Randolph L Kirk, Ph.D.
Randolph Kirk’s research interests span both geoscience and mapping of planetary bodies. He has participated in many missions to the Moon, Venus, Mars, asteroids, comets, and icy satellites. He helped direct planetary mapping at the USGS since the early 1990s, and has developed practical methods for topomapping by shape from shading and by adapting commercial stereo workstations to planetary use.
Recent Accomplishments
- In 2020, NASA's Mars 2020 rover Perseverance landed in Jezero crater at a site mapped by the Astrogeology Science Center. Perseverence was the ninth Mars lander or rover to go to a site we mapped, all of which landed successfully. (Starting in 1962, 10 Mars landings attempted without USGS mapping failed for a variety of reasons. Just days before Perseverence the Chinese landerTianwen-1 became the first such mission to succeed.) Perseverance also carried our maps onboard and used them to guide its final descent, a technological first.
- We are helping to design and caibrate the Europa Imaging System (EIS) cameras for NASA's Europa Clipper mission and to develop software and procedures for making controlled image and topographic maps. As part of this task, we invented and demonstrated a new technique for correcting distortions in frame images that are read out line-by-line so that they can be used for precision mapping.
- We have used stereo images of Mars obtained by different cameras with pixel scales differing up to 50x to assess the resolution and precision of digital topographic models obtained under real-world (Mars) conditions. We are currently using similar techniques with images of Earth’s Moon to quantify how topographic models can be improved by photoclinometry (shape from shading) techniques using one or multiple images.
Education
- Ph.D., Planetary Science, Minor in Physics, California Institute of Technology, January 1987
- M.S., Planetary Science, California Institute of Technology, June 1984
- B.S., Physics, Stanford University, June 1981
Space Mission Participation
- Member, Europa Imaging System Science Team, May 2015–Present
- Member, ExoMars Trace Gas Orbiter CaSSIS Science Team, August 2010–Present
- Member, LRO and Chandrayaan-1 Mini-RF Science Teams, July 2006–Present
- Member, Mars Reconnaissance Orbiter HiRISE Science Team, December 2001–Present
- Member, Mars Exploration Rovers Science Team, August 2000–June 2018
- Associate, Deep Space 1 MICAS Science Team, March 2000–December 2002
- Participating Scientist, NEAR MSI/NIS Team, August 1999–July 2001
- Associate, Imager for Mars Pathfinder Science Team, July 1996–August 1998
- Member, Mars Express HRSC Science Team, January 2000–March 2020
- Associate, Mars 96 HRSC/WAOSS Science Team, March 1993–December 1996
- Member, Cassini RADAR Instrument Team, December 1990–September 2018
- Magellan Guest Investigator, October 1990–September 1994
- Associate, Voyager Imaging Science Team, 1989
Working Groups
- Member, IAU Working Group on Cartographic Coords & Rotational Elements, August 2012–present
- Member, NASA Lunar Geodesy/Cartography Working Group, December 2007–present
- Member, NASA Mars Geodesy/Cartography Working Group, June 1998–present
- Member, ISPRS Working Group “Planetary Mapping & Remote Sensing”, November 1996–present
- Chair, November 2000-October 2004, Co-Chair, Nove
Science and Products
Filter Total Items: 165
Data base of impact craters on Venus based on analysis of Magellan radar images and altimetry data Data base of impact craters on Venus based on analysis of Magellan radar images and altimetry data
No abstract available.
Authors
Gerald Schaber, Randolph Kirk, Robert Strom
Reply to comment on the global resurfacing of Venus Reply to comment on the global resurfacing of Venus
No abstract available.
Authors
R.G. Strom, G. Schaber, D.D. Dawson, Randolph Kirk
Geology of Triton Geology of Triton
Triton, with a diameter of ≡2700 km, is Neptune's only planet-class satellite. The complexity of Triton's surface and the variety of surface features is unequaled among the satellites of the solar system. From a geologic viewpoint, some of Triton's features have apparently familiar morphologies and general interpretative agreement exists. However, many of its landforms have novel...
Authors
S.K. Croft, J.S. Kargel, Randolph Kirk, J. Moore, P.M. Schenk, R.G. Strom
Triton's plumes: Discovery, characteristics, and models Triton's plumes: Discovery, characteristics, and models
This chapter presents (1) basic observations and characteristics of Triton's plumes (scale, geometry, optical properties, and temporal behavior); (2) the current best estimates of other parameters that can be derived directly or inferred from the observations (plume duration, wind velocities, particle properties, mass fluxes, energy requirements, and total erupted mass); and (3) a...
Authors
Randolph Kirk, Laurence Soderblom, R. Brown, S. Kieffer, J.S. Kargel
Venus cartography Venus cartography
The entire surface of the planet Venus is being mapped at global and regional scales (1:50,000,000 through 1:1,500,000) with synthetic aperture radar (SAR), radar altimeter, and radiometer measurements of physical properties from the Magellan spacecraft. The mapping includes SAR image mosaics, shaded relief maps, and topographic contour overlays made from altimetry data and by...
Authors
R. Batson, Randolph Kirk, Kathleen Edwards, H.F. Morgan
Coupling of volatile transport and internal heat flow on Triton Coupling of volatile transport and internal heat flow on Triton
Recently Brown et al. (1991) showed that Triton's internal heat source could amount to 5–20% of the absorbed insolation on Triton, thus significantly affecting volatile transport and atmospheric pressure. Subsequently, Kirk and Brown (1991a) used simple analytical models of the effect of internal heat on the distribution of volatiles on Triton's surface, confirming the speculation of...
Authors
Robert Brown, Randolph Kirk
The Geology of Gaspra The Geology of Gaspra
The surface of Gaspra can be divided into several facets separated by ridges. Superimposed on the facets and ridges are two populations of craters. Type 1 craters are crisply defined and constitute a production function of impact origin. Type 2 craters are mostly irregular shallow depressions and probably of various origins. Some of the type 2 craters may have formed by impact and be...
Authors
M. Carr, Randolph Kirk, A. McEwen, J. Veverka, P. Thomas, J.W. Head, S. Murchie
Galileo Photometry of Asteroid 951 Gaspra Galileo Photometry of Asteroid 951 Gaspra
Galileo images of Gaspra make it possible for the first time to determine a main-belt asteroid's photometric properties accurately by providing surface-resolved coverage over a wide range of incidence and emission angles and by extending the phase angle coverage to phases not observable from Earth. We combine Earth-based telescopic photometry over phase angles 2° ≤ α ≤ 25° with Galileo...
Authors
P. Helfenstein, J. Veverka, P.C. Thomas, D.P. Simonelli, P. Lee, K. Klaasen, T. Johnson, H. Breneman, J.W. Head, S. Murchie, F. Fanale, M. Robinson, B. Clark, J. Granahan, H. Garbeil, A. McEwen, Randolph Kirk, M. Davies, G. Neukum, S. Mottola, R. Wagner, M. Belton, C. Chapman, C. Pilcher
Carbonate-Sulfate Volcanism on Venus? Carbonate-Sulfate Volcanism on Venus?
Venusian canali, outflow channels, and associated volcanic deposits resemble fluvial landforms more than they resemble volcanic features on Earth and Mars. Some canali have meandering habits and features indicative of channel migration that are very similar to meandering river channels and flood plains on Earth, venusian outflow channels closely resemble water-carved outflow channels on...
Authors
Jeffrey Kargel, Randolph Kirk, Bruce Fegley, Allan Treiman
Enhanced visualization for the interpretation of Magellan radar data: Supplement to the Magellan special issue Enhanced visualization for the interpretation of Magellan radar data: Supplement to the Magellan special issue
The differences of radar data from more familiar photographic images, coupled with the unique geologic characteristics of Venus's surface, can make interpretation of the standard Magellan data products difficult for both planetary scientists and nonspecialists. We describe a set of digital processing techniques for transforming individual remote‐sensing datasets in order to make the...
Authors
Randolph Kirk, Laurence Soderblom, Ella M. Lee
The geology and distribution of impact craters on Venus: What are they telling us? The geology and distribution of impact craters on Venus: What are they telling us?
Magellan has revealed an ensemble of impact craters on Venus that is unique in many important ways. We have compiled a data base describing the 842 craters on 89% of Venus' surface mapped through orbit 2578. (The craters range in diameter from 1.5 to 280 km.) We have studied the distribution, size‐density, morphology, geology, and associated surface properties of these craters both in...
Authors
G. Schaber, R.G. Strom, H. J. Moore, Laurence Soderblom, Randolph Kirk, D.J. Chadwick, D.D. Dawson, Lisa R. Gaddis, J. Boyce, Joel Russell
Subsurface energy storage and transport for solar-powered geysers on Triton Subsurface energy storage and transport for solar-powered geysers on Triton
The location of active geyser-like eruptions and related features close to the current subsolar latitude on Triton suggests a solar energy source for these phenomena. Solidstate greenhouse calculations have shown that sunlight can generate substantially elevated subsurface temperatures. A variety of models for the storage of solar energy in a sub-greenhouse layer and for the supply of...
Authors
Randolph Kirk, Robert Brown, Laurence Soderblom
Science and Products
Filter Total Items: 165
Data base of impact craters on Venus based on analysis of Magellan radar images and altimetry data Data base of impact craters on Venus based on analysis of Magellan radar images and altimetry data
No abstract available.
Authors
Gerald Schaber, Randolph Kirk, Robert Strom
Reply to comment on the global resurfacing of Venus Reply to comment on the global resurfacing of Venus
No abstract available.
Authors
R.G. Strom, G. Schaber, D.D. Dawson, Randolph Kirk
Geology of Triton Geology of Triton
Triton, with a diameter of ≡2700 km, is Neptune's only planet-class satellite. The complexity of Triton's surface and the variety of surface features is unequaled among the satellites of the solar system. From a geologic viewpoint, some of Triton's features have apparently familiar morphologies and general interpretative agreement exists. However, many of its landforms have novel...
Authors
S.K. Croft, J.S. Kargel, Randolph Kirk, J. Moore, P.M. Schenk, R.G. Strom
Triton's plumes: Discovery, characteristics, and models Triton's plumes: Discovery, characteristics, and models
This chapter presents (1) basic observations and characteristics of Triton's plumes (scale, geometry, optical properties, and temporal behavior); (2) the current best estimates of other parameters that can be derived directly or inferred from the observations (plume duration, wind velocities, particle properties, mass fluxes, energy requirements, and total erupted mass); and (3) a...
Authors
Randolph Kirk, Laurence Soderblom, R. Brown, S. Kieffer, J.S. Kargel
Venus cartography Venus cartography
The entire surface of the planet Venus is being mapped at global and regional scales (1:50,000,000 through 1:1,500,000) with synthetic aperture radar (SAR), radar altimeter, and radiometer measurements of physical properties from the Magellan spacecraft. The mapping includes SAR image mosaics, shaded relief maps, and topographic contour overlays made from altimetry data and by...
Authors
R. Batson, Randolph Kirk, Kathleen Edwards, H.F. Morgan
Coupling of volatile transport and internal heat flow on Triton Coupling of volatile transport and internal heat flow on Triton
Recently Brown et al. (1991) showed that Triton's internal heat source could amount to 5–20% of the absorbed insolation on Triton, thus significantly affecting volatile transport and atmospheric pressure. Subsequently, Kirk and Brown (1991a) used simple analytical models of the effect of internal heat on the distribution of volatiles on Triton's surface, confirming the speculation of...
Authors
Robert Brown, Randolph Kirk
The Geology of Gaspra The Geology of Gaspra
The surface of Gaspra can be divided into several facets separated by ridges. Superimposed on the facets and ridges are two populations of craters. Type 1 craters are crisply defined and constitute a production function of impact origin. Type 2 craters are mostly irregular shallow depressions and probably of various origins. Some of the type 2 craters may have formed by impact and be...
Authors
M. Carr, Randolph Kirk, A. McEwen, J. Veverka, P. Thomas, J.W. Head, S. Murchie
Galileo Photometry of Asteroid 951 Gaspra Galileo Photometry of Asteroid 951 Gaspra
Galileo images of Gaspra make it possible for the first time to determine a main-belt asteroid's photometric properties accurately by providing surface-resolved coverage over a wide range of incidence and emission angles and by extending the phase angle coverage to phases not observable from Earth. We combine Earth-based telescopic photometry over phase angles 2° ≤ α ≤ 25° with Galileo...
Authors
P. Helfenstein, J. Veverka, P.C. Thomas, D.P. Simonelli, P. Lee, K. Klaasen, T. Johnson, H. Breneman, J.W. Head, S. Murchie, F. Fanale, M. Robinson, B. Clark, J. Granahan, H. Garbeil, A. McEwen, Randolph Kirk, M. Davies, G. Neukum, S. Mottola, R. Wagner, M. Belton, C. Chapman, C. Pilcher
Carbonate-Sulfate Volcanism on Venus? Carbonate-Sulfate Volcanism on Venus?
Venusian canali, outflow channels, and associated volcanic deposits resemble fluvial landforms more than they resemble volcanic features on Earth and Mars. Some canali have meandering habits and features indicative of channel migration that are very similar to meandering river channels and flood plains on Earth, venusian outflow channels closely resemble water-carved outflow channels on...
Authors
Jeffrey Kargel, Randolph Kirk, Bruce Fegley, Allan Treiman
Enhanced visualization for the interpretation of Magellan radar data: Supplement to the Magellan special issue Enhanced visualization for the interpretation of Magellan radar data: Supplement to the Magellan special issue
The differences of radar data from more familiar photographic images, coupled with the unique geologic characteristics of Venus's surface, can make interpretation of the standard Magellan data products difficult for both planetary scientists and nonspecialists. We describe a set of digital processing techniques for transforming individual remote‐sensing datasets in order to make the...
Authors
Randolph Kirk, Laurence Soderblom, Ella M. Lee
The geology and distribution of impact craters on Venus: What are they telling us? The geology and distribution of impact craters on Venus: What are they telling us?
Magellan has revealed an ensemble of impact craters on Venus that is unique in many important ways. We have compiled a data base describing the 842 craters on 89% of Venus' surface mapped through orbit 2578. (The craters range in diameter from 1.5 to 280 km.) We have studied the distribution, size‐density, morphology, geology, and associated surface properties of these craters both in...
Authors
G. Schaber, R.G. Strom, H. J. Moore, Laurence Soderblom, Randolph Kirk, D.J. Chadwick, D.D. Dawson, Lisa R. Gaddis, J. Boyce, Joel Russell
Subsurface energy storage and transport for solar-powered geysers on Triton Subsurface energy storage and transport for solar-powered geysers on Triton
The location of active geyser-like eruptions and related features close to the current subsolar latitude on Triton suggests a solar energy source for these phenomena. Solidstate greenhouse calculations have shown that sunlight can generate substantially elevated subsurface temperatures. A variety of models for the storage of solar energy in a sub-greenhouse layer and for the supply of...
Authors
Randolph Kirk, Robert Brown, Laurence Soderblom