Research


Current Research

Bennu

Global Geologic Mapping and Sample Site Selection

NASA's Origins, Spectral Interpretation, Resource Identification, Security, Regolith Explorer (OSIRIS-REx) spacecraft is traveling to the carbonaceous asteroid 101955 Bennu to determine its physical and chemical properties, and will return a sample of the asteroid to Earth. I am supporting the team as part of the Regolith Development Working Group, where I am helping to assess the sampleability of Bennu by looking for locations that can be safely and efficiently sampled. Stay tuned for more details on Bennu as the mission progresses!

For more information about Bennu, how we're going to grab a sample of the surface, and details about the mission, check out the mission website

^Back to Top


Mars

Martian deglaciation as an indicator of climatic variability

 (Left) Glaciated crater on Mars that contains evidence of paraglacial modification. Glaciation is evident from the presence of concentric crater fill (CCF), while the stratigraphically younger features are evidence of paraglacial modification.  (Right) Sketch map of the paraglacial features in the glaciated crater to the left.

(Left) Glaciated crater on Mars that contains evidence of paraglacial modification. Glaciation is evident from the presence of concentric crater fill (CCF), while the stratigraphically younger features are evidence of paraglacial modification.

(Right) Sketch map of the paraglacial features in the glaciated crater to the left.

Figure2.jpg

Mars contains abundant evidence of glaciation at virtually all latitudes, but the highest concentration of glacial features are present in the mid-latitudes (~30-60°). Inside many glaciated craters, young geologic features indicate deglaciation and subsequent modification, indicating paraglacial modification (which describes how an environment responds deglaciation-induced instabilities). Through assessing the characteristics and relative ages of these paraglacial features compared to remnant glacial deposits within the craters, it is possible to better constrain global climate cycles on Mars. 

Check out the full version of the 2018 paper here, or click here to download a PDF. 

Co-authors on this work: James W. Head and David R. Marchant

 Global distribution of paraglacial features in glaciated crater interiors. 

Global distribution of paraglacial features in glaciated crater interiors. 

Evidence of this paraglacial activity is present at virtually all longitudes on Mars in the mid-latitudes of both hemispheres, but the distribution and association of paraglacial features is not constant, as can be seen in the figure above. The distribution of paraglacial features appear to be dependent on local geologic setting as well as regional accumulation and ablation patterns. See this LPSC abstract for more information.

Recently glaciated terrains on Mars represent important human exploration destinations as they contain abundant deposits of near-surface ice. This ice could be extracted and utilized by humans, cutting down on consumable resources transported from Earth. The wide distribution of glaciated terrains at a variety of latitudes provide abundant exploration targets.

^ Back to top


Moon

Characterizing endmember volcanism on the Moon

 (Left) Apollo 15 Mapping Camera image (A15-M-2610) of the Aristarchus plateau. Note the large, fresh Aristarchus crater, as well as the sinuous rille Vallis Schroteri. The entire uplifted, hummocky plateau has been mantled by pyroclastic materials.  (Right) Topography of the Cobra Head region of the plateau. All of the major volcanic features on the plateau (Cobra Head, Vallis Schroteri, the pyroclastic deposit, and the irregular cones) may have been formed from an eruptive vent located at Cobra Head. 

(Left) Apollo 15 Mapping Camera image (A15-M-2610) of the Aristarchus plateau. Note the large, fresh Aristarchus crater, as well as the sinuous rille Vallis Schroteri. The entire uplifted, hummocky plateau has been mantled by pyroclastic materials.

(Right) Topography of the Cobra Head region of the plateau. All of the major volcanic features on the plateau (Cobra Head, Vallis Schroteri, the pyroclastic deposit, and the irregular cones) may have been formed from an eruptive vent located at Cobra Head. 

jawin_aristarchus_cobraheadlabeled.PNG

The Aristarchus plateau is widely agreed to be the most complex volcanic region on the Moon: the plateau contains both the largest pyroclastic deposit and the widest and deepest sinuous rille, and is surrounded by some of the Moon's youngest mare basalts. While the complex stratigraphy and diversity of volcanic features in the region may have formed through smaller eruptions spread across the plateau, evidence of large irregular cone-like features just south of Cobra Head suggest that the major volcanic features could have formed through a single, continuous fire-fountain eruption. The morphology and physical characteristics of these irregular spatter cone-like features could explain the presence of a pyroclastic deposit and the sinuous rille, and the location and distribution of these features can be used to infer conditions about the volcanic eruption. This emplacement model is currently being tested by assessing the regional morphologic and morphometric properties of the plateau, as well as performing non-linear spectral unmixing of Moon Mineralogy Mapper (M3) spectral data of the pyroclastic deposit. For more information see this LPSC abstract about the eruption model and this one about spectral modeling.

The Aristarchus plateau represents one of the most promising future exploration destinations on the Moon. The large pyroclastic deposit may have a high concentration of trapped volatiles, which is scientifically critical to understand the lunar volatile inventory and also provides abundant opportunity for in situ resource utilization (ISRU). In addition,  the geologic diversity of the plateau allows access to sites of diverse volcanism (explosive/effusive; mafic/silicic), as well as a fresh, well-preserved impact structure in Aristarchus crater. This site is included in the list of high-priority landing sites in the Lunar Science for Landed Missions Workshop Report.

^ Back to top


Past Research


Examining spectral variations of localized lunar pyroclastic deposits

 Alphonsus crater. (A) Sketch map with a Kaguya TC evening mosaic as the basemap. (B) M3 1 μm albedo map. DMDs appear dark, and specific subdeposits studied here are labeled. (C) RGB color composite image using R: IBD 1000 nm, G: BD 1900 nm, and B: R 1580 nm. (D) RGB color composite image using R: BD 950 nm, G: BD 1050 nm, and B: BD 1250 nm. Spectra of mare basalts and crater floor used in right image (D) are identified here.

Alphonsus crater. (A) Sketch map with a Kaguya TC evening mosaic as the basemap. (B) M3 1 μm albedo map. DMDs appear dark, and specific subdeposits studied here are labeled. (C) RGB color composite image using R: IBD 1000 nm, G: BD 1900 nm, and B: R 1580 nm. (D) RGB color composite image using R: BD 950 nm, G: BD 1050 nm, and B: BD 1250 nm. Spectra of mare basalts and crater floor used in right image (D) are identified here.

 Spectra of Alphonsus crater DMDs. (A) Absolute reflectance. Black dashed lines indicate the endpoints used to calculate the continuum. Inset image shows the study areas of each spectral unit (i.e., light, intermediate, dark, and vent) in the western subdeposit. Outline colors correspond to the colors in the spectra. White dashed lines are the approximate outline of the volcanic vents, while the spectral regions outlined in red are the portions used in the analysis. (B) Spectra from (A) with continuum removal applied. (C) The continuum-removed spectra of the W, SE, and NE subdeposits in Alphonsus crater. The colors for the spectra are maintained from (A) and (B). (D) Continuum-removed spectra of SE deposit, as well as spectra from the floor of Alphonsus crater and two basalts from eastern Mare Nubium; see left image (D).

Spectra of Alphonsus crater DMDs. (A) Absolute reflectance. Black dashed lines indicate the endpoints used to calculate the continuum. Inset image shows the study areas of each spectral unit (i.e., light, intermediate, dark, and vent) in the western subdeposit. Outline colors correspond to the colors in the spectra. White dashed lines are the approximate outline of the volcanic vents, while the spectral regions outlined in red are the portions used in the analysis. (B) Spectra from (A) with continuum removal applied. (C) The continuum-removed spectra of the W, SE, and NE subdeposits in Alphonsus crater. The colors for the spectra are maintained from (A) and (B). (D) Continuum-removed spectra of SE deposit, as well as spectra from the floor of Alphonsus crater and two basalts from eastern Mare Nubium; see left image (D).

The localized lunar dark mantle deposits (DMDs) in Alphonsus, J. Herschel, and Oppenheimer craters were analyzed using visible-near-infrared spectroscopy data from the Moon Mineralogy Mapper (M3). Spectra of these localized DMDs were analyzed for compositional and mineralogical variations within the deposits and were compared with nearby mare basalt units. Spectra of the three localized DMDs exhibited mafic absorption features indicating iron-rich compositions, although the DMDs were spectrally distinct from nearby mare basalts. All of the DMDs contained spectral signatures of glassy materials, suggesting the presence of volcanic glass in varying concentrations across the individual deposits. In addition, the albedo and spectral signatures were variable within the Alphonsus and Oppenheimer crater DMDs, suggesting variable deposit thickness and/or variations in the amount of mixing with the local substrate. Two previously unidentified localized DMDs were discovered to the northeast of Oppenheimer crater. The identification of high concentrations of volcanic glass in multiple localized DMDs in different locations suggests that the distribution of volcanic glass across the lunar surface is much more widespread than has been previously documented. The presence of volcanic glass implies an explosive, vulcanian eruption style for localized DMDs, as this allows volcanic glass to rapidly quench, inhibiting crystallization, compared to the larger hawaiian-style eruptions typical of regional DMD emplacement where black beads indicate a higher degree of crystallization. Improved understanding of the local and global distributions of volcanic glass in lunar DMDs will further constrain lunar degassing and compositional evolution throughout lunar volcanic history.

Check out full version of the 2015 paper here, or click here to download a PDF.

Co-authors on this work: Sebastien Besse, Lisa R. Gaddis, Jessica M. Sunshine, James W. Head, and Sara Mazrouei


The relationship between radar scattering and surface roughness of lunar volcanic features

 (Left) Relationships between surface roughness measured using various techniques, including P- and S-band radar circular polarization ratio (CPR) data, and LOLA-derived Topographic Planar Offset (TPO), for a variety of lunar geologic targets, primarily including volcanic features.  (Right) LOLA hillshade map of the four volcanic dome units analyzed in this work., among other volcanic features

(Left) Relationships between surface roughness measured using various techniques, including P- and S-band radar circular polarization ratio (CPR) data, and LOLA-derived Topographic Planar Offset (TPO), for a variety of lunar geologic targets, primarily including volcanic features.

(Right) LOLA hillshade map of the four volcanic dome units analyzed in this work., among other volcanic features

Lunar roughness measurements derived from the Lunar Orbiter Laser Altimeter (LOLA) are compared to 12.6 cm wavelength radar data (S-band) collected by the Miniature Radio Frequency instrument and 70 cm wavelength radar data (P-band) collected by the Arecibo Observatory. These data are compared to assess how surface and subsurface roughness are correlated and affected by parameters including age and composition at length scales between 0.1-100 m. A range of features are analyzed including volcanic domes (Marius Hills, Rümker Hills, Gruithuisen, and Mairan Domes); mare (Imbrium, Serenitatis, and Oceanus Procellarum); pyroclastic dark mantle deposits (Sinus Aestuum, Sulpicius Gallus, and Mare Vaporum); and two young craters (Copernicus and Tycho). Statistically significant positive correlations exist between topographic roughness and both P- and S-band circular polarization ratios. The strongest correlation is observed at the longest length scales. Correlations weaken as length scales become less similar, potentially due to distinct processes controlling surface modification. Roughness is not significantly correlated with local slope. Although the Marius Hills are compositionally distinct from the Gruithuisen and Mairan domes, they are indistinguishable in roughness characteristics. Conversely, the Rümker Hills, mare, and dark mantle deposits are smoother at the length scales examined, possibly due to fine-grained mantling of regolith or pyroclastic deposits. The floor and ejecta of Tycho crater are the roughest surfaces measured in this study, while the floor and ejecta of Copernicus crater overlap the roughness distribution of the volcanic features. This study shows that many factors control the evolution of roughness over time on various length scales.

Check out the full version of the 2014 paper here, or click here to download a PDF. 

Co-authors on this work: Walter S. Kiefer, Caleb I. Fassett, D. Benjamin J. Bussey, Joshua T. S. Cahill, M. Darby Dyar, Samuel J. Lawrence, and Paul D. Spudis

^ Back to top