Laszlo Kestay, Ph.D.
Laszlo Kestay is a planetary volcanologist at the US Geological Survey's Astrogeology Science Center.
Laszlo Kestay is a planetary volcanologist working for the US Geological Survey's Astrogeology Science Center. His last name was formerly Keszthelyi and this spelling is still used for his publications. He has worked for the USGS since 1991 but was only hired in 2003. He is member of the NASA MRO HiRISE and ESA ExoMars CaSSIS science teams.
Professional Experience
2003-present, Research Geologist, Astrogeology Science Center, U.S. Geological Survey. Studying volcanism across the Solar System with remote sensing, numerical modeling, and field studies. Involved in assessing natural resources across the Solar System and the hazards posed by meteorite impacts.
2012-2018, Science Center Director, Astrogeology Science Center U.S. Geological Survey. Manage the science center as it enables humankind's exploration of the Solar System with support for space missions from conception to beyond the grave.
2011, Associate Science Center Director for Technical Operations, Astrogeology Science Center, U.S. Geological Survey. Overseeing the technical activities (cartography, software development, computer science, data archival, etc.) in the Astrogeology Science Center.
2004-2007, Assistant Team Chief Scientist
1994-1996, NSF Earth Sciences Postdoctoral Fellow, University of Hawaii at Manoa and U.S. Geological Survey Hawaiian Volcano Observatory. Supervisor: Stephen Self
Education and Certifications
B.S., Mathematics, Summa Cum Laude, 1987, The University of Texas at Austin
B.S. with Honors, Geological Sciences (Geophysics Option), Summa Cum Laude, 1988, The University of Texas at Austin
M.S., Planetary Science, 1993, Caltech
Ph.D., Geology, 1994, Caltech. Thesis: On the Thermal Budget of Pahoehoe Lava Flows, Advisor: Bruce C. Murray
Science and Products
High Resolution Imaging Science Experiment (HiRISE) observations of glacial and periglacial morphologies in the circum-Argyre Planitia highlands, Mars
Ultrahigh resolution topographic mapping of Mars with HiRISE stereo images: Methods and first results
Comparison of flood lavas on Earth and Mars
Mars reconnaissance orbiter's high resolution imaging science experiment (HiRISE)
A closer look at water-related geologic activity on Mars
Geologic mapping of the Amirani-Gish Bar region of Io: Implications for the global geologic mapping of Io
Windy Mars: A dynamic planet as seen by the HiRISE camera
New estimates for Io eruption temperatures: Implications for the interior
Athabasca Valles, Mars: A lava-draped channel system
Initial insights from 2.5D hydraulic modeling of floods in Athabasca Valles, Mars
Flood lavas on Earth, Io and Mars
The heartbeat of the volcano: The discovery of episodic activity at Prometheus on Io
Science and Products
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- Publications
Filter Total Items: 75
High Resolution Imaging Science Experiment (HiRISE) observations of glacial and periglacial morphologies in the circum-Argyre Planitia highlands, Mars
The landscape of the Argyre Planitia and adjoining Charitum and Nereidum Montes in the southern hemisphere of Mars has been heavily modified since formation of the Argyre impact basin. This study examines morphologies in the Argyre region revealed in images acquired by the High Resolution Imaging Science Experiment (HiRISE) camera and discusses the implications for glacial and periglacial processeAuthorsMaria E. Banks, Alfred S. McEwen, Jeffrey S. Kargel, Victor R. Baker, Robert G. Strom, Michael T. Mellon, Virginia C. Gulick, Laszlo P. Keszthelyi, Kenneth E. Herkenhoff, Jon D. Pelletier, Windy L. JaegerUltrahigh resolution topographic mapping of Mars with HiRISE stereo images: Methods and first results
The Mars Reconnaissance Orbiter (MRO) arrived at Mars on 10 March 2006 and began its primary science phase in November. The High Resolution Imaging Science Experiment (HiRISE) on MRO is the largest, most complex camera ever flown to another planet. Plans call for this scanner to image roughly 1% of Mars by area at a pixel scale of 0.3 m during the next Mars year. Among the thousands of images wAuthorsRandolph L. Kirk, Elpitha Howington-Kraus, Mark R. Rosiek, Debbie Cook, Jeffery A. Anderson, Kris J. Becker, Brent A. Archinal, Laszlo P. Keszthelyi, R. King, Alfred S. McEwenComparison of flood lavas on Earth and Mars
Flood lavas, by definition, cover vast areas in great sheets of lava, without the construction of major edifices (e.g., Geikie, 1880; Washington, 1922; Tyrrell, 1937; Self et al., 1997). The flat terrain that flood lavas produce has led to the term “plateau volcanism” to be used as a synonym for flood volcanism. In addition, the classic erosion pattern of flood lavas leaves a series of topographicAuthorsLaszlo P. Keszthelyi, Alfred S. McEwenMars reconnaissance orbiter's high resolution imaging science experiment (HiRISE)
The HiRISE camera features a 0.5 m diameter primary mirror, 12 m effective focal length, and a focal plane system that can acquire images containing up to 28 Gb (gigabits) of data in as little as 6 seconds. HiRISE will provide detailed images (0.25 to 1.3 m/pixel) covering ∼1% of the Martian surface during the 2‐year Primary Science Phase (PSP) beginning November 2006. Most images will include colAuthorsAlfred S. McEwen, Eric M. Eliason, James W. Bergstrom, Nathan T. Bridges, Candice J. Hansen, W. Alan Delamere, John A. Grant, Virginia C. Gulick, Kenneth E. Herkenhoff, Laszlo P. Keszthelyi, Randolph L. Kirk, Michael T. Mellon, Steven W. Squyres, Nicolas Thomas, Catherine M. WeitzA closer look at water-related geologic activity on Mars
Water has supposedly marked the surface of Mars and produced characteristic landforms. To understand the history of water on Mars, we take a close look at key locations with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter, reaching fine spatial scales of 25 to 32 centimeters per pixel. Boulders ranging up to ∼2 meters in diameter are ubiquitous in the middleAuthorsAlfred S. McEwen, C.J. Hansen, W.A. Delamere, E. M. Eliason, Kenneth E. Herkenhoff, Laszlo P. Keszthelyi, V. C. Gulick, Randolph L. Kirk, M. T. Mellon, J. A. Grant, N. Thomas, C.M. Weitz, S. W. Squyres, N.T. Bridges, S.L. Murchie, F. Seelos, K. Seelos, C.H. Okubo, M.P. Milazzo, L.L. Tornabene, W.L. Jaeger, S. Byrne, P.S. Russell, J.L. Griffes, S. Martinez-Alonso, A. Davatzes, F. C. Chuang, B.J. Thomson, K.E. Fishbaugh, C. M. Dundas, K.J. Kolb, M. E. Banks, J.J. WrayGeologic mapping of the Amirani-Gish Bar region of Io: Implications for the global geologic mapping of Io
We produced the first geologic map of the Amirani-Gish Bar region of Io, the last of four regional maps generated from Galileo mission data. The Amirani-Gish Bar region has five primary types of geologic materials: plains, mountains, patera floors, flows, and diffuse deposits. The flows and patera floors are thought to be compositionally similar, but are subdivided based on interpretations regardiAuthorsDavid A. Williams, Laszlo P. Keszthelyi, David A. Crown, Windy L. Jaeger, Paul M. SchenkWindy Mars: A dynamic planet as seen by the HiRISE camera
With a dynamic atmosphere and a large supply of particulate material, the surface of Mars is heavily influenced by wind-driven, or aeolian, processes. The High Resolution Imaging Science Experiment (HiRISE) camera on the Mars Reconnaissance Orbiter (MRO) provides a new view of Martian geology, with the ability to see decimeter-size features. Current sand movement, and evidence for recent bedform dAuthorsNathan T. Bridges, Paul E. Geissler, Alfred S. McEwen, B.J. Thomson, Frank C. Chuang, Kenneth E. Herkenhoff, Laszlo P. Keszthelyi, Sara Martinez-AlonsoNew estimates for Io eruption temperatures: Implications for the interior
The initial interpretation of Galileo data from Jupiter's moon, Io, suggested eruption temperatures ≥1600°C. Tidal heating models have difficulties explaining Io's prodigious heat flow if the mantle is >1300°C, although we suggest that temperatures up to ~1450°C may be possible. In general, Io eruption temperatures have been overestimated because the incorrect thermal model has been applied. MuchAuthorsLaszlo P. Keszthelyi, Windy L. Jaeger, Moses P. Milazzo, Jani Radebaugh, Ashley G. Davies, Karl L. MitchellAthabasca Valles, Mars: A lava-draped channel system
Athabasca Valles is a young outflow channel system on Mars that may have been carved by catastrophic water floods. However, images acquired by the High-Resolution Imaging Science Experiment camera onboard the Mars Reconnaissance Orbiter spacecraft reveal that Athabasca Valles is now entirely draped by a thin layer of solidified lava - the remnant of a once-swollen river of molten rock. The lava erAuthorsWindy L. Jaeger, Laszlo P. Keszthelyi, Alfred S. McEwen, Colin M. Dundas, Paul C. RussellInitial insights from 2.5D hydraulic modeling of floods in Athabasca Valles, Mars
We present the first application of a 2.5D hydraulic model to catastrophic floods on Mars. This model simulates flow over complex topography and incorporates flood dynamics that could not be modeled in the earlier 1D models. We apply this model to Athabasca Valles, the youngest outflow channel on Mars, investigating previous bank-full discharge estimates and utilizing the interpolated Mars OrbiterAuthorsLaszlo P. Keszthelyi, Roger P. Denlinger, D. R. H. O'Connell, Devon M. BurrFlood lavas on Earth, Io and Mars
Flood lavas are major geological features on all the major rocky planetary bodies. They provide important insight into the dynamics and chemistry of the interior of these bodies. On the Earth, they appear to be associated with major and mass extinction events. It is therefore not surprising that there has been significant research on flood lavas in recent years. Initial models suggested eruption dAuthorsLaszlo P. Keszthelyi, Stephen Self, Thorvaldur ThordarsonThe heartbeat of the volcano: The discovery of episodic activity at Prometheus on Io
The temporal signature of thermal emission from a volcano is a valuable clue to the processes taking place both at and beneath the surface. The Galileo Near Infrared Mapping Spectrometer (NIMS) observed the volcano Prometheus, on the jovian moon Io, on multiple occasions between 1996 and 2002. The 5 micron (μm) brightness of this volcano shows considerable variation from orbit to orbit. PrometheusAuthorsAshley G. Davies, Lionel Wilson, Dennis Matson, Giovanni Leone, Laszlo P. Keszthelyi, Windy L. Jaeger - News