About

A. Deanne Rogers is a Professor in the Department of Geosciences at Stony Brook University. She holds a B.S. from the College of Charleston (1998), an M.S. from Arizona State University (2001), and a Ph.D. from Arizona State University (2005). She also completed a postdoctoral fellowship at the California Institute of Technology from 2005 to 2007. Since joining Stony Brook University in 2007, she manages the Earth and Planetary Remote Sensing Laboratory within the Stony Brook Center for Planetary Exploration. Professor Rogers' research utilizes remote sensing techniques, statistical methods, laboratory spectroscopy, and thermal modeling to investigate a wide range of planetary surface processes. Her work includes analyzing planetary surfaces such as Mars, with a focus on surface bedrock exposures, mineral compositions, and geological history. She has contributed to understanding the mineralogical and geological evolution of planetary surfaces through her detailed research and publications.

Research topics

• Geology
• Astrobiology
• Physics
• Mineralogy
• Chemistry
• Meteorology
• Geomorphology
• Geophysics
• Statistics
• Mathematics
• Paleontology
• Astronomy
• Geochemistry
• Astrophysics

Selected publications

• The Utility of a Hyperspectral Infrared Imager for Crewed Exploration of Planetary Bodies

  Earth and Space Science · 2025-10-01 · 1 citations

  articleOpen access

  Abstract Planetary analog simulations are a powerful exercise for understanding the utility of deployable instruments, their operational protocols, and the visualization of data products during ExtraVehicular Activities (EVAs). This paper presents results of a field campaign by the NASA Solar System Exploration Research Virtual Institute (SSERVI) Remote, In Situ and Synchrotron Studies for Science and Exploration‐2 (RISE2) team to Kilbourne Hole, New Mexico in March/April 2023 to test the utility of a portable thermal infrared (TIR) hyperspectral imager (HSI) during four EVA simulations. The HSI provides emitted radiance spectra from 7 to 14 μm to map spectral variations likely caused by composition and physical properties, which allows HSI data products to aid in sample selection and site documentation. Four pairs of analog astronauts performed a mock EVA at three stations with field deployable instruments including an HSI. The HSI was found to be a useful tool for performing reconnaissance observations, field site documentation, and sample selection for visibly indistinct materials. From these analog simulations we prioritize two recommendations for use of HSI's in crewed missions. First, HSI‐derived data products should be tailored for the specific science objectives and/or sampling objectives of the mission to expedite interpretation and decision‐making. Second, the HSI instrument would ideally have a wide field‐of‐view/panoramic capability to reduce crew time selecting sites to image. Additionally, pre‐EVA reconnaissance from a remotely operated rover could be conducted with an HSI to collect data prior to disturbance and again post human activity.

  PublisherOA PDFDOI

• Widespread ancient anorthosites in the lower crust of Mars

  Communications Earth & Environment · 2025-11-22 · 3 citations

  articleOpen access

  Understanding when and how evolved rocks formed on terrestrial planets remains a fundamental question in planetary geology. Mars preserves ancient surface rocks, providing unique opportunities to study early crustal formation. Here we report extensive detections of feldspathic, possibly anorthositic, rocks uplifted by the Argyre basin-forming impact using orbital remote sensing. The radial distribution of these feldspathic outcrops indicates they originated from the lower martian crust, positioned stratigraphically between olivine-bearing materials and low-calcium pyroxene-bearing upper crustal rocks. This stratigraphy resembles observations at the Hellas basin, suggesting feldspar-rich rocks are widespread in the lower crust. The spatial association of plagioclase-rich outcrops with pyroxene and olivine-bearing units resembles layered mafic intrusions on Earth, suggesting large-scale melting early in Mars’s history produced differentiated igneous complexes. These observations offer direct evidence to support and refine existing models of early crust formation, addressing key questions regarding crustal properties and formation that have lacked widespread observational constraints. Spectrally feldspathic lithologies, stratigraphically located in the lower crust above olivine-bearing material and below low-Ca pyroxene bearing rocks, are exposed in the Argyre impact basin and observed in data from the Mars Reconnaissance Orbiter.

  PublisherOA PDFDOI

• Mineralogy and Geochemistry of Xenoliths and Phreatomagmatic Deposits in Potrillo Volcanic Field, New Mexico, Determined from Portable Instruments: Applications to Surface Exploration of the Moon and Mars

  The Planetary Science Journal · 2025-10-01

  articleOpen access1st authorCorresponding

  Abstract Instruments that yield information about the mineralogy and chemistry of surface materials will be part of future robotic and human exploration of the Moon and Mars. Accurate interpretation of such data can be informed by coordinated analyses of relevant materials in terrestrial analog terrains. We used a suite of portable instrumentation—visible-to-shortwave infrared (VSWIR) spectroscopy, thermal infrared (TIR) spectroscopy, and X-ray fluorescence—to conduct coordinated mineralogical, geochemical, and visual characterization of a suite of outcrops and loose rocks in Kilbourne Hole and Hunts Hole, New Mexico. A variety of textures, particle sizes, and petrogenetic origins were examined. Data were interpreted using spectral models, spectral library comparisons, and chemical calibration curves and compared to mineralogical information derived from X-ray diffraction. Insights and limitations for each technique are presented in terms of surface type; for example, both the VSWIR and TIR instruments exhibited limitations in discerning the full mineralogy of the fine-grained tuff beds. The diverse suite of xenoliths was apparent in TIR spectral images, and the dominant mineral component was identifiable through linear unmixing of TIR spectra. However, inaccuracies in mineral abundance were also observed, highlighting the need for use of more advanced analysis methods. Known lithological diversity was less apparent in VSWIR spectra, which were dominated by minor amounts of phyllosilicates within or coating the rocks. Finally, based on the dearth of mafic minerals and the abundance of quartz, we infer that the Kilbourne/Hunts tuff beds are dominated by fragments of country rock (“accidentals”) rather than juvenile magmatic materials.

  PublisherDOI

• Remote Determination of Martian Chloride Salt Abundances

  Journal of Geophysical Research Planets · 2025-03-01 · 1 citations

  articleOpen access

  Abstract Chloride salt‐bearing deposits are widely distributed across the southern highlands of Mars. Because chloride salts are highly water‐soluble, these deposits may be representative of the last significant period of stable liquid water at the Martian surface. Therefore, these deposits are key to understanding the fate and evolution of surface waters on Mars. However, little consensus exists about the formation conditions of these deposits, and their origins remain enigmatic. This is due in part because remote spectroscopic detection and quantification of many anhydrous chlorides is hampered by a lack of easily discernible diagnostic absorption features. To address this issue, we present a novel Hapke radiative transfer model‐based method to estimate hydration states and salt abundances of Martian chloride salt‐bearing deposits using visible/near‐infrared (VNIR) reflectance spectra. VNIR laboratory spectra are used to derive water abundances of analog chloride‐bearing materials, establishing an experimental basis for application of these methods to Mars. These methods are then applied to orbital Compact Reconnaissance Imaging Spectrometer for Mars data to create maps of the hydration state and modeled salt abundance of chloride‐bearing deposits. When overlain onto high resolution 3D digital terrain models, these methods produce the highest resolution site‐specific salt abundance maps currently available, enhancing our understanding of chloride deposit geologic context. As an example, deposits in the Terra Sirenum region are observed to have higher estimated salt abundances than previously recognized, exhibiting spatial variations in both abundance and surface morphology.

  PublisherOA PDFDOI

• Ancient Anorthosites on Mars: Widespread in the Lower Crust

  Research Square · 2025-06-17

  preprintOpen access
  PublisherOA PDFDOI

• Databases generated for Manuscript titled "Quantifying downward radiative fluxes from nighttime Martian water ice clouds: Applications to thermal modeling of surface temperatures"

  Zenodo (CERN European Organization for Nuclear Research) · 2024-01-24 · 1 citations

  datasetOpen access

  Databases generated for manuscript "Quantifying downward radiative fluxes from nighttime Martian water ice clouds: Applications to thermal modeling of surface temperatures" There are two zip files containing generated databases: The zip file titled "database.zip" contains generated database for calculated fluxes using the methodology mentioned in the manuscript. The database spans calculated fluxes in one degree bins for latitudes spanning 30° to -10° N and longitudes spanning 0° to 360°. There are 14760 separate .csv files that are for each one by one degree bin. The title of each file contains its coordinates in the format XXXNXXXEtb.csv (e.g. 000N000Etb.csv for 0°N, 0°E). Each .csv file contains four separate columns and variable rows. The columns have headers corresponding to specific values. "ls" corresponds to solar longitude or date based on Mars' orbit around the Sun. "Flux" corresponds to calculated flux based on the methodology presented on the manuscript. "Delta-T" is the difference in temperature comparing modeled temperature compared to Thermal Emission Spectrometer (TES) measured temperature. "Tau" corresponds to calculated Dust visible opacities using the methodology presented in this work. The rows in each file vary based on the temporal observations from TES at each location. The zip file titled "fitdatabase.zip" contains generated database for fitted fluxes using the methodology mentioned in the manuscript. The database spans calculated fluxes in one degree bins for latitudes spanning 30° to -10° N and longitudes spanning 0° to 360°. There are 14760 separate .csv files that are for each one by one degree bin. The title of each file contains its coordinates in the format XXXNXXXEtbf.csv (e.g. 000N000Etbf.csv for 0°N, 0°E). Each .csv file contains six separate columns and three hundred and sixty rows. The columns have headers corresponding to specific values. "ls" corresponds to solar longitude or date based on Mars' orbit around the Sun. "Flux" corresponds to calculated flux based on the methodology presented on the manuscript. "Delta-T" is the difference in temperature comparing modeled temperature compared to measured temperature. The fitting algorithm interpolates points between values in the calculated flux database and applies a rolling mean fit with a window spanning ten degrees in solar longitude centered at each calculated flux point. "FLAG" indicates the amount of points of calculated flux points that exist within the ten degree window centered at each flux point to demonstrate to the user how much data had to be fitted. "From Ls" shows the leftmost edge of the rolling mean fit window. "To Ls" shows the rightmost edge of the rolling mean fit window. The rows in each file correspond to one degree of solar longitude the fitting algorithm was designed to cover each solar longitude bin.

  PublisherDOI

• Estimating modal mineralogy using Raman spectroscopy: Multivariate analysis models and Raman cross-section proxies

  American Mineralogist · 2024-04-26 · 2 citations

  article

  Abstract Raman spectroscopy is a powerful technique in the context of planetary exploration because it provides information on mineral identification, chemistry, and abundance. For Raman spectrometers with large spot sizes, multiple mineral phases can be investigated by collecting a single Raman spectrum. There is a lack of methodology for quantifying mineral species in mixtures due to the independent signal strengths of different materials in Raman spectra. Two techniques are presented in this work for quantifying common rock-forming minerals: partial least-squares multivariate analysis and a novel approach called Raman cross-section proxies (numerical metrics associated with specific Raman features). This paper targets 20 mineral species relevant to the mineralogy of the planet Mars. Mineral end-member samples and 187 binary mineral-mineral mixtures (mixture of two distinct minerals) are used for multivariate modeling. Eighteen diamond-mineral mixtures are used to derive Raman cross-section proxies. Mineral abundance proportions are predicted for the binary mineral-mineral mixtures with known mineralogical content to evaluate the efficacy of the two quantitative methods. Technique performance is mineral dependent. The root mean square error for unseen predictions (RMSE-P) using Raman cross-section proxies ranges from ±3.2–17.0 vol%. For the multivariate models, the cross-validated root mean square error (RMSE-CV) ranges from ±8.8 to 26.2 vol%. Although these error estimates are not directly comparable, they provide the most accurate error estimate currently available. Different scenarios may favor the use of one or the other of the two quantitative methods. This work provides fundamental groundwork that can be applied to common rock-forming minerals on terrestrial planets, including Mars. Quantification of mineral abundances aids in answering critical geologic questions related to ancient primary and altered rocks as well as planetary processes and conditions.

  PublisherDOI

• A Novel Surface Energy Balance Method for Thermal Inertia Studies of Terrestrial Analogs

  Earth and Space Science · 2024-09-01 · 4 citations

  articleOpen accessSenior author

  Abstract Surface thermal inertia derived from satellite imagery offers a valuable tool for remotely mapping the physical structure and water content of planetary regolith. Efforts to quantify thermal inertia using surface temperatures on Earth, however, have consistently yielded large uncertainties and suffered from a lack of reproducibility. Unlike dry or airless bodies, Earth's abundant water and dense atmosphere lead to dynamic thermophysical conditions that are a greater challenge to model than on a world like Mars. In this work, an approach was developed using field experiments to inform and fine‐tune a thermophysical model of terrestrial sediment and calculate an inherent thermal inertia value with higher precision and less initial knowledge of the sediment than has previously been achieved remotely on Earth. A thermal inertia derived for a basaltic tephra site in Northern Arizona was replicated within 1% between different field seasons, demonstrating reproducibility. Model‐derived values were validated in situ by two different thermophysical field probes to within 8% of the measured mean values. Analog studies such as this hold the promise of improved interpretations of surface materials on Mars, and an accurate thermal model for Earth is the key step to enabling translation between the two worlds.

  PublisherOA PDFDOI

• Thermal Effects on Drilling Performance in Hot Dry Rock

  IADC/SPE International Drilling Conference and Exhibition · 2024-02-27 · 1 citations

  article

  ABSTRACT High-temperature geothermal resources away from tectonic boundaries or geologic hotspots can be accessed by the drilling of deep wells through significant sections of basement rock. This paper evaluates the impact of rapid cooling on rock cutting process, and incorporates this effect as a part of potential drilling performance optimization. Using data from a series of experiments conducted in a high pressure and high temperature (HPHT) drilling laboratory, we demonstrated that rapid cooling enhanced rates of penetration over 60% in the 300+ °C hot dry rock utilizing a PDC bit or a roller cone bit. Drilling was performed in hard igneous rock samples, with the unconfined compressive strength over 200 MPa. Each sample was heated and confined to predetermined conditions, then drilled with controlled parameters. The drilling performance data was acquired for each experiment, complemented with dynamic in-situ temperature measurements, and visual assessment of rock samples before and after drilling. The rapid cooling effect on the rate of penetration was found to be a function of the temperature difference between the drilling fluid at the bit face and the rock sample temperatures. Unlike previous studies on the Drilling Performance, which overlooked thermal effects, our research focuses on the synergy between rapid cooling and mechanical rock cutting process. This study provides a framework to understand and improve drilling performance for HPHT wells, including deep and hot geothermal wells.

  PublisherDOI

• Diverse volcanism and crustal recycling on early Mars

  Nature Astronomy · 2024-02-12 · 17 citations

  articleOpen access

  Abstract The relatively well-preserved ancient crust of Mars provides a natural window into early planetary evolution not available on Earth due to sustained tectonic recycling and erosion on this planet. Mars has generally been considered a one-plate basaltic planet, though recent evidence suggests magmatic evolution resulting in felsic crust might have occurred sporadically. Here we show multiple lines of evidence for diverse volcanism and complex volcanotectonics in the southern highlands of Mars within and around the ∼3.5–4-billion-year-old Eridania basin. Infrared remote sensing reveals bimodal volcanism consisting of olivine-bearing basalts and voluminous, widespread dacitic (64–69% SiO 2 , and possibly higher) volcanic deposits within a region of high crustal potassium. The diverse igneous compositions are associated with an extraordinary number and morphological range of volcanic structures, including domes, stratovolcanoes, calderas and pyroclastic shields occurring proximal to large (hundreds of kilometres in diametre) basins within the Eridania region. The 2–4 km-deep topographically concave-up basins have crustal thicknesses 10–20 km thinner than adjacent terrain and disrupt patterns of deeply seated remnant crustal magnetism. The Eridania basins may represent ancient episodes of crustal recycling via lithospheric delamination in which altered, hydrated volcanic materials were cycled downward and melted resulting in magmatic evolution analogous to pre-plate tectonic processes on the Archaean Earth.

  PublisherOA PDFDOI

Frequent coauthors

• P. R. Christensen

  Arizona State University

  86 shared

• J. L. Bandfield

  Space Science Institute

  85 shared

• T. D. Glotch

  82 shared

• V. E. Hamilton

  65 shared

• H. Y. McSween

  University of Tennessee at Knoxville

  47 shared

• M. A. Barucci

  Sorbonne Paris Cité

  47 shared

• S. Fornasier

  47 shared

• S. W. Squyres

  University of Maryland, College Park

  46 shared

Labs

• Earth and Planetary Remote Sensing LaboratoryPI

Education

• B.S.

  College of Charleston

  1998

• M.S.

  Arizona State University

  2001

• Ph.D.

  Arizona State University

  2005

• Other

  California Institute of Technology

  2007