Mike Bland is a research space scientist at the U.S. Geological Survey Astrogeology Science Center. His interests primarily lie in combining numerical models with planetary datasets to understand the thermal and tectonic evolution of ice-rich bodies.
Past and current research areas include:
- The mechanics of rifting in ice lithospheres (e.g., Ganymede and Enceladus)
- The formation of contractional features on icy bodies (e.g., Europa, Enceladus, Titan)
- Crater modification due to viscous relaxation (Enceladus and Ceres)
- Mountain formation on Io
- Differentiation of large icy satellites (Ganymede and Titan)
- Production of Ganymede's magnetic field
Professional Experience
Dawn at Ceres Guest Investigator
Education and Certifications
Ph.D. Planetary Science, University of Arizona, Tucson AZ (2008)
BA Physics/Geology, Gustavus Adolphus College, St. Peter MN (2002)
Honors and Awards
First Decade Award, Gustavus Adolphus College (2012)
NASA Earth and Space Science Fellowship (2007)
Gerard P. Kuiper Award, University of Arizona (2007)
Science and Products
Photogrammetrically Controlled, Equirectangular Galileo Image Mosaics of Europa
The Solid State Imager (SSI) on NASA's Galileo spacecraft acquired more than 500 images of Jupiter's moon, Europa, providing the only moderate- to high-resolution images of the moon's surface. Images were acquired as observation sequences during each orbit that targeted the moon. Each of these observation sequences consists of between 1 and 19 images acquired close in time, that typically overlap,
Filter Total Items: 30
Exploring the interior of Europa with the Europa Clipper
The Galileo mission to Jupiter revealed that Europa is an ocean world. The Galileo magnetometer experiment in particular provided strong evidence for a salty subsurface ocean beneath the ice shell, likely in contact with the rocky core. Within the ice shell and ocean, a number of tectonic and geodynamic processes may operate today or have operated at some point in the past, including solid ice con
Authors
James Roberts, William B. McKinnon, Catherine Elder, Gabriel Tobie, John Biersteker, Duncan Young, Ryan S. Park, Gregor Steinbrügge, Francis Nimmo, Samuel Howell, Julie C. Castillo-Rogez, Morgan Cable, Jacob Abrahams, Michael T. Bland, Chase Chivers, Corey Cochrane, Andrew Dombard, Carolyn M. Ernst, Antonio Genova, Christopher Gerekos, Christopher R. Glein, Camilla Harris, Hamish Hay, Paul O. Hayne, Matthew Hedman, Hauke Hussmann, Xianzhe Jia, Krishan Khurana, Walter Kiefer, Randolph L. Kirk, Margaret Kivelson, Justin D. Lawrence, Erin J. Leonard, Jonathan Lunine, Erwan Mazarico, Thomas B. McCord, Alfred S. McEwen, Carol Paty, Lynnae Quick, Carol A. Raymond, Kurt Retherford, Lorenz Roth, Abigail Rymer, Joachim Saur, Kirk Scanlan, Dustin Schroeder, David Senske, Wencheng Shao, Krista Soderlund, Elizabeth Spiers, Marshall Styczinski, Paolo Tortora, Steven Vance, Michaela Villarreal, Benjamin Weiss, Joseph Westlake, Paul Withers, Natalie Wolfenbarger, Bonnie J. Buratti, Haje Korth, Robert Pappalardo, Interior Thematic Working Group
Viscous relaxation of Oort and Edgeworth craters on Pluto: Possible indicators of an epoch of early high heat flow
Impact craters, with their well-defined initial shapes, have proven useful as heat flow probes of a number of icy bodies, provided characteristics of viscous relaxation can be identified. For Pluto's numerous craters, such identifications are hampered/complicated by infilling and erosion by mobile volatile ices, but not in every case. Large craters offer relatively deep probes of rheological struc
Authors
W. B. McKinnon, Michael T. Bland, K. Singer, P. M. Schenk, S. Robbins
Constraints on the composition and thermal structure of Ariel’s icy crust as inferred from its largest observed impact crater
The large graben-like troughs and smooth plains visible on the surface of Ariel are indicative of a period of high heat flow in the Uranian moon's past. High heat flows on icy moons like Ariel can also enable viscous flow that removes impact crater topography, a process called viscous relaxation. Here we use numerical modeling to investigate the conditions necessary to viscously relax Ariel's larg
Authors
Michael T. Bland, Chloe B. Beddingfield, Tom A. Nordheim, Donald A. Patthoff, Steven D. Vance
Silicate volcanism on Europa’s seafloor and implications for habitability
Habitable ocean environments on Europa require an influx of reactants to maintain chemical disequilibrium. One possible source of reactants is seafloor volcanism. Modeling has shown that dissipation of tidal energy in Europa's asthenosphere can generate melt, but melt formation cannot be equated with volcanism. Melt must also be transported through Europa's cold lithosphere to erupt at the seafloo
Authors
Michael T. Bland, Catherine Elder
How well do we know Europa’s topography? An evaluation of the variability in digital terrain models of Europa.
Jupiter’s moon Europa harbors one of the most likely environments for extant extraterrestrial life. Determining whether Europa is truly habitable requires understanding the structure and thickness of its ice shell, including the existence of perched water or brines. Stereo-derived topography from images acquired by NASA Galileo’s Solid State Imager (SSI) of Europa are often used as a constraint on
Authors
Michael T. Bland, Randolph L. Kirk, Donna M. Galuszka, David Mayer, R. A. Beyer, Robin L. Fergason
Improving the usability of Galileo and Voyager images of Jupiter’s moon, Europa
NASA's Voyager 1, Voyager 2, and Galileo spacecraft acquired hundreds of images of Jupiter's moon Europa. These images provide the only moderate- to high-resolution views of the moon's surface and are therefore a critical resource for scientific analysis and future mission planning. Unfortunately, uncertain knowledge of the spacecraft's position and pointing during image acquisition resulted in si
Authors
Michael T. Bland, Lynn A. Weller, Brent Archinal, Ethan Smith, Benjamin H Wheeler
A global shape model for Saturn's moon Enceladus from a dense photogrammetric control network
A planetary bodys global shape provides both insight into its geologic evolution, and a key element of any Planetary Spatial Data Infrastructure (PSDI). NASAs Cassini mission to Saturn acquired more than 600 moderate- to high-resolution images (< 500 m/pixel) of the small, geologically active moon Enceladus. The moons internal global ocean and intriguing geology mark it as a candidate for future e
Authors
Michael T. Bland, Lynn A. Weller, David Mayer, Brent Archinal
Planetary science decadal survey planetary mission concept study report: Ceres: Exploration of Ceres’ habitability
Dwarf planet Ceres is a compelling target as an evolved ocean world with, at least, regional brine reservoirs and potentially ongoing geological activity. As the most water-rich body in the inner solar system (in relative abundance), it is a representative of the population of planetesimals that brought volatiles and organics to the inner solar system. Situated in the Main Belt of asteroids, Ceres
Authors
J. C. Castillo-Rogez, John Brody, Michael T. Bland, Debra Buczkowski, Robert Grimm, A. Hendrix, Kelly Miller, Thomas Prettyman, Lynnae Quick, Carol Raymond, Jennifer Scully, Michael M. Sori, Yasuhito Sekine, David Williams, Michael Zolensky
Dome formation on Ceres by sold-state flow analogous to terrestrial salt tectonics
The dwarf planet Ceres’s outer crust is a complex, heterogeneous mixture of ice, clathrates, salts and silicates. Numerous large domes on Ceres’s surface indicate a degree of geological activity. These domes have been attributed to cryovolcanism, but that is difficult to reconcile with Ceres’s small size and lack of long-lived heat sources. Here we alternatively propose that Ceres’s domes form by
Authors
Michael T. Bland, D. L Buczkowski, H. G. Sizemore, A. I. Ermakov, S. D King, M. M. Sori, C. A. Raymond, J. C. Castillo-Rogez, C. T. Russell
The NASA Roadmap to Ocean Worlds
In this article, we summarize the work of the NASA Outer Planets Assessment Group (OPAG) Roadmaps to Ocean Worlds (ROW) group. The aim of this group is to assemble the scientific framework that will guide the exploration of ocean worlds, and to identify and prioritize science objectives for ocean worlds over the next several decades. The overarching goal of an Ocean Worlds exploration program as d
Authors
A. Noble Hendrix, T. Hurford, L.M. Barge, Michael T. Bland, J.S. Bowman, W. Brinckerhoff, B. J. Buratti, M. Cable, J. C. Castillo-Rogez, G. C. Collins, S. Diniega, C.R. German, A.G. Hayes, T.M. Hoehler, S. Mehran Hosseini, C. Howett, A.S. McEwen, C. Neish, M. Neveu, T.A. Nordheim, G.W. Patterson, Donald A. Patthoff, C. Phillips, A. Rhoden, B. Schmidt, K. Singer, J. M. Soderblom, S.D. Vance
Cryovolcanic rates on Ceres revealed by topography
Cryovolcanism, defined here as the extrusion of icy material from depth, may be an important planetary phenomenon in shaping the surfaces of many worlds in the outer Solar System and revealing their thermal histories1,2,3. However, the physics, chemistry and ubiquity of this geologic process remain poorly understood, especially in comparison to the better-studied silicate volcanism on the terrestr
Authors
M. M. Sori, H. G. Sizemore, S. Byrne, A. M. Bramson, Michael T. Bland, N. T. Stein, C. T. Russell
Floor-fractured craters on Ceres and implications for interior processes
Several of the impact craters on Ceres have sets of fractures on their floors. These fractures appear similar to those found within a class of lunar craters referred to as floor-fractured craters (FFCs). We have cataloged the Ceres FFCs according to the classification scheme designed for the Moon. An analysis of the depth to diameter ratio for Ceres craters shows that, like lunar FFCs, the Ceres F
Authors
Debra L. Buczkowski, Hanna G. Sizemore, Michael T. Bland, Jennifer E. C. Scully, Lynnae C. Quick, Kynan H. G. Hughson, Ryan S. Park, F. Preusker, Carol A. Raymond, Christopher T. Russell
Non-USGS Publications**
Bland, M. T. 2013. Predicted crater morphologies on Ceres: Probing internal structure and evolution. Icarus, 226, 510-521.
Bland, M. T. and McKinnon, W. B., 2013. Does folding accommodate Europa’s contractional strain? The effect of surface temperature on fold formation in ice lithospheres. Geophys. Res. Lett., 40, 2534-2538, doi:10.1002/grl.50506.
Bland, M. T., and McKinnon, W. B., 2012. Forming Europa’s folds: Strain requirements for the production of large-amplitude deformation. Icarus,221, 694-709.
Bland, M. T., Singer, K. S., McKinnon, W. B., and Schenk, P. M. 2012. Enceladus’ extreme heat flux as revealed by its relaxed craters. Geo. Res. Lett., 39, L17204, doi:10.1029/2012GL052736.
Bland, M. T., McKinnon, W. B., and Showman, A. P., 2010. The effects of strain localization on the formation of Ganymede’s grooved terrain. Icarus, 210, 396-410.
Bland, M. T., Showman, A. P., and Tobie, G., 2009. The orbital-thermal evolution and global expansion of Ganymede. Icarus, 200, 207-221.
**Disclaimer: The views expressed in Non-USGS publications are those of the author and do not represent the views of the USGS, Department of the Interior, or the U.S. Government.
Science and Products
- Data
Photogrammetrically Controlled, Equirectangular Galileo Image Mosaics of Europa
The Solid State Imager (SSI) on NASA's Galileo spacecraft acquired more than 500 images of Jupiter's moon, Europa, providing the only moderate- to high-resolution images of the moon's surface. Images were acquired as observation sequences during each orbit that targeted the moon. Each of these observation sequences consists of between 1 and 19 images acquired close in time, that typically overlap, - Publications
Filter Total Items: 30
Exploring the interior of Europa with the Europa Clipper
The Galileo mission to Jupiter revealed that Europa is an ocean world. The Galileo magnetometer experiment in particular provided strong evidence for a salty subsurface ocean beneath the ice shell, likely in contact with the rocky core. Within the ice shell and ocean, a number of tectonic and geodynamic processes may operate today or have operated at some point in the past, including solid ice conAuthorsJames Roberts, William B. McKinnon, Catherine Elder, Gabriel Tobie, John Biersteker, Duncan Young, Ryan S. Park, Gregor Steinbrügge, Francis Nimmo, Samuel Howell, Julie C. Castillo-Rogez, Morgan Cable, Jacob Abrahams, Michael T. Bland, Chase Chivers, Corey Cochrane, Andrew Dombard, Carolyn M. Ernst, Antonio Genova, Christopher Gerekos, Christopher R. Glein, Camilla Harris, Hamish Hay, Paul O. Hayne, Matthew Hedman, Hauke Hussmann, Xianzhe Jia, Krishan Khurana, Walter Kiefer, Randolph L. Kirk, Margaret Kivelson, Justin D. Lawrence, Erin J. Leonard, Jonathan Lunine, Erwan Mazarico, Thomas B. McCord, Alfred S. McEwen, Carol Paty, Lynnae Quick, Carol A. Raymond, Kurt Retherford, Lorenz Roth, Abigail Rymer, Joachim Saur, Kirk Scanlan, Dustin Schroeder, David Senske, Wencheng Shao, Krista Soderlund, Elizabeth Spiers, Marshall Styczinski, Paolo Tortora, Steven Vance, Michaela Villarreal, Benjamin Weiss, Joseph Westlake, Paul Withers, Natalie Wolfenbarger, Bonnie J. Buratti, Haje Korth, Robert Pappalardo, Interior Thematic Working GroupViscous relaxation of Oort and Edgeworth craters on Pluto: Possible indicators of an epoch of early high heat flow
Impact craters, with their well-defined initial shapes, have proven useful as heat flow probes of a number of icy bodies, provided characteristics of viscous relaxation can be identified. For Pluto's numerous craters, such identifications are hampered/complicated by infilling and erosion by mobile volatile ices, but not in every case. Large craters offer relatively deep probes of rheological strucAuthorsW. B. McKinnon, Michael T. Bland, K. Singer, P. M. Schenk, S. RobbinsConstraints on the composition and thermal structure of Ariel’s icy crust as inferred from its largest observed impact crater
The large graben-like troughs and smooth plains visible on the surface of Ariel are indicative of a period of high heat flow in the Uranian moon's past. High heat flows on icy moons like Ariel can also enable viscous flow that removes impact crater topography, a process called viscous relaxation. Here we use numerical modeling to investigate the conditions necessary to viscously relax Ariel's largAuthorsMichael T. Bland, Chloe B. Beddingfield, Tom A. Nordheim, Donald A. Patthoff, Steven D. VanceSilicate volcanism on Europa’s seafloor and implications for habitability
Habitable ocean environments on Europa require an influx of reactants to maintain chemical disequilibrium. One possible source of reactants is seafloor volcanism. Modeling has shown that dissipation of tidal energy in Europa's asthenosphere can generate melt, but melt formation cannot be equated with volcanism. Melt must also be transported through Europa's cold lithosphere to erupt at the seaflooAuthorsMichael T. Bland, Catherine ElderHow well do we know Europa’s topography? An evaluation of the variability in digital terrain models of Europa.
Jupiter’s moon Europa harbors one of the most likely environments for extant extraterrestrial life. Determining whether Europa is truly habitable requires understanding the structure and thickness of its ice shell, including the existence of perched water or brines. Stereo-derived topography from images acquired by NASA Galileo’s Solid State Imager (SSI) of Europa are often used as a constraint onAuthorsMichael T. Bland, Randolph L. Kirk, Donna M. Galuszka, David Mayer, R. A. Beyer, Robin L. FergasonImproving the usability of Galileo and Voyager images of Jupiter’s moon, Europa
NASA's Voyager 1, Voyager 2, and Galileo spacecraft acquired hundreds of images of Jupiter's moon Europa. These images provide the only moderate- to high-resolution views of the moon's surface and are therefore a critical resource for scientific analysis and future mission planning. Unfortunately, uncertain knowledge of the spacecraft's position and pointing during image acquisition resulted in siAuthorsMichael T. Bland, Lynn A. Weller, Brent Archinal, Ethan Smith, Benjamin H WheelerA global shape model for Saturn's moon Enceladus from a dense photogrammetric control network
A planetary bodys global shape provides both insight into its geologic evolution, and a key element of any Planetary Spatial Data Infrastructure (PSDI). NASAs Cassini mission to Saturn acquired more than 600 moderate- to high-resolution images (< 500 m/pixel) of the small, geologically active moon Enceladus. The moons internal global ocean and intriguing geology mark it as a candidate for future eAuthorsMichael T. Bland, Lynn A. Weller, David Mayer, Brent ArchinalPlanetary science decadal survey planetary mission concept study report: Ceres: Exploration of Ceres’ habitability
Dwarf planet Ceres is a compelling target as an evolved ocean world with, at least, regional brine reservoirs and potentially ongoing geological activity. As the most water-rich body in the inner solar system (in relative abundance), it is a representative of the population of planetesimals that brought volatiles and organics to the inner solar system. Situated in the Main Belt of asteroids, CeresAuthorsJ. C. Castillo-Rogez, John Brody, Michael T. Bland, Debra Buczkowski, Robert Grimm, A. Hendrix, Kelly Miller, Thomas Prettyman, Lynnae Quick, Carol Raymond, Jennifer Scully, Michael M. Sori, Yasuhito Sekine, David Williams, Michael ZolenskyDome formation on Ceres by sold-state flow analogous to terrestrial salt tectonics
The dwarf planet Ceres’s outer crust is a complex, heterogeneous mixture of ice, clathrates, salts and silicates. Numerous large domes on Ceres’s surface indicate a degree of geological activity. These domes have been attributed to cryovolcanism, but that is difficult to reconcile with Ceres’s small size and lack of long-lived heat sources. Here we alternatively propose that Ceres’s domes form byAuthorsMichael T. Bland, D. L Buczkowski, H. G. Sizemore, A. I. Ermakov, S. D King, M. M. Sori, C. A. Raymond, J. C. Castillo-Rogez, C. T. RussellThe NASA Roadmap to Ocean Worlds
In this article, we summarize the work of the NASA Outer Planets Assessment Group (OPAG) Roadmaps to Ocean Worlds (ROW) group. The aim of this group is to assemble the scientific framework that will guide the exploration of ocean worlds, and to identify and prioritize science objectives for ocean worlds over the next several decades. The overarching goal of an Ocean Worlds exploration program as dAuthorsA. Noble Hendrix, T. Hurford, L.M. Barge, Michael T. Bland, J.S. Bowman, W. Brinckerhoff, B. J. Buratti, M. Cable, J. C. Castillo-Rogez, G. C. Collins, S. Diniega, C.R. German, A.G. Hayes, T.M. Hoehler, S. Mehran Hosseini, C. Howett, A.S. McEwen, C. Neish, M. Neveu, T.A. Nordheim, G.W. Patterson, Donald A. Patthoff, C. Phillips, A. Rhoden, B. Schmidt, K. Singer, J. M. Soderblom, S.D. VanceCryovolcanic rates on Ceres revealed by topography
Cryovolcanism, defined here as the extrusion of icy material from depth, may be an important planetary phenomenon in shaping the surfaces of many worlds in the outer Solar System and revealing their thermal histories1,2,3. However, the physics, chemistry and ubiquity of this geologic process remain poorly understood, especially in comparison to the better-studied silicate volcanism on the terrestrAuthorsM. M. Sori, H. G. Sizemore, S. Byrne, A. M. Bramson, Michael T. Bland, N. T. Stein, C. T. RussellFloor-fractured craters on Ceres and implications for interior processes
Several of the impact craters on Ceres have sets of fractures on their floors. These fractures appear similar to those found within a class of lunar craters referred to as floor-fractured craters (FFCs). We have cataloged the Ceres FFCs according to the classification scheme designed for the Moon. An analysis of the depth to diameter ratio for Ceres craters shows that, like lunar FFCs, the Ceres FAuthorsDebra L. Buczkowski, Hanna G. Sizemore, Michael T. Bland, Jennifer E. C. Scully, Lynnae C. Quick, Kynan H. G. Hughson, Ryan S. Park, F. Preusker, Carol A. Raymond, Christopher T. RussellNon-USGS Publications**
Bland, M. T. 2013. Predicted crater morphologies on Ceres: Probing internal structure and evolution. Icarus, 226, 510-521.Bland, M. T. and McKinnon, W. B., 2013. Does folding accommodate Europa’s contractional strain? The effect of surface temperature on fold formation in ice lithospheres. Geophys. Res. Lett., 40, 2534-2538, doi:10.1002/grl.50506.Bland, M. T., and McKinnon, W. B., 2012. Forming Europa’s folds: Strain requirements for the production of large-amplitude deformation. Icarus,221, 694-709.Bland, M. T., Singer, K. S., McKinnon, W. B., and Schenk, P. M. 2012. Enceladus’ extreme heat flux as revealed by its relaxed craters. Geo. Res. Lett., 39, L17204, doi:10.1029/2012GL052736.Bland, M. T., McKinnon, W. B., and Showman, A. P., 2010. The effects of strain localization on the formation of Ganymede’s grooved terrain. Icarus, 210, 396-410.Bland, M. T., Showman, A. P., and Tobie, G., 2009. The orbital-thermal evolution and global expansion of Ganymede. Icarus, 200, 207-221.**Disclaimer: The views expressed in Non-USGS publications are those of the author and do not represent the views of the USGS, Department of the Interior, or the U.S. Government.