Michael Bland, Ph.D.
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
Geomorphological evidence for ground ice on dwarf planet Ceres
The vanishing cryovolcanoes of Ceres
The missing large impact craters on Ceres
Composition and structure of the shallow subsurface of Ceres revealed by crater morphology
Mountain building on Io driven by deep faulting
Constraining the heat flux between Enceladus’ tiger stripes: numerical modeling of funiscular plains formation
Forming Ganymede’s grooves at smaller strain: Toward a self-consistent local and global strain history for Ganymede
Non-USGS Publications**
**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
- Publications
Filter Total Items: 31
Geomorphological evidence for ground ice on dwarf planet Ceres
Five decades of observations of Ceres suggest that the dwarf planet has a composition similar to carbonaceous meteorites and may have an ice-rich outer shell protected by a silicate layer. NASA’s Dawn spacecraft has detected ubiquitous clays, carbonates and other products of aqueous alteration across the surface of Ceres, but surprisingly it has directly observed water ice in only a few areas. HerAuthorsBritney E. Schmidt, Kynan H.G. Hughson, Heather T. Chilton, Jennifer E. C. Scully, Thomas Platz, Andreas Nathues, Hanna Sizemore, Michael T. Bland, Shane Byrne, Simone Marchi, David O'Brien, Norbert Schorghofer, Harald Hiesinger, Ralf Jaumann, Jan Hendrick Pasckert, Justin D. Lawrence, Debra Buzckowski, Julie C. Castillo-Rogez, Mark V. Sykes, Paul M. Schenk, Maria-Cristina DeSanctis, Giuseppe Mitri, Michelangelo Formisano, Jian-Yang Li, Vishnu Reddy, Lucille Le Corre, Christopher T. Russell, Carol A. RaymondThe vanishing cryovolcanoes of Ceres
Ahuna Mons is a 4 km tall mountain on Ceres interpreted as a geologically young cryovolcanic dome. Other possible cryovolcanic features are more ambiguous, implying that cryovolcanism is only a recent phenomenon or that other cryovolcanic structures have been modified beyond easy identification. We test the hypothesis that Cerean cryovolcanic domes viscously relax, precluding ancient domes from reAuthorsMichael M. Sori, Shane Byrne, Michael T. Bland, Ali Bramson, Anton Ermakov, Christoper Hamilton, Katharina Otto, Ottaviano Ruesch, Christopher RussellThe missing large impact craters on Ceres
Asteroids provide fundamental clues to the formation and evolution of planetesimals. Collisional models based on the depletion of the primordial main belt of asteroids predict 10–15 craters >400 km should have formed on Ceres, the largest object between Mars and Jupiter, over the last 4.55 Gyr. Likewise, an extrapolation from the asteroid Vesta would require at least 6–7 such basins. However, CereAuthorsS. Marchi, A. Ermakov, C.A. Raymond, R.R. Fu, D.P. O'Brien, Michael T. Bland, E. Ammannito, M.C. De Sanctis, Tim Bowling, P. Schenk, J.E.C. Scully, D.L. Buczkowski, D.A. Williams, H. Hiesinger, C.T. RussellComposition and structure of the shallow subsurface of Ceres revealed by crater morphology
Before NASA’s Dawn mission, the dwarf planet Ceres was widely believed to contain a substantial ice-rich layer below its rocky surface. The existence of such a layer has significant implications for Ceres’s formation, evolution, and astrobiological potential. Ceres is warmer than icy worlds in the outer Solar System and, if its shallow subsurface is ice-rich, large impact craters are expected to bAuthorsMichael T. Bland, Carol A. Raymond, Paul M. Schenk, Roger R. Fu, Thomas Kneisl, Jan Hendrick Pasckert, Harald Hiesinger, Frank Preusker, Ryan S. Park, Simone Marchi, Scott King, Julie C. Castillo-Rogez, Christopher T. RussellMountain building on Io driven by deep faulting
Jupiter’s volcanic moon Io possesses some of the highest relief in the Solar System: massive, isolated mountain blocks that tower up to 17 km above the surrounding plains. These mountains are likely to result from pervasive compressive stresses induced by subsidence of the surface beneath the near-continual emplacement of volcanic material. The stress state that results from subsidence and warmingAuthorsMichael T. Bland, William B. McKinnonConstraining the heat flux between Enceladus’ tiger stripes: numerical modeling of funiscular plains formation
The Cassini spacecraft’s Composite Infrared Spectrometer (CIRS) has observed at least 5 GW of thermal emission at Enceladus’ south pole. The vast majority of this emission is localized on the four long, parallel, evenly-spaced fractures dubbed tiger stripes. However, the thermal emission from regions between the tiger stripes has not been determined. These spatially localized regions have a uniqueAuthorsMichael T. Bland, William B. McKinnon, Paul M. SchenkForming Ganymede’s grooves at smaller strain: Toward a self-consistent local and global strain history for Ganymede
The ubiquity of tectonic features formed in extension, and the apparent absence of ones formed in contraction, has led to the hypothesis that Ganymede has undergone global expansion in its past. Determining the magnitude of such expansion is challenging however, and extrapolation of locally or regionally inferred strains to global scales often results in strain estimates that exceed those based onAuthorsMichael T. Bland, W. B. McKinnonNon-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.