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: 69
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
Granular flows at recurring slope lineae on Mars indicate a limited role for liquid water
Recent liquid water flow on Mars has been proposed based on geomorphological features, such as gullies. Recurring slope lineae — seasonal flows that are darker than their surroundings — are candidate locations for seeping liquid water on Mars today, but their formation mechanism remains unclear. Topographical analysis shows that the terminal slopes of recurring slope lineae match the stopping angl
Authors
Colin M. Dundas, Alfred S. McEwen, Matthew Chojnacki, Moses P. Milazzo, Shane Byrne, Jim McElwaine, Anna Urso
Changes in blast zone albedo patterns around new martian impact craters
“Blast zones” (BZs) around new martian craters comprise various albedo features caused by the initial impact, including diffuse halos, extended linear and arcuate rays, secondary craters, ejecta patterns, and dust avalanches. We examined these features for changes in repeat images separated by up to four Mars years. Here we present the first comprehensive survey of the qualitative and quantitative
Authors
Ingrid J. Daubar, Colin M. Dundas, Shane Byrne, Paul E. Geissler, Gwen Bart, Alfred S. McEwen, Patrick Russell, Matthew Chojnacki, M.P. Golombek
Effects of varying obliquity on Martian sublimation thermokarst landforms
Scalloped depressions in the Martian mid-latitudes are likely formed by sublimation of ice-rich ground. The stability of subsurface ice changes with the planetary obliquity, generally becoming less stable at lower axial tilt. As a result, the relative rates of sublimation and creep change over time. A landscape evolution model shows that these variations produce internal structure in scalloped dep
Authors
Colin M. Dundas
Special section introduction on MicroMars to MegaMars
The study of Earth's surface and atmosphere evolved from local investigations to the incorporation of remote sensing on a global scale. The study of Mars has followed the opposite progression, beginning with telescopic observations, followed by flyby and orbital missions, landers, and finally rover missions in the last ∼20 years. This varied fleet of spacecraft (seven of which are currently operat
Authors
Nathan T. Bridges, Colin M. Dundas, Lauren A. Edgar
Geologic context of recurring slope lineae in Melas and Coprates Chasmata, Mars
One of the major Mars discoveries of recent years is the existence of recurring slope lineae (RSL), which suggests that liquid water occurs on or near the surface of Mars today. These dark and narrow features emerge from steep, rocky exposures and incrementally grow, fade, and reform on a seasonal basis and are detected in images from the High Resolution Imaging Science Experiment camera. RSL are
Authors
Matthew Chojnacki, Alfred McEwen, Colin M. Dundas, Lujendra Ojha, Anna Urso, Sarah Sutton
A revised surface age for the North Polar Layered Deposits of Mars
The North Polar Layered Deposits (NPLD) of Mars contain a complex stratigraphy that has been suggested to retain a record of past eccentricity- and obliquity-forced climate changes. The surface accumulation rate in the current climate can be constrained by the crater retention age. We scale NPLD crater diameters to account for icy target strength and compare surface age using a new production func
Authors
Margaret E. Landis, Shane Byrne, Ingrid J. Daubar, Kenneth E. Herkenhoff, Colin M. Dundas
Limited role for thermal erosion by turbulent lava in proximal Athabasca Valles, Mars
The Athabasca Valles flood lava is among the most recent (<50 Ma) and best preserved effusive lava flows on Mars and was probably emplaced turbulently. The Williams et al. (2005) model of thermal erosion by lava has been applied to what we term “proximal Athabasca,” the 75 km long upstream portion of Athabasca Valles. For emplacement volumes of 5000 and 7500 km3and average flow thicknesses of 20 a
Authors
Vincenzo Cataldo, David A. Williams, Colin M. Dundas, Laszlo P. Kestay
Modeling the development of martian sublimation thermokarst landforms
Sublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsurface. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the mid-latitudes and considered likely thermokarst features. We describe a landscape evolution model that couples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens of
Authors
Colin M. Dundas, Shane Byrne, Alfred S. McEwen
Science and Products
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- Publications
Filter Total Items: 69
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 consisteAuthorsLivio 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. WrayOrigin 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 modAuthorsCarolyn H. Van der Bogert, Harald Hiesinger, Colin M. Dundas, T. Kruger, Alfred S. McEwen, Michael Zanetti, Mark S. RobinsonSubsurface 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 craterAuthorsDonna Viola, Alfred S. McEwen, Colin M. Dundas, Shane ByrneEffects 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-meAuthorsColin M. DundasGranular flows at recurring slope lineae on Mars indicate a limited role for liquid water
Recent liquid water flow on Mars has been proposed based on geomorphological features, such as gullies. Recurring slope lineae — seasonal flows that are darker than their surroundings — are candidate locations for seeping liquid water on Mars today, but their formation mechanism remains unclear. Topographical analysis shows that the terminal slopes of recurring slope lineae match the stopping anglAuthorsColin M. Dundas, Alfred S. McEwen, Matthew Chojnacki, Moses P. Milazzo, Shane Byrne, Jim McElwaine, Anna UrsoChanges in blast zone albedo patterns around new martian impact craters
“Blast zones” (BZs) around new martian craters comprise various albedo features caused by the initial impact, including diffuse halos, extended linear and arcuate rays, secondary craters, ejecta patterns, and dust avalanches. We examined these features for changes in repeat images separated by up to four Mars years. Here we present the first comprehensive survey of the qualitative and quantitativeAuthorsIngrid J. Daubar, Colin M. Dundas, Shane Byrne, Paul E. Geissler, Gwen Bart, Alfred S. McEwen, Patrick Russell, Matthew Chojnacki, M.P. GolombekEffects of varying obliquity on Martian sublimation thermokarst landforms
Scalloped depressions in the Martian mid-latitudes are likely formed by sublimation of ice-rich ground. The stability of subsurface ice changes with the planetary obliquity, generally becoming less stable at lower axial tilt. As a result, the relative rates of sublimation and creep change over time. A landscape evolution model shows that these variations produce internal structure in scalloped depAuthorsColin M. DundasSpecial section introduction on MicroMars to MegaMars
The study of Earth's surface and atmosphere evolved from local investigations to the incorporation of remote sensing on a global scale. The study of Mars has followed the opposite progression, beginning with telescopic observations, followed by flyby and orbital missions, landers, and finally rover missions in the last ∼20 years. This varied fleet of spacecraft (seven of which are currently operatAuthorsNathan T. Bridges, Colin M. Dundas, Lauren A. EdgarGeologic context of recurring slope lineae in Melas and Coprates Chasmata, Mars
One of the major Mars discoveries of recent years is the existence of recurring slope lineae (RSL), which suggests that liquid water occurs on or near the surface of Mars today. These dark and narrow features emerge from steep, rocky exposures and incrementally grow, fade, and reform on a seasonal basis and are detected in images from the High Resolution Imaging Science Experiment camera. RSL areAuthorsMatthew Chojnacki, Alfred McEwen, Colin M. Dundas, Lujendra Ojha, Anna Urso, Sarah SuttonA revised surface age for the North Polar Layered Deposits of Mars
The North Polar Layered Deposits (NPLD) of Mars contain a complex stratigraphy that has been suggested to retain a record of past eccentricity- and obliquity-forced climate changes. The surface accumulation rate in the current climate can be constrained by the crater retention age. We scale NPLD crater diameters to account for icy target strength and compare surface age using a new production funcAuthorsMargaret E. Landis, Shane Byrne, Ingrid J. Daubar, Kenneth E. Herkenhoff, Colin M. DundasLimited role for thermal erosion by turbulent lava in proximal Athabasca Valles, Mars
The Athabasca Valles flood lava is among the most recent (<50 Ma) and best preserved effusive lava flows on Mars and was probably emplaced turbulently. The Williams et al. (2005) model of thermal erosion by lava has been applied to what we term “proximal Athabasca,” the 75 km long upstream portion of Athabasca Valles. For emplacement volumes of 5000 and 7500 km3and average flow thicknesses of 20 aAuthorsVincenzo Cataldo, David A. Williams, Colin M. Dundas, Laszlo P. KestayModeling the development of martian sublimation thermokarst landforms
Sublimation-thermokarst landforms result from collapse of the surface when ice is lost from the subsurface. On Mars, scalloped landforms with scales of decameters to kilometers are observed in the mid-latitudes and considered likely thermokarst features. We describe a landscape evolution model that couples diffusive mass movement and subsurface ice loss due to sublimation. Over periods of tens ofAuthorsColin M. Dundas, Shane Byrne, Alfred S. McEwen - News