Kenneth Edward Herkenhoff, Ph.D. (Former Employee)
Science and Products
Filter Total Items: 149
Ventifacts at the Pathfinder landing site
About half of the rocks at the Mars Pathfinder Ares Vallis landing site appear to be ventifacts, rocks abraded by windborne particles. Comparable resolution images taken by the Imager for Mars Pathfinder (IMP) camera and the Viking landers show that ventifacts are more abundant at the Pathfinder site. The ventifacts occur in several forms, including rocks with faceted edges, finger‐like projection
Authors
N.T. Bridges, R. Greeley, A. F. C. Haldemann, Kenneth E. Herkenhoff, M. Kraft, T. J. Parker, A. W. Ward
Aeolian features and processes at the Mars Pathfinder landing site
The Mars Pathfinder landing site contains abundant features attributed to aeolian, or wind, processes. These include wind tails, drift deposits, duneforms of various types, ripplelike features, and ventifacts (the first clearly seen on Mars). Many of these features are consistant with formation involving sand-size particles. Although some features, such as dunes, could develop from saltating sand-
Authors
Ronald Greeley, Michael Kraft, Robert Sullivan, Gregory Wilson, Nathan Bridges, Kenneth E. Herkenhoff, Ruslan O. Kuzmin, Michael Malin, Wes Ward
Imager for Mars Pathfinder (IMP) image calibration
The Imager for Mars Pathfinder returned over 16,000 high-quality images from the surface of Mars. The camera was well-calibrated in the laboratory, with <5% radiometric uncertainty. The photometric properties of two radiometric targets were also measured with 3% uncertainty. Several data sets acquired during the cruise and on Mars confirm that the system operated nominally throughout the course of
Authors
R.J. Reid, P. H. Smith, M. Lemmon, R. Tanner, M. Burkland, E. Wegryn, J. Weinberg, R. Marcialis, D.T. Britt, N. Thomas, R. Kramm, A. Dummel, D. Crowe, B.J. Bos, J.F. Bell, P. Rueffer, F. Gliem, J. R. Johnson, J.N. Maki, Kenneth E. Herkenhoff, Robert B. Singer
Results from the Mars Pathfinder camera
Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the pr
Authors
P. H. Smith, J. F. III Bell, N. T. Bridges, D.T. Britt, Lisa R. Gaddis, R. Greeley, H.U. Keller, Kenneth E. Herkenhoff, R. Jaumann, J. R. Johnson, Randolph L. Kirk, M. Lemmon, J.N. Maki, M.C. Malin, S.L. Murchie, J. Oberst, T. J. Parker, R.J. Reid, R.M. Sablotny, Laurence A. Soderblom, C. Stoker, R. Sullivan, N. Thomas, M.G. Tomasko, W. Ward, E. Wegryn
Structure and kinematics of a complex impact crater, Upheaval Dome, southeast Utah
Two vastly different phenomena, impact and salt diapirism, have been proposed for the origin of Upheaval Dome, southeast Utah. Detailed geologic mapping, seismic refraction data, and the presence of shock metamorphosed rocks indicate that the dome originated by collapse of a transient cavity formed by impact. Evidence is: (1) the occurrence of a lag deposit of rare impactites, (2) fan-tailed fract
Authors
Bryan J. Kriens, Eugene Merle Shoemaker, Kenneth E. Herkenhoff
Science and Products
Filter Total Items: 149
Ventifacts at the Pathfinder landing site
About half of the rocks at the Mars Pathfinder Ares Vallis landing site appear to be ventifacts, rocks abraded by windborne particles. Comparable resolution images taken by the Imager for Mars Pathfinder (IMP) camera and the Viking landers show that ventifacts are more abundant at the Pathfinder site. The ventifacts occur in several forms, including rocks with faceted edges, finger‐like projection
Authors
N.T. Bridges, R. Greeley, A. F. C. Haldemann, Kenneth E. Herkenhoff, M. Kraft, T. J. Parker, A. W. Ward
Aeolian features and processes at the Mars Pathfinder landing site
The Mars Pathfinder landing site contains abundant features attributed to aeolian, or wind, processes. These include wind tails, drift deposits, duneforms of various types, ripplelike features, and ventifacts (the first clearly seen on Mars). Many of these features are consistant with formation involving sand-size particles. Although some features, such as dunes, could develop from saltating sand-
Authors
Ronald Greeley, Michael Kraft, Robert Sullivan, Gregory Wilson, Nathan Bridges, Kenneth E. Herkenhoff, Ruslan O. Kuzmin, Michael Malin, Wes Ward
Imager for Mars Pathfinder (IMP) image calibration
The Imager for Mars Pathfinder returned over 16,000 high-quality images from the surface of Mars. The camera was well-calibrated in the laboratory, with <5% radiometric uncertainty. The photometric properties of two radiometric targets were also measured with 3% uncertainty. Several data sets acquired during the cruise and on Mars confirm that the system operated nominally throughout the course of
Authors
R.J. Reid, P. H. Smith, M. Lemmon, R. Tanner, M. Burkland, E. Wegryn, J. Weinberg, R. Marcialis, D.T. Britt, N. Thomas, R. Kramm, A. Dummel, D. Crowe, B.J. Bos, J.F. Bell, P. Rueffer, F. Gliem, J. R. Johnson, J.N. Maki, Kenneth E. Herkenhoff, Robert B. Singer
Results from the Mars Pathfinder camera
Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the pr
Authors
P. H. Smith, J. F. III Bell, N. T. Bridges, D.T. Britt, Lisa R. Gaddis, R. Greeley, H.U. Keller, Kenneth E. Herkenhoff, R. Jaumann, J. R. Johnson, Randolph L. Kirk, M. Lemmon, J.N. Maki, M.C. Malin, S.L. Murchie, J. Oberst, T. J. Parker, R.J. Reid, R.M. Sablotny, Laurence A. Soderblom, C. Stoker, R. Sullivan, N. Thomas, M.G. Tomasko, W. Ward, E. Wegryn
Structure and kinematics of a complex impact crater, Upheaval Dome, southeast Utah
Two vastly different phenomena, impact and salt diapirism, have been proposed for the origin of Upheaval Dome, southeast Utah. Detailed geologic mapping, seismic refraction data, and the presence of shock metamorphosed rocks indicate that the dome originated by collapse of a transient cavity formed by impact. Evidence is: (1) the occurrence of a lag deposit of rare impactites, (2) fan-tailed fract
Authors
Bryan J. Kriens, Eugene Merle Shoemaker, Kenneth E. Herkenhoff