli, Alfred S. McEwen, Maurizio Pajola, Sarah S. Sutton, James J. Wray
Origin of discrepancies between crater size-frequency distributions of coeval lunar geologic units via target property contrasts
Recent work on dating Copernican-aged craters, using Lunar Reconnaissance Orbiter (LRO) Camera data, re-encountered a curious discrepancy in crater size-frequency distribution (CSFD) measurements that was observed, but not understood, during the Apollo era. For example, at Tycho, Copernicus, and Aristarchus craters, CSFDs of impact melt deposits give significantly younger relative and absolute mod
Authors
Carolyn H. Van der Bogert, Harald Hiesinger, Colin M. Dundas, T. Kruger, Alfred S. McEwen, Michael Zanetti, Mark S. Robinson
Subsurface volatile content of martian double-layer ejecta (DLE) craters
Excess ice is widespread throughout the martian mid-latitudes, particularly in Arcadia Planitia, where double-layer ejecta (DLE) craters also tend to be abundant. In this region, we observe the presence of thermokarstically-expanded secondary craters that likely form from impacts that destabilize a subsurface layer of excess ice, which subsequently sublimates. The presence of these expanded crater
Authors
Donna Viola, Alfred S. McEwen, Colin M. Dundas, Shane Byrne
Effects of lava heating on volatile-rich slopes on Io
The upper crust of Io may be very rich in volatile sulfur and SO2. The surface is also highly volcanically active, and slopes may be warmed by radiant heat from the lava. This is particularly the case in paterae, which commonly host volcanic eruptions and long-lived lava lakes. Paterae slopes are highly variable, but some are greater than 70°. I model the heating of a volatile slope for two end-me
Authors
Colin M. Dundas
Science and Products
Filter Total Items: 77
An aeolian grainflow model for Martian Recurring Slope Lineae
Recurring Slope Lineae (RSL) on Mars have been enigmatic since their discovery; their behavior resembles a seeping liquid but sources of water remain puzzling. This work demonstrates that the properties of RSL are consistent with observed behaviors of Martian and terrestrial aeolian processes. Specifically, RSL are well-explained as flows of sand that remove a thin coating of dust. Observed RSL pr
Authors
Colin M. Dundas
Present-day mass wasting in sulfate-rich sediments in the equatorial regions of Mars
Present-day topographic changes are observed on steep slopes in equatorial regions of Mars that are associated with sulfate-rich sediments. Hydrated sulfates are known to be present in many sedimentary deposits on Mars. We document volume changes in the form of mass movements and gullies over these regions. We have estimated erosion rates of ~12 mm/yr (or ~1.2–120 mm/yr with uncertainties) over st
Authors
Melissa F Thomas, Alfred S. McEwen, Colin M. Dundas
Report from the Ice and Climate Evolution Science Analysis group (ICE-SAG)
This document is the final report of the Ice and Climate Evolution Science Analysis Group (ICESAG) that was formed by the Mars Exploration Program Analysis Group (MEPAG) as part of its preparations for the upcoming NASA Planetary Science Decadal Survey for 2023 through 2032 (see §1). Through telecons, one face-to-face meeting, and discussions with experts in relevant topics, ICE-SAG has identified
Authors
Than Putzig, Serina Diniega, Colin M. Dundas, Timothy N. Titus
Active boulder movement at high Martian latitudes
Lobate stony landforms occur on steep slopes at high latitudes on Mars. We demonstrate active boulder movement at seven such sites. Sub-meter-scale boulders frequently move distances of a few meters. The movement is concentrated in the vicinity of the lobate landforms but also occurs on other slopes. This provides evidence for a new, common style of activity on Mars, which may play an important ro
Authors
Colin M. Dundas, Michael T. Mellon, Susan J. Conway, Renaldo Gastineau
Dark halos produced by current impact cratering on Mars
Hundreds of new impact craters have been observed to form on Mars since spacecraft began imaging that planet. New impact craters produced visible ejecta deposits and many of them also have visible rays, similar to lunar and mercurian craters. However, some of the new martian impact craters have a circular feature of relatively low reflectance that we call a “halo.” This feature is distinct from th
Authors
Gwendolyn D. Bart, Ingrid J. Daubar, Boris A Ivanov, Colin M. Dundas, Alfred S. McEwen
The formation of gullies on Mars today
A decade of high-resolution monitoring has revealed extensive activity in fresh Martian gullies. Flows within the gullies are diverse: they can be relatively light, neutral or dark, colourful or bland, and range from superficial deposits to 10 m-scale topographic changes. We observed erosion and transport of material within gullies, new terraces, freshly eroded channel segments, migrating sinuous
Authors
Colin M. Dundas, Alfred S. McEwen, Serina Diniega, Candice J. Hansen, Jim N. McElwaince
The flood lavas of Kasei Valles, Mars
Both the northern and southern arms of Kasei Valles are occupied by platy-ridged flood lavas. We have mapped these flows and examined their morphology to better understand their emplacement. The lavas were emplaced as high-flux, turbulent flows (exceeding 106 m3 s−1). Lava in southern Kasei Valles can be traced back up onto the Tharsis rise, which is also the likely source of lavas in the northern
Authors
Colin M. Dundas, Glen E. Cushing, Laszlo P. Kestay
Exposed subsurface ice sheets in the Martian mid-latitudes
Thick deposits cover broad regions of the Martian mid-latitudes with a smooth mantle; erosion
in these regions creates scarps that expose the internal structure of the mantle.We
investigated eight of these locations and found that they expose deposits of water ice that
can be >100 meters thick, extending downward from depths as shallow as 1 to 2 meters below
the surface.The scarps are actively ret
Authors
Colin M. Dundas, Ali M Bramson, Lujendra Ojha, James J. Wray, Michael T. Mellon, Shane Byrne, Alfred S. McEwen, N. E. Putzig, Donna Viola, Sarah Sutton, E. Clark, J.W. Holt
Image simulation and assessment of the colour and spatial capabilities of the Colour and Stereo Surface Imaging System (CaSSIS) on the ExoMars Trace Gas Orbiter
This study aims to assess the spatial and visible/near-infrared (VNIR) colour/spectral capabilities of the 4-band Colour and Stereo Surface Imaging System (CaSSIS) aboard the ExoMars 2016 Trace Grace Orbiter (TGO). The instrument response functions for the CaSSIS imager was used to resample spectral libraries, modelled spectra and to construct spectrally (i.e., in I/F space) and spatially consiste
Authors
Livio L. Tornabene, Frank P. Seelos, Antoine Pommerol, Nicolas Thomas, Christy M. Caudill, Patricio Becerra, John C. Bridges, Shane Byrne, Marco Cardinale, Matthew Chojnacki, Susan J. Conway, Gabriele Cremonese, Colin M. Dundas, M. R. El-Maarry, Jennifer Fernando, Candice J. Hansen, Kayle Hansen, Tanya N. Harrison, Rachel Henson, Lucia Marinangeli, Alfred S. McEwen, Maurizio Pajola, Sarah S. Sutton, James J. Wray
Origin of discrepancies between crater size-frequency distributions of coeval lunar geologic units via target property contrasts
Recent work on dating Copernican-aged craters, using Lunar Reconnaissance Orbiter (LRO) Camera data, re-encountered a curious discrepancy in crater size-frequency distribution (CSFD) measurements that was observed, but not understood, during the Apollo era. For example, at Tycho, Copernicus, and Aristarchus craters, CSFDs of impact melt deposits give significantly younger relative and absolute mod
Authors
Carolyn H. Van der Bogert, Harald Hiesinger, Colin M. Dundas, T. Kruger, Alfred S. McEwen, Michael Zanetti, Mark S. Robinson
Subsurface volatile content of martian double-layer ejecta (DLE) craters
Excess ice is widespread throughout the martian mid-latitudes, particularly in Arcadia Planitia, where double-layer ejecta (DLE) craters also tend to be abundant. In this region, we observe the presence of thermokarstically-expanded secondary craters that likely form from impacts that destabilize a subsurface layer of excess ice, which subsequently sublimates. The presence of these expanded crater
Authors
Donna Viola, Alfred S. McEwen, Colin M. Dundas, Shane Byrne
Effects of lava heating on volatile-rich slopes on Io
The upper crust of Io may be very rich in volatile sulfur and SO2. The surface is also highly volcanically active, and slopes may be warmed by radiant heat from the lava. This is particularly the case in paterae, which commonly host volcanic eruptions and long-lived lava lakes. Paterae slopes are highly variable, but some are greater than 70°. I model the heating of a volatile slope for two end-me
Authors
Colin M. Dundas