Laurence Soderblom, PhD (Former Employee)
Science and Products
Filter Total Items: 137
Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars
Outcrop exposures of sedimentary rocks at the Opportunity landing site (Meridiani Planum) form a set of genetically related strata defined here informally as the Burns formation. This formation can be subdivided into lower, middle, and upper units which, respectively, represent eolian dune, eolian sand sheet, and mixed eolian sand sheet and interdune facies associations. Collectively...
Authors
J. Grotzinger, R. E. Arvidson, J. Bell, W. Calvin, B.C. Clark, D.A. Fike, M. Golombek, R. Greeley, A. Haldemann, Kenneth Herkenhoff, B. Jolliff, A. Knoll, M. Malin, S. McLennan, T. Parker, Laurence Soderblom, J. Sohl-Dickstein, S. Squyres, N.J. Tosca, W.A. Watters
Initial results of rover localization and topographic mapping for the 2003 mars exploration rover mission Initial results of rover localization and topographic mapping for the 2003 mars exploration rover mission
This paper presents the initial results of lander and rover localization and topographic mapping of the MER 2003 mission (by Sol 225 for Spirit and Sol 206 for Opportunity). The Spirit rover has traversed a distance of 3.2 km (actual distance traveled instead of odometry) and Opportunity at 1.2 km. We localized the landers in the Gusev Crater and on the Meridiani Planum using two-way...
Authors
Rongxing Li, Steven Squyres, Raymond Arvidson, Brent Archinal, James F. Bell, Yang Cheng, Larry Crumpler, David Des Marais, Kaichang Di, Todd Ely, Matthew Golombek, Eric Graat, John Grant, Joe Guinn, Andrew Johnson, Ronald Greeley, Randolph Kirk, Mark Maimone, Laurence Soderblom, Shane Thompson, Jue Wang, Patrick Whelley, Fengliang Xu
Joint analysis of visible and infrared images Joint analysis of visible and infrared images
Analysis of data combining daytime visible reflected, daytime IR emitted, and nighttime IR emitted images allows us to isolate the physical effects of topography, albedo, and thermal inertia. To a good approximation, these physical influences interact linearly so that maps showing topographic shading, albedo, and relative thermal inertia can be produced by simple algebraic manipulation...
Authors
Randolph Kirk, Laurence Soderblom, Glen Cushing, Timothy Tituus
Cassini radar views the surface of Titan Cassini radar views the surface of Titan
The Cassini Titan Radar Mapper imaged about 1% of Titan's surface at a resolution of ∼0.5 kilometer, and larger areas of the globe in lower resolution modes. The images reveal a complex surface, with areas of low relief and a variety of geologic features suggestive of dome-like volcanic constructs, flows, and sinuous channels. The surface appears to be young, with few impact craters...
Authors
C. Elachi, S. Wall, M. Allison, Y. Anderson, R. Boehmer, P. Callahan, P. Encrenaz, E. Flamini, G. Franceschetti, Y. Gim, G. Hamilton, S. Hensley, M. Janssen, W. Johnson, K. Kelleher, Randolph Kirk, R. Lopes, R. Lorenz, J. Lunine, D. Muhleman, S. Ostro, F. Paganelli, G. Picardi, F. Posa, L. Roth, R. Seu, S. Shaffer, Laurence Soderblom, B. Stiles, E. Stofan, S. Vetrella, R. West, C. Wood, L. Wye, H. Zebker
Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan
Titan is the only satellite in our Solar System with a dense atmosphere. The surface pressure is 1.5 bar (ref. 1) and, similar to the Earth, N 2 is the main component of the atmosphere. Methane is the second most important component, but it is photodissociated on a timescale of 10 years (ref. 3). This short timescale has led to the suggestion that Titan may possess a surface or...
Authors
Christophe Sotin, R. Jaumann, B. Buratti, R. Brown, R. Clark, L.A. Soderblom, K. Baines, G. Bellucci, J.-P. Bibring, F. Capaccioni, P. Cerroni, M. Combes, A. Coradini, D. Cruikshank, P. Drossart, V. Formisano, Y. Langevin, D. Matson, T. McCord, R.M. Nelson, P. Nicholson, B. Sicardy, S. Lemouelic, S. Rodriguez, K. Stephan, C.K. Scholz
The evolution of Titan's mid-latitude clouds The evolution of Titan's mid-latitude clouds
Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal that the horizontal structure, height, and optical depth of Titan's clouds are highly, dynamic. Vigorous cloud centers are seen to rise from the middle to the upper troposphere within 30 minutes and dissipate within the next hour. Their development indicates that Titan's clouds evolve convectively; dissipate through...
Authors
C.A. Griffith, P. Penteado, K. Baines, P. Drossart, J. Barnes, G. Bellucci, J. Bibring, R. Brown, B. Buratti, F. Capaccioni, P. Cerroni, R. Clark, M. Combes, A. Coradini, D. Cruikshank, V. Formisano, R. Jaumann, Y. Langevin, D. Matson, T. McCord, V. Mennella, R. Nelson, P. Nicholson, B. Sicardy, Christophe Sotin, L.A. Soderblom, R. Kursinski
Science and Products
Filter Total Items: 137
Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars Stratigraphy and sedimentology of a dry to wet eolian depositional system, Burns formation, Meridiani Planum, Mars
Outcrop exposures of sedimentary rocks at the Opportunity landing site (Meridiani Planum) form a set of genetically related strata defined here informally as the Burns formation. This formation can be subdivided into lower, middle, and upper units which, respectively, represent eolian dune, eolian sand sheet, and mixed eolian sand sheet and interdune facies associations. Collectively...
Authors
J. Grotzinger, R. E. Arvidson, J. Bell, W. Calvin, B.C. Clark, D.A. Fike, M. Golombek, R. Greeley, A. Haldemann, Kenneth Herkenhoff, B. Jolliff, A. Knoll, M. Malin, S. McLennan, T. Parker, Laurence Soderblom, J. Sohl-Dickstein, S. Squyres, N.J. Tosca, W.A. Watters
Initial results of rover localization and topographic mapping for the 2003 mars exploration rover mission Initial results of rover localization and topographic mapping for the 2003 mars exploration rover mission
This paper presents the initial results of lander and rover localization and topographic mapping of the MER 2003 mission (by Sol 225 for Spirit and Sol 206 for Opportunity). The Spirit rover has traversed a distance of 3.2 km (actual distance traveled instead of odometry) and Opportunity at 1.2 km. We localized the landers in the Gusev Crater and on the Meridiani Planum using two-way...
Authors
Rongxing Li, Steven Squyres, Raymond Arvidson, Brent Archinal, James F. Bell, Yang Cheng, Larry Crumpler, David Des Marais, Kaichang Di, Todd Ely, Matthew Golombek, Eric Graat, John Grant, Joe Guinn, Andrew Johnson, Ronald Greeley, Randolph Kirk, Mark Maimone, Laurence Soderblom, Shane Thompson, Jue Wang, Patrick Whelley, Fengliang Xu
Joint analysis of visible and infrared images Joint analysis of visible and infrared images
Analysis of data combining daytime visible reflected, daytime IR emitted, and nighttime IR emitted images allows us to isolate the physical effects of topography, albedo, and thermal inertia. To a good approximation, these physical influences interact linearly so that maps showing topographic shading, albedo, and relative thermal inertia can be produced by simple algebraic manipulation...
Authors
Randolph Kirk, Laurence Soderblom, Glen Cushing, Timothy Tituus
Cassini radar views the surface of Titan Cassini radar views the surface of Titan
The Cassini Titan Radar Mapper imaged about 1% of Titan's surface at a resolution of ∼0.5 kilometer, and larger areas of the globe in lower resolution modes. The images reveal a complex surface, with areas of low relief and a variety of geologic features suggestive of dome-like volcanic constructs, flows, and sinuous channels. The surface appears to be young, with few impact craters...
Authors
C. Elachi, S. Wall, M. Allison, Y. Anderson, R. Boehmer, P. Callahan, P. Encrenaz, E. Flamini, G. Franceschetti, Y. Gim, G. Hamilton, S. Hensley, M. Janssen, W. Johnson, K. Kelleher, Randolph Kirk, R. Lopes, R. Lorenz, J. Lunine, D. Muhleman, S. Ostro, F. Paganelli, G. Picardi, F. Posa, L. Roth, R. Seu, S. Shaffer, Laurence Soderblom, B. Stiles, E. Stofan, S. Vetrella, R. West, C. Wood, L. Wye, H. Zebker
Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan Release of volatiles from a possible cryovolcano from near-infrared imaging of Titan
Titan is the only satellite in our Solar System with a dense atmosphere. The surface pressure is 1.5 bar (ref. 1) and, similar to the Earth, N 2 is the main component of the atmosphere. Methane is the second most important component, but it is photodissociated on a timescale of 10 years (ref. 3). This short timescale has led to the suggestion that Titan may possess a surface or...
Authors
Christophe Sotin, R. Jaumann, B. Buratti, R. Brown, R. Clark, L.A. Soderblom, K. Baines, G. Bellucci, J.-P. Bibring, F. Capaccioni, P. Cerroni, M. Combes, A. Coradini, D. Cruikshank, P. Drossart, V. Formisano, Y. Langevin, D. Matson, T. McCord, R.M. Nelson, P. Nicholson, B. Sicardy, S. Lemouelic, S. Rodriguez, K. Stephan, C.K. Scholz
The evolution of Titan's mid-latitude clouds The evolution of Titan's mid-latitude clouds
Spectra from Cassini's Visual and Infrared Mapping Spectrometer reveal that the horizontal structure, height, and optical depth of Titan's clouds are highly, dynamic. Vigorous cloud centers are seen to rise from the middle to the upper troposphere within 30 minutes and dissipate within the next hour. Their development indicates that Titan's clouds evolve convectively; dissipate through...
Authors
C.A. Griffith, P. Penteado, K. Baines, P. Drossart, J. Barnes, G. Bellucci, J. Bibring, R. Brown, B. Buratti, F. Capaccioni, P. Cerroni, R. Clark, M. Combes, A. Coradini, D. Cruikshank, V. Formisano, R. Jaumann, Y. Langevin, D. Matson, T. McCord, V. Mennella, R. Nelson, P. Nicholson, B. Sicardy, Christophe Sotin, L.A. Soderblom, R. Kursinski