B. Horgan

Purdue University West Lafayette

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Co-Authors

E. B. Rampe

Johnson Space Center

R. C. Wiens

Purdue University West Lafayette

J. R. Johnson

Johns Hopkins University Applied Physics Laboratory

N. Mangold

Laboratoire de Planétologie et Géosciences

M. S. Rice

Western Washington University

J. F. Bell

Arizona State University

E. A. Cloutis

University of Winnipeg

A. A. Fraeman

Jet Propulsion Laboratory

K. M. Stack

Jet Propulsion Laboratory

J. F. Bell

Arizona State University

Cooperative Institutions

Jet Propulsion Laboratory

236

Planetary Science Institute

211

California Institute of Technology

190

Centre National de la Recherche Scientifique

119

Arizona State University

109

University of Arizona

Johnson Space Center

Ames Research Center

Cornell University

Johns Hopkins University Applied Physics Laboratory

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Potential Ancient Soils Preserved at Mawrth Vallis from Comparisons with Eastern Oregon Paleosols: Implications for Early Martian Climate

B. Horgan J. L. Bishop P. R. Christensen J. F. Bell

Paleosol

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Citations (4)

Investigating the Response of Sulfides and Fe- Oxides Under Space Weathering Conditions Through the Analysis of Returned and Experimental Samples

Microscopy and Microanalysis (2022)

L. C. Chaves M. S. Thompson B. Horgan Cathy Dukes M. J. Loeffler

Journal Article Investigating the Response of Sulfides and Fe- Oxides Under Space Weathering Conditions Through the Analysis of Returned and Experimental Samples Get access Laura Chaves, Laura Chaves Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, IN, United States Corresponding Author: lchavesm@purdue.edu Search for other works by this author on: Oxford Academic Google Scholar Michelle Thompson, Michelle Thompson Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, IN, United States Search for other works by this author on: Oxford Academic Google Scholar Briony Horgan, Briony Horgan Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, IN, United States Search for other works by this author on: Oxford Academic Google Scholar Cathy Dukes, Cathy Dukes Laboratory for Astrophysics and Surface Physics, University of Virginia, Charlottesville, VA United States. Search for other works by this author on: Oxford Academic Google Scholar Mark Loeffler Mark Loeffler Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ, United States Search for other works by this author on: Oxford Academic Google Scholar Microscopy and Microanalysis, Volume 28, Issue S1, 1 August 2022, Pages 2698–2699, https://doi.org/10.1017/S1431927622010182 Published: 01 August 2022

Atmospheric research

10.1017/s1431927622010182

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Citations (1)

GNARALOO BAY: STRATIGRAPHIC RELATIONSHIPS AT THE APEX OF A MARTIAN FLUVIO-DELTAIC SYSTEM AT JEZERO CRATER, MARS

Robert W. Barnes Sanjeev Gupta Alexander J. Jones B. Horgan Brad Garzcynski

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SPECTRAL ANALYSIS OF EXPLOSIVE AND EFFUSIVE VOLCANISM IN THE MARIUS HILLS VOLCANIC COMPLEX

Abstracts with programs - Geological Society of America (2018)

M. J. McBride B. Horgan Samuel J. Lawrence

Volcanology

10.1130/abs/2018am-321659

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Orbital Context and In Situ Observations of Nili Fossae Olivine-Carbonate

A. J. Brown R. C. Wiens S. Maurice P. Pinet Lucia Mandon

Earth and Space Science Open Archive This is a preprint and has not been peer reviewed. ESSOAr is a venue for early communication or feedback before peer review. Data may be preliminary.Learn more about preprints preprintOpen AccessYou are viewing the latest version by default [v1]Orbital Context and In Situ Observations of Nili Fossae Olivine-CarbonateAuthorsAdrianBrowniDRogerWiensiDSylvestreMauricePatrickPinetiDLuciaMandoniDStephaneLe MoueliciDLisaMayhewAryaUdryiDBrionyHorganiDNathalieTurenneFredCalefEdwardCloutisiDThierryFouchetiDClémentRoyeriDMaría-PazZorzanoiDEleniRavanisSarahFagentsAlbertoFairénSee all authors Adrian BrowniDCorresponding Author• Submitting AuthorSelf EmployediDhttps://orcid.org/0000-0002-9352-6989view email addressThe email was not providedcopy email addressRoger WiensiDSpace Science and ApplicationsiDhttps://orcid.org/0000-0002-3409-7344view email addressThe email was not providedcopy email addressSylvestre MauriceIRAP, CNRS, Université de Toulouse, UPS-OMPview email addressThe email was not providedcopy email addressPatrick PinetiDInstitut de Recherche en Astrophysique et Planétologie (IRAP)iDhttps://orcid.org/0000-0002-1933-5631view email addressThe email was not providedcopy email addressLucia MandoniDLESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de ParisiDhttps://orcid.org/0000-0002-9310-0742view email addressThe email was not providedcopy email addressStephane Le MoueliciDLPG Nantes, UMR 6112, CNRS, OSUNA, Université de NantesiDhttps://orcid.org/0000-0001-5260-1367view email addressThe email was not providedcopy email addressLisa MayhewUniversity of Colorado at Boulderview email addressThe email was not providedcopy email addressArya UdryiDUniversity of Nevada Las VegasiDhttps://orcid.org/0000-0002-0074-8110view email addressThe email was not providedcopy email addressBriony HorganiDPurdue UniversityiDhttps://orcid.org/0000-0001-6314-9724view email addressThe email was not providedcopy email addressNathalie TurenneUniversity of Winnipegview email addressThe email was not providedcopy email addressFred CalefJet Propulsion Laboratoryview email addressThe email was not providedcopy email addressEdward CloutisiDUniversity of WinnipegiDhttps://orcid.org/0000-0001-7301-0929view email addressThe email was not providedcopy email addressThierry FouchetiDLESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de ParisiDhttps://orcid.org/0000-0001-9040-8285view email addressThe email was not providedcopy email addressClément RoyeriDLESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de ParisiDhttps://orcid.org/0000-0002-5472-7235view email addressThe email was not providedcopy email addressMaría-Paz ZorzanoiDCentro de AstrobiologíaiDhttps://orcid.org/0000-0002-4492-9650view email addressThe email was not providedcopy email addressEleni RavanisUniversity of Hawaii at Manoaview email addressThe email was not providedcopy email addressSarah FagentsUniv Hawaiiview email addressThe email was not providedcopy email addressAlberto FairénCentro de Astrobiología (CSIC-INTA), Madrid, Spain, and Dept. of Astronomy, Cornell Universityview email addressThe email was not providedcopy email address

Electronic mail

10.1002/essoar.10509013.1

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Citations (0)

Complex Volcanism at Lunar Floor-Fractured Crater Oppenheimer U

L. R. Gaddis K. A. Bennett B. Horgan Marie McBride J. D. Stopar

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The Global Distribution of Weathered Glass on Mars

AGUFM (2012)

B. Horgan M. Chojnacki Jialong Lai David Clarke J. Joseph

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Preliminary Results from a Field Study of the Mineralogy of the White Sands National Monument Dune Field

Lunar and Planetary Science Conference (2014)

L. K. Fenton J. L. Bishop B. Lafuente B. Horgan Anna Szynkiewicz

White (mutation)

National monument

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Deriving Amorphous Component Abundance and Composition of Rocks and Sediments on Earth and Mars

Journal of Geophysical Research Planets (2018)

R. J. Smith E. B. Rampe B. Horgan E. Dehouck

Abstract X‐ray amorphous materials have been detected in all samples measured by the CheMin X‐ray diffractometer (XRD) on board the Mars Science Laboratory rover in Gale Crater, Mars. The origin(s) of these materials are poorly understood, and there are significant uncertainties on their estimated abundances and compositions. Three methods are used to estimate the bulk amorphous component abundance and composition of Martian samples using XRD and bulk chemical data: (1) Rietveld refinements, (2) FULLPAT analyses, and (3) mass balance calculations. We tested these methods against a quantitative XRD (internal standard) method commonly used in terrestrial laboratories. Additionally, we tested for instrumentation effects by measuring our samples on a laboratory XRD instrument (PANalytical X'Pert Pro) and the CheMin test bed instrument (CheMin IV). We used three natural samples known to contain amorphous materials: glacial sediment, Hawaiian soil, and a paleosol. Our methods resulted in nine amorphous abundances and four amorphous compositions for each sample. For a single sample, amorphous abundance estimates and amorphous compositions are relatively similar across all estimation methods. CheMin analog measurements perform well in our tests, with amorphous abundances and compositions comparable to laboratory quantitative XRD measurements, though slightly underestimated. This suggests that previous amorphous component estimates for Martian samples are relatively accurate. This study highlights the usefulness of the mass balance calculation method for characterizing amorphous materials in terrestrial samples, providing important supplemental information to destructive and time consuming size separation and dissolution procedures.

10.1029/2018je005612

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Citations (33)

Spectral Diversity of Rocks and Soils in Mastcam Observations Along the Curiosity Rover's Traverse in Gale Crater, Mars

Journal of Geophysical Research Planets (2022)

M. S. Rice Christina Seeger J. F. Bell F. J. Calef Michael St. Clair

Abstract The Mars Science Laboratory Curiosity rover has explored over 400 m of vertical stratigraphy within Gale crater to date. These fluvio‐deltaic, lacustrine, and aeolian strata have been well‐documented by Curiosity's in situ and remote science instruments, including the Mast Camera (Mastcam) pair of multispectral imagers. Mastcam visible to near‐infrared spectra can broadly distinguish between iron phases and oxidation states, and in combination with chemical data from other instruments, Mastcam spectra can help constrain mineralogy, depositional origin, and diagenesis. However, no traverse‐scale analysis of Mastcam multispectral data has yet been performed. We compiled a database of Mastcam spectra from >600 multispectral observations and quantified spectral variations across Curiosity's traverse through Vera Rubin ridge (sols 0–2302). From principal component analysis and an examination of spectral parameters, we identified nine rock spectral classes and five soil spectral classes. Rock classes are dominated by spectral differences attributed to hematite and other oxides (due to variations in grain size, composition, and abundance) and are mostly confined to specific stratigraphic members. Soil classes fall along a mixing line between soil spectra dominated by fine‐grained Fe‐oxides and those dominated by olivine‐bearing sands. By comparing trends in soil versus rock spectra, we find that locally derived sediments are not significantly contributing to the spectra of soils. Rather, varying contributions of dark, mafic sands from the active Bagnold Dune field is the primary spectral characteristic of soils. These spectral classes and their trends with stratigraphy provide a basis for comparison in Curiosity's ongoing exploration of Gale crater.

Spectral slope

10.1029/2021je007134

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Citations (15)