Jeff Andrews-Hanna

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Chapters

• Andrews-hanna, J. C., Andrews-hanna, J. C., Zuber, M. T., & Zuber, M. T. (2010).

  Elliptical craters and basins on the terrestrial planets

  . In Large meteorite impacts and planetary evolution. Geological Society of America. doi:10.1130/2010.2465(01)
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  The four largest well-preserved impact basins in the solar system, Borealis, Hellas, and Utopia on Mars, and South Pole–Aitken on the Moon, are all signifi cantly elongated, with aspect ratios >1.2. This population stands in contrast to experimental studies of impact cratering that predict

Journals/Publications

• Andrews-Hanna, J. (2018). Structure and evolution of the lunar interior. New Views of the Moon 2 (Reviews in Mineralogy and Geophysics).
• Andrews-Hanna, J. C., Weber, R. C., Garrick-Bethell, I., Evans, A. J., Kiefer, W. S., Grimm, R. E., Keane, J. T., Laneuville, M., Ishihara, Y., Kamata, S., & Matsuyama, I. (2023). The Structure and Evolution of the Lunar Interior. Reviews in Mineralogy and Geochemistry, 89(1), 243-292.
• Andrews-Hanna, J., & Broquet, A. (2023). The history of global strain and geodynamics on Mars. \icarus, 395, 115476.
• Bjonnes, E., Johnson, B. C., & Andrews-Hanna, J. C. (2023). Basin Crustal Structure at the Multiring Basin Transition. Journal of Geophysical Research (Planets), 128(4), e2022JE007507.
• Broquet, A., & Andrews-Hanna, J. (2023). Geophysical evidence for an active mantle plume underneath Elysium Planitia on Mars. Nature Astronomy, 7, 160-169.
• Broquet, A., & Andrews-Hanna, J. (2023). Plume-induced flood basalts on Hesperian Mars: An investigation of Hesperia Planum. \icarus, 391, 115338.
• Liang, W., Andrews-Hanna, J. C., & Evans, A. J. (2023). The Missing Craters and Basin Rings Beneath the Lunar Maria. Journal of Geophysical Research (Planets), 128(12), e2023JE007876.
• Moruzzi, S. A., Andrews-Hanna, J. C., Schenk, P., & Johnson, B. C. (2023). Pluto's Sputnik basin as a peak-ring or multiring basin: A comparative study. \icarus, 405, 115721.
• Moruzzi, S. A., Kiefer, W. S., & Andrews-Hanna, J. C. (2023). Thrust faulting on Venus: Tectonic modeling of the Vedma Dorsa Ridge Belt. \icarus, 392, 115378.
• Nahm, A. L., Watters, T. R., Johnson, C. L., Banks, M. E., Bogert, C. H., Weber, R. C., & Andrews-Hanna, J. C. (2023). Tectonics of the Moon. Reviews in Mineralogy and Geochemistry, 89(1), 691-727.
• Siegler, M. A., Feng, J., Lehman-Franco, K., Andrews-Hanna, J. C., Economos, R. C., Clair, M. S., Million, C., Head, J. W., Glotch, T. D., & White, M. N. (2023). Author Correction: Remote detection of a lunar granitic batholith at Compton-Belkovich. \nat, 622(7982), E1-E1.
• Andrews-Hanna, J. C. (2022). Marsquakes coming into focus. Nature Astronomy, 6, 1349-1350.
• Andrews-Hanna, J. C., & Liang, W. (2022). Probing the source of ancient linear gravity anomalies on the Moon. Icarus. doi:10.1016/j.icarus.2022.114978
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  A large set of linear to arcuate gravity anomalies which are not associated with any surface expressions was revealed by lunar gravity data from the GRAIL mission. The anomalies can be categorized into two types: a set of large anomalies that border the Procellarum KREEP terrane (PKT) region, and the linear gravity anomalies (LGAs) that are scattered throughout the lunar highlands. In this study, we use band-passed gravity gradient maps and localized power spectral analyses to characterize the nature of and the differences between the two types of anomalies. The results show that the PKT border anomalies are primarily long wavelength features whose power spectra are not clearly distinguishable from the background spectrum of the surrounding region, while the linear gravity anomalies are short wavelength features whose power spectra in at least one case rises significantly above the background spectrum over a wide range of degrees. This difference in gravitational signature suggests a fundamental difference in the nature of the sources of the two types of anomalies. We then used a Markov chain Monte Carlo model to test different interpretations for the most prominent LGA by comparing the observed power spectrum to modeled spectra for elliptical, triangular, and T-shaped intrusive geometries. We find multiple geometries are able to fit the power spectrum of the LGA equally well. Analogs of comparable scale to the LGAs originate from extensional stress regimes, supporting an inferred period of global expansion in the early Moon, though the cause of that expansion remains uncertain. If the depth extent of the intrusions were governed by neutral buoyancy, we find that intrusions on the nearside similar to those on the farside would have been eruptive and may have contributed to the earliest mare volcanism. The total volume of the intrusions is ~20% of the mare volume, revealing a lower magma production rate on the farside than on the nearside. • Lunar linear gravity anomalies fundamentally different from PKT border anomalies in nature and origin. • Prominent northern farside linear gravity anomaly (~600 km length) has a best-fit top depth of ~10 km. • Inferred intrusions beneath large Martian collapse pits perhaps best analog to lunar linear gravity anomalies.
• Hood, L., Oliveira, J., Andrews-Hanna, J. .., Wieczorek, M., & Stewart, S. (2021). Magnetic Anomalies in Five Lunar Impact Basins: Implications for Impactor Trajectories and Inverse Modeling. Journal of Geophysical Research (Planets), 126(2), e06668.
• Horvath, D. G., & Andrews-Hanna, J. C. (2021). The hydrology and climate of Mars during the sedimentary infilling of Gale crater. Earth and Planetary Science Letters, 568, 117032.
• Horvath, D. G., Moitra, P., Hamilton, C. W., Craddock, R. A., & Andrews-Hanna, J. C. (2021). Evidence for geologically recent explosive volcanism in Elysium Planitia, Mars. \icarus, 365, 114499.
• Moitra, P., Horvath, D. G., & Andrews-Hanna, J. C. (2021). Investigating the roles of magmatic volatiles, ground ice and impact-triggering on a very recent and highly explosive volcanic eruption on Mars. Earth and Planetary Science Letters, 567, 116986.
• Andrews-Hanna, J. C. (2020). The tectonic architecture of wrinkle ridges on Mars. \icarus, 351, 113937.
• Horvath, D. G., Moitra, P., Hamilton, C. W., Craddock, R. A., & Andrews-Hanna, J. C. (2020). Evidence for geologically recent explosive volcanism in Elysium Planitia, Mars. arXiv e-prints, arXiv:2011.05956.
• Jansen, J., Andrews-Hanna, J., Milbury, C., Head, I., Li, Y., Melosh, H., & Zuber, M. (2019). Radial gravity anomalies associated with the ejecta of the Orientale basin. \icarus, 319, 444-458.
• Andrews-Hanna, J., Head, J., Johnson, B., Keane, J., Kiefer, W., McGovern, P., Neumann, G., Wieczorek, M., & Zuber, M. (2018). Ring faults and ring dikes around the Orientale basin on the Moon. \icarus, 310, 1-20.
• Andrews-hanna, J. C., Collins, G. S., Freed, A. M., Johnson, B. C., Melosh, H. J., & Zuber, M. T. (2018).

  Controls on the Formation of Lunar Multiring Basins

  . Journal of Geophysical Research, 123(11), 3035-3050. doi:10.1029/2018je005765
• Evans, A., Andrews-Hanna, J., Head, J., Soderblom, J., Solomon, S., & Zuber, M. (2018). Reexamination of Early Lunar Chronology With GRAIL Data: Terranes, Basins, and Impact Fluxes. Journal of Geophysical Research (Planets), 123, 1596-1617.
• Evans, A., Tikoo, S., & Andrews-Hanna, J. (2018). The Case Against an Early Lunar Dynamo Powered by Core Convection. Geophysical Research Letters, 45, 98-107.
• Bottke, W., & Andrews-Hanna, J. (2017). A post-accretionary lull in large impacts on early Mars. Nature Geoscience, 10, 344-348.
• Cole, H., & Andrews-Hanna, J. (2017). The anatomy of a wrinkle ridge revealed in the wall of Melas Chasma, Mars. Journal of Geophysical Research (Planets), 122, 889-900.
• Horvath, D., & Andrews-Hanna, J. (2017). Reconstructing the past climate at Gale crater, Mars, from hydrological modeling of late-stage lakes. Geophysical Research Letters, 44, 8196-8204.
• Jansen, J., Andrews-Hanna, J., Li, Y., Lucey, P., Taylor, G., Goossens, S., Lemoine, F., Mazarico, E., Head, J., Milbury, C., Kiefer, W., Soderblom, J., & Zuber, M. (2017). Small-scale density variations in the lunar crust revealed by GRAIL. Icarus, 291, 107-123.
• Andrews-hanna, J. C., Goossens, S., Head, J. W., Jansen, J. C., Kiefer, W. S., Lemoine, F. G., Li, Y., Lucey, P. G., Mazarico, E., Milbury, C., Soderblom, J. M., Taylor, G. J., & Zuber, M. T. (2016).

  Small-scale density variations in the lunar crust revealed by GRAIL.

  . Icarus, 291, 107-123. doi:10.1016/j.icarus.2017.03.017
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  Data from the Gravity Recovery and Interior Laboratory (GRAIL) mission have revealed that ~98% of the power of the gravity signal of the Moon at high spherical harmonic degrees correlates with the topography. The remaining 2% of the signal, which cannot be explained by topography, contains information about density variations within the crust. These high-degree Bouguer gravity anomalies are likely caused by small-scale (10's of km) shallow density variations. Here we use gravity inversions to model the small-scale three-dimensional variations in the density of the lunar crust. Inversion results from three non-descript areas yield shallow density variations in the range of 100-200 kg/m3. Three end-member scenarios of variations in porosity, intrusions into the crust, and variations in bulk crustal composition were tested as possible sources of the density variations. We find that the density anomalies can be caused entirely by changes in porosity. Characteristics of density anomalies in the South Pole-Aitken basin also support porosity as a primary source of these variations. Mafic intrusions into the crust could explain many, but not all of the anomalies. Additionally, variations in crustal composition revealed by spectral data could only explain a small fraction of the density anomalies. Nevertheless, all three sources of density variations likely contribute. Collectively, results from this study of GRAIL gravity data, combined with other studies of remote sensing data and lunar samples, show that the lunar crust exhibits variations in density by ±10% over scales ranging from centimeters to 100's of kilometers.
• Ehlmann, B., Anderson, F., Andrews-Hanna, J. .., Catling, D., Christensen, P., Cohen, B., Dressing, C., Edwards, C., Elkins-Tanton, L., Farley, K., Fassett, C., Fischer, W., Fraeman, A., Golombek, M., Hamilton, V., Hayes, A., Herd, C., Horgan, B., Hu, R., , Jakosky, B., et al. (2016). The sustainability of habitability on terrestrial planets: Insights, questions, and needed measurements from Mars for understanding the evolution of Earth-like worlds. Journal of Geophysical Research (Planets), 121, 1927-1961.
• Evans, A., Soderblom, J., Andrews-Hanna, J., Solomon, S., & Zuber, M. (2016). Identification of buried lunar impact craters from GRAIL data and implications for the nearside maria. \grl, 43, 2445-2455.
• Horvath, D., Andrews-Hanna, J., Newman, C., Mitchell, K., & Stiles, B. (2016). The influence of subsurface flow on lake formation and north polar lake distribution on Titan. Icarus, 277, 103-124.
• Johnson, B., Blair, D., Collins, G., Melosh, H., Freed, A., Taylor, G., Head, J., Wieczorek, M., Andrews-Hanna, J., Nimmo, F., Keane, J., Miljkovi{\'c}, K., Soderblom, J., & Zuber, M. (2016). Formation of the Orientale lunar multiring basin. Science, 354, 441-444.
• Karasozen, E., Andrews-Hanna, J., Dohm, J., & Anderson, R. (2016). The formation of the South Tharsis Ridge Belt: Basin and Range-style extension on early Mars?. Journal of Geophysical Research (Planets), 121, 916-943.
• Zuber, M., Smith, D., Neumann, G., Goossens, S., Andrews-Hanna, J., Head, J., Kiefer, W., Asmar, S., Konopliv, A., Lemoine, F., Matsuyama, I., Melosh, H., McGovern, P., Nimmo, F., Phillips, R., Solomon, S., Taylor, G., Watkins, M., Wieczorek, M., , Williams, J., et al. (2016). Gravity field of the Orientale basin from the Gravity Recovery and Interior Laboratory Mission. Science, 354, 438-441.
• Andrews-hanna, J. C., Asmar, S. W., Baker, D. M., Goossens, S. J., Head, J. W., Kiefer, W. S., Konopliv, A. S., Lemoine, F. G., Mazarico, E., Melosh, H. J., Miljkovic, K., Neumann, G. A., Nimmo, F., Phillips, R. J., Sabaka, T. J., Smith, D. E., Soderblom, J. M., Solomon, S. C., Sori, M. M., , Wieczorek, M. A., et al. (2015).

  Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements.

  . Science advances, 1(9), e1500852. doi:10.1126/sciadv.1500852
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  Observations from the Gravity Recovery and Interior Laboratory (GRAIL) mission indicate a marked change in the gravitational signature of lunar impact structures at the morphological transition, with increasing diameter, from complex craters to peak-ring basins. At crater diameters larger than ~200 km, a central positive Bouguer anomaly is seen within the innermost peak ring, and an annular negative Bouguer anomaly extends outward from this ring to the outer topographic rim crest. These observations demonstrate that basin-forming impacts remove crustal materials from within the peak ring and thicken the crust between the peak ring and the outer rim crest. A correlation between the diameter of the central Bouguer gravity high and the outer topographic ring diameter for well-preserved basins enables the identification and characterization of basins for which topographic signatures have been obscured by superposed cratering and volcanism. The GRAIL inventory of lunar basins improves upon earlier lists that differed in their totals by more than a factor of 2. The size-frequency distributions of basins on the nearside and farside hemispheres of the Moon differ substantially; the nearside hosts more basins larger than 350 km in diameter, whereas the farside has more smaller basins. Hemispherical differences in target properties, including temperature and porosity, are likely to have contributed to these different distributions. Better understanding of the factors that control basin size will help to constrain models of the original impactor population.
• Soderblom, J., Evans, A., Johnson, B., Melosh, H., Miljkovi{\'c}, K., Phillips, R., Andrews-Hanna, J., Bierson, C., Head, J., Milbury, C., Neumann, G., Nimmo, F., Smith, D., Solomon, S., Sori, M., Wieczorek, M., & Zuber, M. (2015). The fractured Moon: Production and saturation of porosity in the lunar highlands from impact cratering. \grl, 42, 6939-6944.
• Andrews-Hanna, J., Besserer, J., Head, J., Howett, C., Kiefer, W., Lucey, P., McGovern, P., Melosh, H., Neumann, G., Phillips, R., Schenk, P., Smith, D., Solomon, S., & Zuber, M. (2014). Structure and evolution of the lunar Procellarum region as revealed by GRAIL gravity data. Nature, 514, 68-71.
• Besserer, J., Nimmo, F., Wieczorek, M., Weber, R., Kiefer, W., McGovern, P., Andrews-Hanna, J., Smith, D., & Zuber, M. (2014). GRAIL gravity constraints on the vertical and lateral density structure of the lunar crust. \grl, 41, 5771-5777.
• Williams, J., Konopliv, A., Boggs, D., Park, R., Yuan, D., Lemoine, F., Goossens, S., Mazarico, E., Nimmo, F., Weber, R., Asmar, S., Melosh, H., Neumann, G., Phillips, R., Smith, D., Solomon, S., Watkins, M., Wieczorek, M., Andrews-Hanna, J., , Head, J., et al. (2014). Lunar interior properties from the GRAIL mission. Journal of Geophysical Research (Planets), 119, 1546-1578.
• Andrews-Hanna, J. (2013). The origin of the non-mare mascon gravity anomalies in lunar basins. \icarus, 222, 159-168.
• Andrews-Hanna, J., Asmar, S., Head, J., Kiefer, W., Konopliv, A., Lemoine, F., Matsuyama, I., Mazarico, E., McGovern, P., Melosh, H., Neumann, G., Nimmo, F., Phillips, R., Smith, D., Solomon, S., Taylor, G., Wieczorek, M., Williams, J., & Zuber, M. (2013). Ancient Igneous Intrusions and Early Expansion of the Moon Revealed by GRAIL Gravity Gradiometry. Science, 339, 675-678.
• Isherwood, R., Jozwiak, L., Jansen, J., & Andrews-Hanna, J. (2013). The volcanic history of Olympus Mons from paleo-topography and flexural modeling. Earth and Planetary Science Letters, 363, 88-96.
• Kattoum, Y., & Andrews-Hanna, J. (2013). Evidence for ring-faults around the Orientale basin on the Moon from gravity. \icarus, 226, 694-707.
• Melosh, H., Freed, A., Johnson, B., Blair, D., Andrews-Hanna, J., Neumann, G., Phillips, R., Smith, D., Solomon, S., Wieczorek, M., & Zuber, M. (2013). The Origin of Lunar Mascon Basins. Science, 340, 1552-1555.
• Wieczorek, M., Neumann, G., Nimmo, F., Kiefer, W., Taylor, G., Melosh, H., Phillips, R., Solomon, S., Andrews-Hanna, J., Asmar, S., Konopliv, A., Lemoine, F., Smith, D., Watkins, M., Williams, J., & Zuber, M. (2013). The Crust of the Moon as Seen by GRAIL. Science, 339, 671-675.
• Andrews-hanna, J. C. (2012).

  The formation of Valles Marineris: 1. Tectonic architecture and the relative roles of extension and subsidence

  . Journal of Geophysical Research, 117(E3), n/a-n/a. doi:10.1029/2011je003953
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  [1] The formation of the Valles Marineris troughs on Mars is widely held to involve some combination of horizontal extension and vertical subsidence or collapse, but the specific tectonic mechanism is poorly understood. This study uses boundary element models of Valles Marineris formation to evaluate a range of fault dip angles for two end-member models of trough formation: simple extensional tectonism, and extension together with vertical accommodation at the base of the lithosphere representing either viscous lower crustal flow or some other form of deep-seated collapse. The models are constrained by the lack of footwall uplift on the plateau surface outside the troughs, and the lack of significant tectonic failure of the plateau in response to the stress changes induced by Valles Marineris formation. The results demonstrate that trough formation by extensional tectonism alone generates large surface uplifts in the surrounding plateau and enormous stresses in the lithosphere, in conflict with the observations. The only mechanism that is compatible with both the observed topography and the limitations imposed by the finite strength of the lithosphere is trough formation through displacement along steeply dipping to subvertical border faults, together with vertical accommodation at the base of the subsiding fault block. Fault dips are constrained to be greater than or equal to 85°, leading to a ratio of vertical subsidence to horizontal extension exceeding 5.7 and a maximum extension of less than 4.6 km. These results confirm earlier studies suggesting that trough formation involved a substantial component of vertical subsidence or collapse, with only modest amounts of total extension.
• Andrews-hanna, J. C. (2012).

  The formation of Valles Marineris: 2. Stress focusing along the buried dichotomy boundary

  . Journal of Geophysical Research, 117(E4), n/a-n/a. doi:10.1029/2011je003954
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  [1] Although Valles Marineris is widely regarded as an extensional tectonic feature, the source of stress responsible for its formation remains unknown. This study argues that the tensile stresses that triggered Valles Marineris tectonism are a result of its location south of and subparallel to the buried crustal dichotomy boundary beneath Tharsis. The emplacement of the Tharsis volcanic load straddling the pre-existing topographic step of the crustal dichotomy boundary would have resulted in an abrupt change in the thickness of the load, causing differential subsidence and extension across the boundary. Thin-shell flexural models predict a narrow belt of focused tensile stresses south of the buried dichotomy boundary, coinciding with the location of present-day Valles Marineris. The interaction of these boundary-generated stresses with the competing stress fields associated with Tharsis loading can explain the formation of Noctis Labyrinthus in the west, and the deflection of the Valles Marineris troughs away from the buried boundary toward the east. Finite element models demonstrate that the magnitudes and vertical variations of stress at Valles Marineris are sensitive to the timing of loading and flexure in Tharsis. The incremental loading and flexure expected for a large volcanic rise results in the maximum tensile stress at Valles Marineris occurring at depth, with tensile stresses through the majority of the lithospheric column. Dikes forming within this tensile stress belt would propagate through the full vertical extent of the lithosphere due to the stress release associated with the dilation of the dikes, playing a crucial role in the formation of the Valles Marineris troughs.
• Andrews-hanna, J. C. (2012).

  The formation of Valles Marineris: 3. Trough formation through super-isostasy, stress, sedimentation, and subsidence

  . Journal of Geophysical Research, 117(E6), n/a-n/a. doi:10.1029/2012je004059
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  [1] Despite the enormous size of the Valles Marineris chasmata on Mars, the mechanism responsible for the formation of these unique troughs remains unknown. Previous studies proposed mechanisms of trough formation through extensional tectonism, vertical collapse into subsurface voids, or some combination of the two. Recent work in a pair of companion papers demonstrated that the troughs must have formed dominantly by vertical subsidence with little net horizontal extension, and that the modest extension required likely arose from the effect of the buried dichotomy boundary beneath Tharsis. This study now proposes a new mechanism of Valles Marineris formation, with a focus on the large-scale geodynamic and tectonic processes. Prior to the formation of Valles Marineris, the lithosphere within Tharsis was maintained in a super-isostatic state by the membrane-flexural support of the rise. Local moderate extension at Valles Marineris controlled subsequent intrusive activity, resulting in the emplacement of long parallel dikes. This intrusive activity weakened the lithosphere, effectively removing the flexural support from long lithospheric blocks. Left unsupported, these blocks would have subsided approximately 0.49 ± 0.32 km to their isostatic level. The total subsidence would have been increased to 8.6 ± 5.6 km by the effects of contemporaneous sedimentary loading within the troughs and viscous deformation at the base of the crust. This mechanism successfully predicts the observed depths of the Valles Marineris chasmata, and is consistent with all geological and geophysical observations. The unique nature of Valles Marineris is explained as a result of the unique geodynamic and tectonic environment of Tharsis.
• Andrews-hanna, J. C., Li, J., Phillips, R. J., Plaut, J. J., Sun, Y., & Zuber, M. T. (2012).

  Density variations within the south polar layered deposits of Mars

  . Journal of Geophysical Research, 117(E4), n/a-n/a. doi:10.1029/2011je003937
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  [1] The south polar layered deposits (SPLD) constitute the largest known reservoir of water on Mars. Previous studies solved for the best fit uniform density of the deposits using a forward approach. Here we invert for the lateral density variations in the layered deposit using gravity data from radio tracking of Mars Reconnaissance Orbiter, topography from MOLA on board Mars Global Surveyor, and radar sounding data from MARSIS on board Mars Express. We use the gravity anomalies outside the SPLD to construct a Wiener filter, which is applied to the gravitational signature of the SPLD to remove the short-wavelength anomalies over the SPLD that are spectrally consistent with an origin in the crust or mantle. We then use a constrained inversion for the vertically averaged density within the SPLD as a function of position. The results suggest significant density variations within the SPLD. An inverse relationship between the density and thickness of the SPLD suggests that thicker portions of the cap contain less dust. Alternatively, the Dorsa Argentea Formation may extend beneath the SPLD and result in the observed high gravity anomaly in the marginal area of the SPLD. We find these conclusions to be robust against the choice of inversion constraint and perturbations to the applied filter. A synthetic test is also performed to verify the recoverability of the density variation in our approach.
• Andrews-hanna, J. C., Wiseman, S. M., & Zabrusky, K. (2012).

  Reconstructing the distribution and depositional history of the sedimentary deposits of Arabia Terra, Mars

  . Icarus, 220(2), 311-330. doi:10.1016/j.icarus.2012.05.007
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  Abstract The sedimentary deposits of Meridiani Planum formed during the martian climate transition at the Noachian–Hesperian boundary between warm–wet and cold–dry conditions, and give valuable insight into how and when this transition occurred. We show that these deposits share characteristics with sedimentary outcrops across Arabia Terra. Despite near-ubiquitous dust cover across much of Arabia Terra, spectral signatures of polyhydrated sulfate minerals resembling those in Meridiani were identified in Schiaparelli and another unnamed crater. An erosional morphology analysis using both image and topographic data was then used to identify morphologies characteristic of Meridiani-type deposits and catalogue their occurrences throughout Arabia Terra. The occurrences of deposits with compositions and morphologies resembling the Meridiani deposits throughout Arabia Terra suggest that Meridiani-type sedimentary rocks were once more widespread. Elevations of the eroded remnants were used to reconstruct the pre-erosional paleo-surface of the deposits. Within this study area, these deposits once covered ∼2.5–3.6 × 106 km2 and represent an eroded volume of 0.9–1.7 × 106 km3 of sediment. Crater retention ages using craters of a range of preservation states and stratigraphic levels reveal that the deposits were laid down and subsequently eroded during a ∼270 Myr period between ∼3.83 and 3.56 Ga. The deposits formed following the transition from fluvial dissection to evaporite deposition at the end of the Noachian. The high erosion rates (∼3 × 10−6 m/yr) suggest that Mars may have maintained a thick atmosphere relative to today even as it dried out in the Early Hesperian.
• Andrews-hanna, J. C., & Lewis, K. W. (2011).

  Early Mars hydrology: 2. Hydrological evolution in the Noachian and Hesperian epochs

  . Journal of Geophysical Research, 116(E2). doi:10.1029/2010je003709
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  [1] Mars was warmer and wetter during the early to middle Noachian, before a hydrologic and climatic transition in the late Noachian led to a decrease in erosion rates, a change in valley network morphology, and a geochemical shift from phyllosilicate to sulfate formation that culminated in the formation of widespread sulfate-rich sedimentary deposits in Meridiani Planum and the surrounding Arabia Terra region. This secular evolution was overprinted by episodic and periodic variability, as recorded in the fluvial record, sedimentary layering, and erosional discontinuities. We investigate the temporal evolution of Martian groundwater hydrology during the Noachian and early Hesperian epochs using global-scale hydrological models. The results suggest that the more active hydrological cycle in the Noachian was a result of a greater total water inventory, causing a saturated near-surface and high precipitation rates. The late Noachian hydrologic, climatic, and geochemical transition can be explained by a fundamental shift in the hydrological regime driven by a net loss of water due to impact and solar wind erosion of the atmosphere. Following this transition, the water table retreated deep beneath the surface, except in isolated regions of focused groundwater upwelling and evaporation, producing the playa evaporites in Meridiani Planum and Arabia Terra. This long-term evolution was modulated by shorter-term climate forcing in the form of periodic and chaotic variations in the orbital parameters of Mars, resulting in changes in the volume of water sequestered in the polar caps and cryosphere. This shorter-term forcing can explain the observed periodic and bundled sedimentary layering, erosional unconformities, and evidence for a fluctuating water table at Meridiani Planum.
• Andrews-hanna, J. C., Baldridge, A. M., Bishop, J. L., Chojnacki, M., Clark, R. N., Dundas, C. M., Ehlmann, B. L., Milliken, R. E., Murchie, S. L., Seelos, F. P., Squyres, S. W., Swayze, G. A., Tornabene, L. L., & Wray, J. J. (2011).

  Columbus crater and other possible groundwater-fed paleolakes of Terra Sirenum, Mars

  . Journal of Geophysical Research, 116(1). doi:10.1029/2010je003694
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  Columbus crater in the Terra Sirenum region of the Martian southern highlands contains light-toned layered deposits with interbedded sulfate and phyllosilicate minerals, a rare occurrence on Mars. Here we investigate in detail the morphology, thermophysical properties, mineralogy, and stratigraphy of these deposits; explore their regional context; and interpret the crater's aqueous history. Hydrated mineral-bearing deposits occupy a discrete ring around the walls of Columbus crater and are also exposed beneath younger materials, possibly lava flows, on its floor. Widespread minerals identified in the crater include gypsum, polyhydrated and monohydrated Mg/Fe-sulfates, and kaolinite; localized deposits consistent with montmorillonite, Fe/Mg-phyllosilicates, jarosite, alunite, and crystalline ferric oxide or hydroxide are also detected. Thermal emission spectra suggest abundances of these minerals in the tens of percent range. Other craters in northwest Terra Sirenum also contain layered deposits and Al/Fe/Mg-phyllosilicates, but sulfates have so far been found only in Columbus and Cross craters. The region's intercrater plains contain scattered exposures of Al-phyllosilicates and one isolated mound with opaline silica, in addition to more common Fe/Mg-phyllosilicates with chlorides. A Late Noachian age is estimated for the aqueous deposits in Columbus, coinciding with a period of inferred groundwater upwelling and evaporation, which (according to model results reported here) could have formed evaporites in Columbus and other craters in Terra Sirenum. Hypotheses for the origin of these deposits include groundwater cementation of crater-filling sediments and/or direct precipitation from subaerial springs or in a deep (∼900 m) paleolake. Especially under the deep lake scenario, which we prefer, chemical gradients in Columbus crater may have created a habitable environment at this location on early Mars.
• Andrews-hanna, J. C., Arvidson, R. E., Bishop, J. L., Dobrea, E. N., Glotch, T. D., Lichtenberg, K. A., Morris, R. V., Murchie, S. L., Mustard, J. F., Remolar, D. F., & Roach, L. H. (2010).

  Stratigraphy of hydrated sulfates in the sedimentary deposits of Aram Chaos, Mars

  . Journal of Geophysical Research, 115. doi:10.1029/2009je003353
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  [1] Sedimentary deposits within the 280 km wide crater containing Aram Chaos (∼3°N, 339°E) have been differentially eroded by wind to expose a stratigraphic column 900–1000 m thick that unconformably overlies the chaos bedrock. A detailed stratigraphic and mineralogical description of the deposits is presented based on data from the Mars Reconnaissance Orbiter Compact Reconnaissance Imaging Spectrometer for Mars, Context Imager, and High Resolution Imaging Science Experiment. Two sedimentary units overlie the basement chaos material representing the original plains fill in Aram Crater: the first and oldest is composed of (1) a 50–75 m thick dark-toned basal unit containing ferric hydroxysulfate intercalated with monohydrated-sulfate-bearing materials, (2) a 75–100 m thick light-toned unit with monohydrated sulfates, and (3) a 175–350 m thick light-toned resistant capping unit with nanophase ferric oxides and monohydrated sulfates. After a period of wind erosion, these deposits were partially and unconformably covered by the second sedimentary unit, a 75–100 m thick, discontinuous dark-toned unit containing crystalline hematite and polyhydrated sulfate material. These sedimentary deposits were formed by evaporite deposition during at least two distinct rising groundwater episodes fed by regional-scale recharge. Later groundwater event(s) formed the polyhydrated materials, indicating that environmental conditions changed to a higher water-to-rock ratio. Wind has continued to shape the landscape after the last wetting event to produce the features and exposures observed.
• Andrews-hanna, J. C., Arvidson, R. E., Bishop, J. L., Griffes, J. L., Marais, D. J., Morris, R. V., Murchie, S. L., Poulet, F., Seelos, F. P., & Wiseman, S. M. (2010).

  Spectral and stratigraphic mapping of hydrated sulfate and phyllosilicate‐bearing deposits in northern Sinus Meridiani, Mars

  . Journal of Geophysical Research, 115. doi:10.1029/2009je003354
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  We present detailed stratigraphic and spectral analyses that focus on a region in northern Sinus Meridiani located between 1°N to 5°N latitude and 3°W to 1°E longitude. Several stratigraphically distinct units are defined and mapped using morphologic expression, spectral properties, and superposition relationships. Previously unreported exposures of hydrated sulfates and Fe/Mg smectites are identified using MRO CRISM and MEX OMEGA near‐infrared (1.0 to 2.5 µm) spectral reflectance observations. Layered deposits with monohydrated and polyhydrated sulfate spectral signatures that occur in association with a northeast‐southwest trending valley are reexamined using highresolution CRISM, HiRISE, and CTX images. Layers that are spectrally dominated by monohydrated and polyhydrated sulfates are intercalated. The observed compositional layering implies that multiple wetting events, brine recharge, or fluctuations in evaporation rate occurred. We infer that these hydrated sulfate‐bearing layers were unconformably deposited following the extensive erosion of preexisting layered sedimentary rocks and may postdate the formation of the sulfate‐ and hematite‐bearing unit analyzed by the MER Opportunity rover. Therefore, at least two episodes of deposition separated by an unconformity occurred. Fe/Mg phyllosilicates are detected in units that predate the sulfateand hematite‐bearing unit. The presence of Fe/Mg smectite in older units indicates that the relatively low pH formation conditions inferred for the younger sulfate‐ and hematitebearing unit are not representative of the aqueous geochemical environment that prevailed during the formation and alteration of earlier materials. Sedimentary deposits indicative of a complex aqueous history that evolved over time are preserved in Sinus Meridiani, Mars.
• Andrews-hanna, J. C., Arvidson, R. E., Wiseman, S. M., & Zuber, M. T. (2010).

  Early Mars hydrology: Meridiani playa deposits and the sedimentary record of Arabia Terra

  . Journal of Geophysical Research, 115(E6). doi:10.1029/2009je003485
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  United States. National Aeronautics and Space Administration (NASA Mars Data Analysis Program)
• Evans, A. J., Andrews-hanna, J. C., Evans, A. J., & Zuber, M. T. (2010).

  Geophysical limitations on the erosion history within Arabia Terra

  . Journal of Geophysical Research, 115(E5). doi:10.1029/2009je003469
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  [1] The Arabia Terra region, an area of ∼1 × 107 km2 lying south of the hemispheric dichotomy boundary and centered at (25E, 5N), is a unique physiographic province with topography and crustal thickness intermediate between those of the southern highlands and northern lowlands. Previous workers have identified numerous morphological indicators suggestive of erosion. Using altimetry data returned by the Mars Orbiter Laser Altimeter (MOLA) on the Mars Global Surveyor (MGS) along with gravity data from the Mars Reconnaissance Orbiter (MRO), we place geophysical constraints on the amount of erosion permitted within Arabia Terra. Admittance estimates using a multitaper, spatiospectral localization approach provide a best fit to the observations through degree 50 at an elastic lithosphere thickness of 15 km. The elevation difference between Arabia Terra and the highlands would require as much as 5 km of erosion in certain areas to yield the current topography, neglecting the effects of subsequent flexure. However, incorporating flexural rebound requires substantially more erosion, up to 25 km, in order to reproduce the elevation and crustal thickness deficit of Arabia Terra. Such a large amount of erosion would result in exterior flexural uplift surpassing 1 km and gravity anomalies exceeding observations by ∼60 mGal. Consequently, it is unlikely that Arabia Terra was formed from surface erosion alone. We determine that no more than 3 × 107 km3 of material could have been removed from Arabia Terra, while 1.7 × 108 km3 of erosion is required to explain the observed crustal thickness.
• Andrews-hanna, J. C. (2009).

  Planetary science: A mega-landslide on Mars

  . Nature Geoscience, 2(4), 248-249. doi:10.1038/ngeo483
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  The vast Thaumasia plateau on Mars is fringed by extensive zones of deformation. Topographic and structural analysis suggests that the plateau may have slipped in a massive landslide, deforming its margins in the process.
• Andrews-hanna, J. C., Arvidson, R. E., Bibring, J., Bishop, J. L., Lichtenberg, K. A., Milliken, R. E., Morris, R. V., Murchie, S. L., Mustard, J. F., Parente, M., Roach, L. H., Seelos, F. P., & Wiseman, S. M. (2009).

  Evidence for the origin of layered deposits in Candor Chasma, Mars, from mineral composition and hydrologic modeling

  . Journal of Geophysical Research, 114. doi:10.1029/2009je003343
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  [1] New results from the Compact Reconnaissance Imaging Spectrometer for Mars and High Resolution Imaging Science Experiment and Context Imager cameras on Mars Reconnaissance Orbiter provide insights into the origin of interior layered deposits in Valles Marineris from analysis of a thick, well-exposed section in western Candor Chasma. Most of the deposit is dominated spectrally by nanophase ferric oxide like that found in the globally distributed eolian dust, with the addition of a prevalent component of monohydrated sulfates. A rippled mantle containing both pyroxene and monohydrated sulfate emanates from discrete layers, which are interpreted as interbedded basaltic sand. Ferric minerals are observed in most of the sulfate-rich layers, and locally a coarse-grained grayer component has been concentrated from the layers by sorting. Polyhydrated sulfates are concentrated in discrete layers high in the section, implying chasma-scale changes in brine chemistry during formation of the layered deposits. Hydrological models were constructed in order to assess whether evaporite deposition from groundwater discharge could have trapped eolian sediments to form the observed deposits. The predicted thickness and extent of the evaporite-trapped sediment is consistent with the distribution of interior layered deposits in Candor Chasma as well as in other chasmata of Valles Marineris. In this scenario, eolian dust and sand were trapped and lithified by evaporites formed by evaporation of groundwater discharge that was highly localized within the chasmata. Sulfates precipitated in the resulting saline conditions, and diagenetic alteration formed crystalline ferric minerals including hematite. This model links the layered deposits in Valles Marineris and those in Meridiani Planum to a common regional process.
• Andrews-hanna, J. C., Banerdt, W. B., & Zuber, M. T. (2008).

  The Borealis basin and the origin of the martian crustal dichotomy.

  . Nature, 453(7199), 1212-5. doi:10.1038/nature07011
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  The most prominent feature on the surface of Mars is the near-hemispheric dichotomy between the southern highlands and northern lowlands. The root of this dichotomy is a change in crustal thickness along an apparently irregular boundary, which can be traced around the planet, except where it is presumably buried beneath the Tharsis volcanic rise. The isostatic compensation of these distinct provinces and the ancient population of impact craters buried beneath the young lowlands surface suggest that the dichotomy is one of the most ancient features on the planet. However, the origin of this dichotomy has remained uncertain, with little evidence to distinguish between the suggested causes: a giant impact or mantle convection/overturn. Here we use the gravity and topography of Mars to constrain the location of the dichotomy boundary beneath Tharsis, taking advantage of the different modes of compensation for Tharsis and the dichotomy to separate their effects. We find that the dichotomy boundary along its entire path around the planet is accurately fitted by an ellipse measuring approximately 10,600 by 8,500 km, centred at 67 degrees N, 208 degrees E. We suggest that the elliptical nature of the crustal dichotomy is most simply explained by a giant impact, representing the largest such structure thus far identified in the Solar System.
• Andrews-hanna, J. C., Hauck, S. A., & Zuber, M. T. (2008).

  Strike-slip faults on Mars: Observations and implications for global tectonics and geodynamics

  . Journal of Geophysical Research, 113(E8). doi:10.1029/2007je002980
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  [1] The tectonic evolution of Mars has been driven primarily by the interaction of Tharsis-induced loading stresses with a uniform contractional stress field, leading to global assemblages of graben and wrinkle ridges. Until recently, strike-slip faults have appeared to be largely absent from the tectonic record. We here present evidence for a new set of Noachian to Early Hesperian strike-slip faults southwest of Tharsis. The best-preserved fault in the newly mapped set has a length of ∼200 km and measured lateral offset of 5–9 km. We use the locations of both previously mapped and newly identified strike-slip faults to investigate the tectonic and geodynamic evolution of Mars. We model the tectonic evolution of the planet in response to the evolving balance between the loading and contractional stresses, finding widespread regions in which strike-slip faulting was favored. The observed tectonic history is consistent with a scenario in which loading-induced stresses peaked early in Mars history, followed by the growth of contractional stresses, leading to a shift in the preferred locus of strike-slip faulting from regions southwest of Tharsis in the Noachian to Early Hesperian, to northwest of Tharsis in the Early Amazonian. The contractional strain history inferred from the ages and locations of the strike-slip faults is consistent with the strains calculated from models of the thermal evolution of Mars in which the gradual secular cooling of the planet over time was augmented by plume-induced contraction during Tharsis formation in the Noachian.
• Morris, R. V., Ollila, A. M., Andrews-hanna, J. C., Arvidson, R. E., Clark, R. N., Dobrea, E. Z., Lanza, N. L., Marais, D. J., Marzo, G. A., Morris, R. V., Murchie, S. L., Newsom, H. E., Ollila, A. M., Poulet, F., Roush, T. L., Seelos, F. P., Swayze, G. A., & Wiseman, S. M. (2008).

  Phyllosilicate and sulfate‐hematite deposits within Miyamoto crater in southern Sinus Meridiani, Mars

  . Geophysical Research Letters, 35(19). doi:10.1029/2008gl035363
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  [1] Orbital topographic, image, and spectral data show that sulfate- and hematite-bearing plains deposits similar to those explored by the MER rover Opportunity unconformably overlie the northeastern portion of the 160 km in diameter Miyamoto crater. Crater floor materials exhumed to the west of the contact exhibit CRISM and OMEGA NIR spectral signatures consistent with the presence of Fe/Mg-rich smectite phyllosilicates. Based on superposition relationships, the phyllosilicate-bearing deposits formed either in-situ or were deposited on the floor of Miyamoto crater prior to the formation of the sulfate-rich plains unit. These findings support the hypothesis that neutral pH aqueous conditions transitioned to a ground-water driven acid sulfate system in the Sinus Meridiani region. The presence of both phyllosilicate and sulfate- and hematite-bearing deposits within Miyamoto crater make it an attractive site for exploration by future rover missions.
• Andrews-hanna, J. C., & Phillips, R. J. (2007).

  Hydrological modeling of outflow channels and chaos regions on Mars

  . Journal of Geophysical Research, 112(E8). doi:10.1029/2006je002881
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  [1] The Martian outflow channels were carved by the eruption of catastrophic floods from groundwater aquifers. This study models the time evolution of a typical outflow channel flood originating within a chaos region. The flood initiates when superlithostatic pore pressures within a confined aquifer lead to the propagation of hydrofractures through the confining cryosphere to the surface. The peak discharges are modulated by diffusion of the flood pulse within the chaos region, resulting in a rapid rise in discharge immediately after flood initiation. Later flow is limited by diffusion through the aquifer and is sensitive to the variation of the hydraulic properties with changing pore pressure. After the termination of the flood by freezing within the chaos region much of the aquifer remains pressurized. Diffusion of the excess pressure from the undrained portions of the aquifer back toward the chaos region triggers a second flood, ultimately resulting in a periodic series of floods. For Iani Chaos at the source of Ares Valles, modeled peak discharges on the order of 106 to 107 m3 s−1 were obtained, with total volumes of individual floods ranging from 600 to 5000 km3 and a minimum period between successive floods of ∼44 years. The cumulative flood volume depends upon the number of floods, which is a function of the volume of pressurized aquifer or the duration of recharge from distant sources. These results suggest that individual channels were likely carved by large numbers of floods and were unlikely to have experienced bankfull flow in their final state.
• Andrews-hanna, J. C., Asmar, S. W., Konopliv, A. S., Lemoine, F. G., Phillips, R. J., Plaut, J. J., Smith, D. E., Smrekar, S. E., & Zuber, M. T. (2007).

  Density of Mars' south polar layered deposits.

  . Science (New York, N.Y.), 317(5845), 1718-9. doi:10.1126/science.1146995
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  Both poles of Mars are hidden beneath caps of layered ice. We calculated the density of the south polar layered deposits by combining the gravity field obtained from initial results of radio tracking of the Mars Reconnaissance Orbiter with existing surface topography from the Mars Orbiter Laser Altimeter on the Mars Global Surveyor spacecraft and basal topography from the Mars Advanced Radar for Subsurface and Ionospheric Sounding on the Mars Express spacecraft. The results indicate a best-fit density of 1220 kilograms per cubic meter, which is consistent with water ice that has approximately 15% admixed dust. The results demonstrate that the deposits are probably composed of relatively clean water ice and also refine the martian surface-water inventory.
• Andrews-hanna, J. C., Phillips, R. J., & Zuber, M. T. (2007).

  Meridiani Planum and the global hydrology of Mars.

  . Nature, 446(7132), 163-6. doi:10.1038/nature05594
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  The Opportunity Mars Exploration Rover found evidence for groundwater activity in the Meridiani Planum region of Mars in the form of aeolian and fluvial sediments composed of sulphate-rich grains. These sediments appear to have experienced diagenetic modification in the presence of a fluctuating water table. In addition to the extensive secondary aqueous alteration, the primary grains themselves probably derive from earlier playa evaporites. Little is known, however, about the hydrologic processes responsible for this environmental history-particularly how such extensive evaporite deposits formed in the absence of a topographic basin. Here we investigate the origin of these deposits, in the context of the global hydrology of early Mars, using numerical simulations, and demonstrate that Meridiani is one of the few regions of currently exposed ancient crust predicted to have experienced significant groundwater upwelling and evaporation. The global groundwater flow would have been driven primarily by precipitation-induced recharge and evaporative loss, with the formation of the Tharsis volcanic rise possibly playing a role through the burial of aquifers and induced global deformation. These results suggest that the deposits formed as a result of sustained groundwater upwelling and evaporation, rather than ponding within an enclosed basin. The evaporite formation coincided with a transition to more arid conditions that increased the relative impact of a deep-seated, global-scale hydrology on the surface evolution.

Proceedings Publications

• Andrews-Hanna, J., Evans, A., & Mallik, A. (2023, mar). Forming the Lunar Asymmetries. In LPI Contributions, 2806.
• Bjonnes, E., Johnson, B., Andrews-Hanna, J., Garrick-Bethell, I. .., Kiefer, W., Broquet, A., & Wakita, S. (2023, mar). Excavation of Apollo Samples 76535 and 78235 During the Formation of the Serenitatis Basin: Implications for the Formation Age of the Basin. In LPI Contributions, 2806.
• Broquet, A., & Andrews-Hanna, J. (2023). "Is There an Active Mantle Plume Beneath Elysium Planitia?", bookti Pluto.
• Broquet, A., & Andrews-Hanna, J. (2023, mar). The Moon Without Mare. In LPI Contributions, 2806.
• Levin, J., Evans, A., Andrews-Hanna, J. .., & Daubar, I. (2023, mar). Bounding and Contextualizing Vertical Distribution of KREEP in the Moon's Upper Crust. In LPI Contributions, 2806.
• Liang, W., Broquet, A., Andrews-Hanna, J., Zhang, N., Ding, M., & Evans, A. (2023, mar). Vestiges of a Lunar Ilmenite Layer Revealed by GRAIL Gravity Data. In LPI Contributions, 2806.
• Moitra, P., Mallik, A., Barnes, J., & Andrews-Hanna, J. (2023, mar). Effects of C-O-H Degassing and Bubble Growth on Explosive Lunar Volcanic Eruptions Eruptions. In LPI Contributions, 2806.
• Moruzzi, S., Andrews-Hanna, J., & Schenk, P. (2023, mar). Structure and Geophysical Evolution of Sputnik Basin on Pluto. In LPI Contributions, 2806.
• Nunes, D., Smrekar, S., Hensley, S., Adeli, S., Andrews-Hanna, J. .., Buczkowski, D., Campbell, B., Dyar, M., Gilmore, M., Helbert, J., Herrick, R., Horn, R., Jozwiak, L., Keller, M., Leeb, D., Mazarico, E., Mueller, N., Pedersen, G., Schulte, M., , Stock, J., et al. (2023, mar). Seeking Venus on Earth: The VERITAS/DLR Analog Field Campaign. In LPI Contributions, 2806.
• Smrekar, S., Hensley, S., Dyar, M., Whitten, J., Nunes, D., Helbert, J., Iess, L., Mazarico, E., Andrews-Hanna, J. .., Breuer, D., Buczkowski, D., Campbell, B., Davaille, A., DiAchille, G., Fassett, C., Gilmore, M., Herrick, R., Jozwiak, L., Kataria, T., , Konopliv, A., et al. (2023, jan). VERITAS (Venus Emissivity, Radio Science, InSAR, Topography, and Spectroscopy: Surface Science Objectives. In LPI Contributions, 2807.
• Andrews-Hanna, J., Moruzzi, S., & Kiefer, W. (2022, mar). Ridge Belts on Venus: A Thrust-Faulting Model of Vedma Dorsa. In 53rd Lunar and Planetary Science Conference, 2678.
• Bjonnes, E., Johnson, B., Andrews-Hanna, J., Garrick-Bethell, I. .., & Kiefer, W. (2022, aug). Excavation of Lightly Shocked Deep Lunar Material During Crater Collapse. In LPI Contributions, 2695.
• Cryder, M., & Andrews-Hanna, J. (2022, mar). Morphology and Subsurface Structure of Wrinkle Ridges on Mars. In 53rd Lunar and Planetary Science Conference, 2678.
• Horvath, D., & Andrews-Hanna, J. (2022, mar). The Climate and Hydrology of the Jezero Crater Paleolake. In 53rd Lunar and Planetary Science Conference, 2678.
• Horvath, D., Andrews-Hanna, J., Newman, C., & Lian, Y. (2022, mar). The Influence of Complex Hydrogeology on Lake Formation at the North and South Polar Regions of Titan. In 53rd Lunar and Planetary Science Conference, 2678.
• Broquet, A., & Andrews-Hanna, J. (2021, mar). Plume-Induced Flood Basalts on Hesperian Mars: An Investigation of Hesperia Planum. In 52nd Lunar and Planetary Science Conference.
• Horvath, D., Andrews-Hanna, J., Newman, C., & Lian, Y. (2021, mar). Comparative Hydrology of the North and South Polar Regions of Titan. In 52nd Lunar and Planetary Science Conference.
• Liang, W., & Andrews-Hanna, J. (2021, mar). Exploring the Source of the Lunar Linear Gravity Anomalies. In 52nd Lunar and Planetary Science Conference.
• Moitra, P., Horvath, D., & Andrews-Hanna, J. (2021, mar). Roles of Magmatic Volatile, Ground Ice, and Impact Triggering on the Dynamics of the Most Recent Explosive Volcanic Eruption on Mars. In 52nd Lunar and Planetary Science Conference.
• Moruzzi, S., Andrews-Hanna, J., & Schenk, P. (2021, mar). Constraining the Compensation State, Structure, and Geophysical Evolution of Sputnik Basin on Pluto. In 52nd Lunar and Planetary Science Conference.
• Smrekar, S., Andrews-Hanna, J., Breuer, D., Byrne, P., Buczkowski, D., Campbell, B., Davaille, A., Dyar, D., Di Achille, G., Fassett, C., Gilmore, M., Grimm, R., Helbert, J., Hensley, S., Herrick, R., Iess, L., Jozwiak, L., Katiaria, T., Mastrogiuseppe, M., , Mazarico, E., et al. (2021, may). Habitability, Geodynamics, and the Case for Venus. In Bulletin of the American Astronomical Society, 53.
• Smrekar, S., Hensley, S., Dyar, M., Helbert, J., Andrews-Hanna, J. .., Breuer, D., Buczkowski, D., Campbell, B., Davaille, A., Fasset, C., Gilmore, M., Herrick, R., Iess, L., Jozwiak, L., Kataria, T., Konopliv, A., Mastrogiuseppe, M., Mazerico, E., Mueller, N., , Nunes, D., et al. (2021, mar). VERITAS (Venus Emissivity, Radio Science, In-SAR, Topography, and Spectroscopy): A Proposed Discovery Mission. In 52nd Lunar and Planetary Science Conference.
• Andrews-Hanna, J. (2020, mar). The Incomplete Record of Tectonic Strain on Mars. In Lunar and Planetary Science Conference.
• Hood, L., Oliveira, J., Andrews-Hanna, J. .., Wieczorek, M., & Stewart, S. (2020, mar). Magnetic Anomalies in Lunar Impact Basins: Implications for Impactor Trajectories. In Lunar and Planetary Science Conference.
• Horvath, D., & Andrews-Hanna, J. (2020, mar). The Influence of Climate and Sedimentation on the Depositional Environment Within Gale Crater, Mars: Implications for the Sedimentary Sequence Observed by Curiosity. In Lunar and Planetary Science Conference.
• Horvath, D., Andrews-Hanna, J., & Newman, C. (2020, mar). The Hydrology of the South Polar Region of Titan. In Lunar and Planetary Science Conference.
• Liang, W., & Andrews-Hanna, J. (2020, mar). Looking Deeper into the Linear Gravity Gradient Anomalies on the Moon. In Lunar and Planetary Science Conference.
• Moitra, P., Andrews-Hanna, J., & Horvath, D. (2020, mar). Exploring the Mechanism Behind the Most Recent Explosive Volcanic Eruption on Mars: Volatile Source and Impact Triggering. In Lunar and Planetary Science Conference.
• Smrekar, S., Hensley, S., Dyar, M., Helbert, J., Andrews-Hanna, J. .., Breuer, D., Buczkowski, D., Campbell, B., Davaille, A., DiAchille, G., Fassett, C., Gilmore, M., Herrick, R., Iess, L., Jozwiak, L., Konopliv, A., Mastrogiuseppe, M., Mazerico, E., Mueller, N., , Nunes, D., et al. (2020, mar). Veritas (Venus Emissivity, Radio Science, Insar, Topography, and Spectroscopy): A Proposed Discovery Mission. In Lunar and Planetary Science Conference.
• Andrews-Hanna, J. (2019, December). Subsurface hydrology and water-rock interactions on early Mars. In American Geophysical Union Fall Meeting, P54C-05.
• Andrews-Hanna, J. (2019, Mar). A Taxonomy of Wrinkle Ridges on Mars. In Lunar and Planetary Science Conference.
• Bjonnes, E., Johnson, B., & Andrews-Hanna, J. (2019, Mar). Exploring the Peak-Ring to Multiring Basin Transition on the Moon. In Lunar and Planetary Science Conference.
• Horvath, D., Moitra, P., & Andrews-Hanna, J. (2019, Mar). A Late-Amazonian Phreatomagmatic Tephra Deposit in Elysium Planitia, Mars. In Lunar and Planetary Science Conference.
• Moitra, P., Horvath, D., & Andrews-Hanna, J. (2019, Mar). Explosive Magma-Water Interaction on Mars: Insight from a Young Pyroclastic Deposit in Elysium Planitia. In Lunar and Planetary Science Conference.
• Andrews-Hanna, J. (2018, mar). Ring Faults and Ring Dikes Around Lunar Basins. In Lunar and Planetary Science Conference, 49.
• Evans, A., & Andrews-Hanna, J. (2018, mar). Mars Habitability and the Significance of Obliquity-Driven Coupling of Magmatism and Ice Deposition: A Case Study at Olympus Mons. In Lunar and Planetary Science Conference, 49.
• Evans, A., Tikoo, S., & Andrews-Hanna, J. (2018, mar). The Lunar Core Dynamo Energy Dilemma. In Lunar and Planetary Science Conference, 49.
• Horvath, D., & Andrews-Hanna, J. (2018, mar). "The Thickness and Morphology of a Young Pyroclastic Deposit in Cerberus Palus, Mars: Implications for the Formation Sequence". In Lunar and Planetary Science Conference, 49.
• Andrews-Hanna, J. (2017, mar). A Very Recent Pyroclastic Eruption from the Cerberus Fossae on Mars. In Lunar and Planetary Science Conference, 48.
• Andrews-Hanna, J., & Bottke, W. (2017, oct). Mars During the Pre-Noachian. In LPI Contributions, 2014, 3078.
• Andrews-Hanna, J., & Soto, A. (2017, mar). Climatic Control Over Explosive Volcanism on Mars. In Lunar and Planetary Science Conference, 48.
• Andrews-Hanna, J., Weber, R., Ishihara, Y., Kamata, S., Keane, J., Kiefer, W., Matsuyama, I., Siegler, M., & Warren, P. (2017, may). Structure and Evolution of the Lunar Interior. In New Views of the Moon 2 - Europe, 1988.
• Evans, A., Andrews-Hanna, J., Soderblom, J., Solomon, S., & Zuber, M. (2017, mar). Insights into Early Lunar Chronology from GRAIL Data. In Lunar and Planetary Science Conference, 48.
• Horvath, D., & Andrews-Hanna, J. (2017, mar). Implications for the Past Climate and Hydrogeology at Gale Crater, Mars from Hydrological Modeling of Lakes. In Lunar and Planetary Science Conference, 48.
• Horvath, D., & Andrews-Hanna, J. (2017, oct). Reconstructing the Paleo-Climate and Hydrology of Gale Crater, Mars in the Late Noachian and Hesperian Epochs. In LPI Contributions, 2014, 3069.
• James, P., Andrews-Hanna, J., & Zuber, M. (2017, mar). What GRAIL Teaches Us About Error and Bias in Preliminary Gravity Fields. In Lunar and Planetary Science Conference, 48.
• Johnson, B., Andrews-Hanna, J., Collins, G., Freed, A., Melosh, H., & Zuber, M. (2017, mar). Multiring Basin Formation: Controls on Ring Location and Spacing. In Lunar and Planetary Science Conference, 48.
• Mazarico, E., Iess, L., Marchi, F., Andrews-Hanna, J., & Smrekar, S. (2017, nov). Advancing Venus Geophysics with the NF4 Venus Origins Explorer (VOX) Gravity Investigation. In LPI Contributions, 2061, 8003.
• Soto, A., Andrews-Hanna, J., & Horvath, D. (2017, jan). Progress in Climate/Groundwater Modeling of Ancient Mars. In The Mars Atmosphere: Modelling and observation.
• Andrews-Hanna, J. (2016, may). Re-Evaluating the Geophysical Evidence for a Procellarum Impact Basin on the Lunar Nearside. In New Views of the Moon 2, 1911.
• Andrews-Hanna, J., & Bottke, W. (2016, mar). The Post-Accretionary Doldrums on Mars: Constraints on the Pre-Noachian Impact Flux. In Lunar and Planetary Science Conference, 47.
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