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
Lava–water interaction and hydrothermal activity within the 2014–2015 Holuhraun Lava Flow Field, Iceland
Lava that erupted during the 2014–2015 Holuhraun eruption in Iceland flowed into a proglacial river system, resulting in aqueous cooling of the lava and an ephemeral hydrothermal system. We carried out a monitoring study of this system from 2015 to 2018 to document the cooling of the lava over this time, using thermocouple measurements and data-logging sensors. The heat loss rate from advection th
Authors
Colin M. Dundas, Laszlo P. Keszthelyi, Einat Lev, M. Elise Rumpf, Christopher W. Hamilton, Armann Hoskuldsson, Thorvaldur Thordarson
Mars orbiter for resources, ices, and environments (MORIE)
The MORIE mission concept study examined the science and technical trade space to address high priority questions related to ice reservoirs and environmental transitions. The study team converged on a medium-class SEP-enabled orbiter with seven instruments to unlock the extent and volume of subsurface ice and geologic sequence stratigraphy through time. Observations would include the first radar i
Authors
Wendy M. Calvin, Nathaniel E. Putzig, John W Holt, Ali M Bramson, Colin M. Dundas, Bethany L. Ehlmann, Briony H. N. Horgan, Gareth A Morgan, Scott L. Murchie, G Wesley Patterson, Kimberly D. Seelos, Hanna G Sizemore, Steve Matousek, Ryan Woolley, Carlos Brinoccolo, Valerie Scott, Cassie Stuurman, Kevin Wheeler, Brian Sutin, Marc Lane, Nathan Barba, Ivair Gontijo, Katherine Park, Mariko Burgin, Scott Hensley, Jan Martin, Jean Biancone, David Hinkle, Barbara Insua
Geomorphological evidence for a dry dust avalanche origin of slope streaks on Mars
Mars has several different types of slope feature that resemble aqueous flows. However, the current cold, dry conditions are inimical to liquid water, resulting in uncertainty about its role in modern surface processes. Dark slope streaks were among the first distinctive young slope features to be identified on Mars and the first with activity seen in orbital images. They form markings on steep sl
Authors
Colin M. Dundas
Sparse subsurface radar reflectors in Hellas Planitia, Mars
Geomorphological features potentially related to subsurface ice, such as scalloped depressions, expanded craters, pedestal craters, and banded terrain, are present in and around Hellas Planitia, Mars. We present a radar survey of the region using the Shallow Radar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO) to identify candidate subsurface reflectors that may be due to the p
Authors
Claire W Cook, Ali M Bramson, Shane Byrne, John W Holt, Michael S Christoffersen, Donna Viola, Colin M. Dundas, Timothy A Goudge
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
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Filter Total Items: 69
Lava–water interaction and hydrothermal activity within the 2014–2015 Holuhraun Lava Flow Field, Iceland
Lava that erupted during the 2014–2015 Holuhraun eruption in Iceland flowed into a proglacial river system, resulting in aqueous cooling of the lava and an ephemeral hydrothermal system. We carried out a monitoring study of this system from 2015 to 2018 to document the cooling of the lava over this time, using thermocouple measurements and data-logging sensors. The heat loss rate from advection thAuthorsColin M. Dundas, Laszlo P. Keszthelyi, Einat Lev, M. Elise Rumpf, Christopher W. Hamilton, Armann Hoskuldsson, Thorvaldur ThordarsonMars orbiter for resources, ices, and environments (MORIE)
The MORIE mission concept study examined the science and technical trade space to address high priority questions related to ice reservoirs and environmental transitions. The study team converged on a medium-class SEP-enabled orbiter with seven instruments to unlock the extent and volume of subsurface ice and geologic sequence stratigraphy through time. Observations would include the first radar iAuthorsWendy M. Calvin, Nathaniel E. Putzig, John W Holt, Ali M Bramson, Colin M. Dundas, Bethany L. Ehlmann, Briony H. N. Horgan, Gareth A Morgan, Scott L. Murchie, G Wesley Patterson, Kimberly D. Seelos, Hanna G Sizemore, Steve Matousek, Ryan Woolley, Carlos Brinoccolo, Valerie Scott, Cassie Stuurman, Kevin Wheeler, Brian Sutin, Marc Lane, Nathan Barba, Ivair Gontijo, Katherine Park, Mariko Burgin, Scott Hensley, Jan Martin, Jean Biancone, David Hinkle, Barbara InsuaGeomorphological evidence for a dry dust avalanche origin of slope streaks on Mars
Mars has several different types of slope feature that resemble aqueous flows. However, the current cold, dry conditions are inimical to liquid water, resulting in uncertainty about its role in modern surface processes. Dark slope streaks were among the first distinctive young slope features to be identified on Mars and the first with activity seen in orbital images. They form markings on steep slAuthorsColin M. DundasSparse subsurface radar reflectors in Hellas Planitia, Mars
Geomorphological features potentially related to subsurface ice, such as scalloped depressions, expanded craters, pedestal craters, and banded terrain, are present in and around Hellas Planitia, Mars. We present a radar survey of the region using the Shallow Radar (SHARAD) instrument on board the Mars Reconnaissance Orbiter (MRO) to identify candidate subsurface reflectors that may be due to the pAuthorsClaire W Cook, Ali M Bramson, Shane Byrne, John W Holt, Michael S Christoffersen, Donna Viola, Colin M. Dundas, Timothy A GoudgeAn 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 prAuthorsColin M. DundasPresent-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 stAuthorsMelissa F Thomas, Alfred S. McEwen, Colin M. DundasReport 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 identifiedAuthorsThan Putzig, Serina Diniega, Colin M. Dundas, Timothy N. TitusActive 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 roAuthorsColin M. Dundas, Michael T. Mellon, Susan J. Conway, Renaldo GastineauDark 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 thAuthorsGwendolyn D. Bart, Ingrid J. Daubar, Boris A Ivanov, Colin M. Dundas, Alfred S. McEwenThe 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 sinuousAuthorsColin M. Dundas, Alfred S. McEwen, Serina Diniega, Candice J. Hansen, Jim N. McElwainceThe 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 northernAuthorsColin M. Dundas, Glen E. Cushing, Laszlo P. KestayExposed 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 retAuthorsColin 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 - News