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Justin Filiberto

Publications and source records attributed to Justin Filiberto.

At least 19 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS2024

Basalt Alteration in a CO 2 -SO 2 Atmosphere: Implications for Surface Processes on Venus

Venus’ surface and interior dynamics remain largely unconstrained, due in great part to the major obstacles to exploration imposed by its 470°C, 90 bar surface conditions and its thick, opaque atmosphere. Orbiter-based thermal emission data provide opportunities to characterize the surface composition of Venus. However, interpretations of such spectra depend on understanding interactions between the planet’s surface basaltic rocks and its caustic, sulfur dioxide (SO 2 )-bearing carbon dioxide (CO 2 ) atmosphere. Several studies, using remote sensing, thermodynamic modeling, and laboratory experiments, have placed constraints on basaltic alteration mineralogies and rates. Yet constraint with respect to SO 2 -mediated reactions with basalts of contrasting compositions remains incomplete. Here, we present new data from a series of gas-solid reaction experiments, in which samples of two basalt compositions were reacted in an SO 2 -bearing CO 2 atmosphere, at relevant Venus temperatures, pressure, and oxygen fugacity. We subjected reacted specimens to scanning electron microscopy (SEM) and scanning transmission electron microscopy (STEM) analyses using sample cross-sections produced with focused ion beam (FIB) milling. Surface alteration products were characterized, and their abundances estimated; subsurface cation concentrations were mapped to show depth of alteration. We demonstrate that the initial rate of reaction in our experiments is very rapid. Alkaline basalt samples are coated by (meta)thenardite (Na 2 SO 4 ) and amorphous calcium carbonate (CaCO 3 ) alteration products, and tholeiitic basalt samples are primarily covered by anhydrite (CaSO 4 ), Fe-oxide (Fe x O y : likely magnetite, Fe 3 O 4 ), and other minor phases.

Venus↗
NASA NTRS2024

Formation and Interior Evolution of Mars

The formation and earliest evolution of Mars involved core formation followed by magma ocean solidification and primordial crust formation. Here, we review the formation and early interior evolution of Mars as understood through meteorite studies. Martian meteorites exhibit ages that span the entire history of the Solar System, but most derive from compositionally distinct sources that formed early in the history of Mars. Geochemical and isotopic studies of Martian meteorites have provided critical information on Mars’ building blocks, bulk composition, and its differentiation into a core, mantle and crust. Radiogenic isotope systems provide vital insights into the petrogenesis of Martian meteorite source regions and into the nature and timescales of primordial differentiation on Mars. Application of short-lived isotope chronometers to Martian meteorites indicates that the Martian core formed early within <10 million years (Ma), while magma ocean differentiation and crust formation occurred soon thereafter, within the first tens of Ma of Solar System history. Bulk silicate Mars is variably depleted in moderately volatile elements relative to chondrites, but to a lesser extent than the Earth. The nature and evolution of more volatile elements and volatile species on Mars (e.g., H 2 O, C, S, halogens) remains an active area of investigation, but overall suggest that Mars is more enriched in volatile elements than the Moon but less than the Earth. While geochemical exploration of Mars coupled with new discoveries of Martian meteorites has provided a wealth of information, the compositional and lithologic diversity on Mars significantly exceeds that seen in the suites of Martian meteorites currently studied. This implies that our current perspective on the planet’s evolution is very likely biased, highlighting the need for future sample return missions to Mars.

Accretion↗
NASA NTRS2024

A Survey of the Severity of Mental Health Symptoms in the Planetary Science Community

There is a growing recognition of a mental health crisis within the academic and research communities. Members of the planetary science community have called for healthier work environments to improve mental well-being. As a preliminary step towards improving workplace culture, we sought to determine if the broader mental health crisis extends to planetary science and assess the severity of anxiety, depressive, and stress symptoms. Our 2022 mental health survey of the planetary science community suggests that the severity of anxiety and depressive symptoms in the community is greater than in the general US population. Further, the anxiety and depressive symptoms are more severe for graduate students and postdoctoral researchers than any other career stage. Comparing groups within planetary science, we found that anxiety, depressive, and/or stress symptoms appear greater among marginalized groups, such as women, people of color, and members of the LGBTQ+ community. A mental health problem is impacting the planetary science community. Improving well-being will promote enhanced research quality and productivity.

David Trang↗
NASA NTRS2024

Analysis of faults and pit chains in Noctis Labyrinthus: Implications for early extension and possible magmatic plumbing

Noctis Labyrinthus has been a region of disputed origin due to its complexity and poor understanding of how various processes and mechanisms may have combined to form it. The surface is an integrated record of intensive tectonic activity expressed by a multiple extended sets of dip-slip faults oriented in different directions, and thought to have acted on this region over its history. These faults are always coalescent to pits and pit chains displaying a complicated geological history in the region. To understand this geological history, we mapped the surface features in Noctis Labyrinthus using the High-Resolution Stereo Camera (HRSC) onboard Mars Express ND2 nadir channel basemaps, and we adapted the Digital Terrain Map (DTM) from the Mission Experiment Gridded Data Record (MEGDR) of Mars Orbiter Laser Altimeter (MOLA) onboard Mars Global Surveyor (MGS) for the topography. We have investigated the spatial distribution and trend of fault systems, the pit chains' morphology, and the correlation between these two types of features. Our results show three fault systems: i) NS and NNE-SSW, ii) EW and ENE-WSW, and iii) NNW-SSE and NW. The analysis of the faults trending, cross-cutting correlation and the superimposition led to identify multiple intersections between these faults that have been alongside with the reactivations of some inherited faults. We interpreted the first system of fault to be related to coeval lateral extension, generated by regional stress tensor, which is probably related to the slight bending of Valles Marineris within two phases of bidirectional extension. The second system of faults has been generated by the radial oblate stress tensor related to the formation of the small shield volcanoes in Syria Planum. However, the third system is likely related to the external driving process, probably in the Tharsis province. We classified pits in four evolutionary stages based on their morphometric attributes. We believe that the formation of the pit chains in Noctis Labyrinthus is related to a surface collapse after a pressure drop related to the magma chamber deflation associated with Syria Planum volcanic province. We propose a deformational model based on early extension and magmatic plumbing as driving processes for the formation of Noctis Labyrinthus.

Mayssa El Yazidi↗
NASA NTRS2024

Revision 1: Characterizing Basalt-Atmosphere Interactions on Venus: A Review of Thermodynamic and Experimental Results

The surface of Venus is in contact with a hot (~470° C), high pressure (92 bars), and caustic (CO 2 with S, but little H 2 O) atmosphere, which should cause progressive alteration of the crust in the form of sulfate and iron-oxide coatings; however, the exact rate of alteration and mineral species are not well constrained. Different experimental approaches, each with its own limitations, are currently being used to constrain mineralogy and alteration rate. One note is that no experimental approach has been able to fully replicate the necessary conditions and sustain them for a significant length of time. Further, geochemical modeling studies can also constrain surface alteration mineralogy, again with different assumptions and limitations. Here we review recent geochemical modeling and experimental studies to constrain the state of the art for alteration mineralogy, rate of alteration, open questions about the surface mineralogy of Venus, and what can be constrained before the fleet of missions arrive later this decade. Combining the new results confirm that basalt on the surface of Venus should react quickly and form coatings of sulfates and iron-oxides; however, the mineralogy and rate of alteration is dependent on physical properties of the protolith (including bulk composition, mineralogy, and crystallinity), as well as atmospheric composition, and surface temperature. Importantly, the geochemically modelling results show that the mineralogy is largely controlled by atmospheric oxygen fugacity, which is not well constrained for the near surface environment on Venus. Therefore, alteration experiments run over a range of oxygen and sulfur fugacities are needed across a wide range of Venus analog materials with varying mineralogy and crystallinity.

Justin Filiberto↗
NASA NTRS2021

Habitability Models for Astrobiology

Habitability has been generally defined as the capability of an environment to support life. Ecologists have beenusing Habitat Suitability Models (HSMs) for more than four decades to study the habitability of Earth fromlocal to global scales. Astrobiologists have been proposing different habitability models for some time, with lit-tle integration and consistency among them, being different in function to those used by ecologists. Habitabilitymodels are not only used to determine whether environments are habitable, but they also are used to charac-terize what key factors are responsible for the gradual transition from low to high habitability states. Here wereview and compare some of the different models used by ecologists and astrobiologists and suggest how theycould be integrated into new habitability standards. Such standards will help improve the comparison and charac-terization of potentially habitable environments, prioritize target selections, and study correlations between habit-ability and biosignatures. Habitability models are the foundation of planetary habitability science, and the synergybetween ecologists and astrobiologists is necessary to expand our understanding of the habitability of Earth,the Solar System, and extrasolar planets.

Habitability↗
NASA NTRS2021

Near-infrared Reflectance of Rocks at high Temperature: Preliminary Results and Implications for Near-infrared Emissivity of Venus's Surface

Light emitted from Venus’s surface can be viewed through spectral “windows” in its atmosphere, in the nearinfrared (NIR) around 1000 nanometer (nm) wavelengths. The NIR emissivity of Venus’s surface can constrain rock types and their weathering state; emissivities can be measured directly or calculated from reflectances. We measured the reflectances of igneous and sedimentary rocks at Venus’s surface temperature, 400 °C–500 °C at 850 and 950 nm; samples were heated in a box furnace in air, illuminated by light-emitting diodes (LEDs), and imaged with a modified charge-coupled device (CCD) camera. Reflectances were also measured at 25 °C from 350 to 1400 nm. Rock reflectances at 850 and 950 nm and 400 °C–500 °C are nearly identical to those at 25 °C, except for the effects of nanophase hematite forming on some surfaces. Fresh basalts have reflectances (high and low temperatures) near 7.5%; a leucogranite similarly has reflectances near 50%. Pigmentary hematite has nearly identical reflectances at high- and low-temperature at these wavelengths. Pigmentary hematite appears dark brown 400 °C–500 °C because its absorption edge has shifted to beyond the limit of human vision. These rock reflectances imply that basalts should have emissivities near 0.9, and granite (and similar felsic rocks) should have lower emissivities ∼0.5. Thus, basalt and felsic rock should be easily distinguished in NIR emissivity measurements of Venus’s surface, such as are baselined in recent Venus mission proposals. Other sedimentary rocks should have even lower emissivities: quartz sand at around ∼0.3, and anhydrite as low as 0.1.

Allan H Treiman↗
NASA NTRS2020

Advanced Curation of Astromaterials for Planetary Science Over the Next Decade

Advanced curation is a cross-disciplinary field of research and development aiming to improve curation and sample acquisition practices in existing astromaterials collections and to enable future sample return activities.The primary result of advanced curation is to both reduce and quantify contamination to astromaterials and preserve the scientific integrity of all samples from mission inception to scientific analysis. Over the next decade, NASA should support advanced curation research and monitoring efforts as they pertain to improving our current collections and preparing for samples from current and future astromaterials acquisition activities.We highlight here five advanced curation activities of critical importance for the success of sample science supported by NASA over the coming decade, including: 1) supporting efforts to build contamination knowledge collections as part of sample return missions, which requires curation involvement from the earliest stages of sample return mission planning;2) supporting Earth-based astromaterials collection campaigns of meteorites and cosmic dust as they represent relatively inexpensive sample acquisition activities that continue to grow NASA’s astromaterials collections and enable new discoveries;3) preparing to curate and process samples under “cold” conditions to enable return of samples from volatile-rich Solar System targets like permanently shadowed regions on the lunar surface orcomets;4) determining how best to combine clean room technology and biosafety technology into one infrastructure to support curation of samples from bodies designated as Category V:Restricted Earth Return; and 5) supporting real-time monitoring and testing of curation labs to verify that sample processing environments remain clean from the standpoint of inorganic, organic, and biological contamination

Francis M. McCubbin↗
NASA NTRSDate not supplied

Mineralogy and Spectroscopy of Mount Etna Lava Flows as an Analogue to Venus

Reports of geologically recent volcanism at Venus [1–3] raise the question of whether Venus is actively resurfacing. Observing the venusian surface is difficult due to the planet’s thick, relatively opaque atmosphere, but emission from the surface is detectable via a few atmospheric windows in the near-infrared (NIR) around 1 μm [4]. Spectroscopy of rocks at these wavelengths varies due to its primary composition and the presence of secondary weathering products [2, 5, 6]. If degree of alteration can be tied to the spectroscopic response, then the weathering of the venusian surface can reveal its age and extent of recent volcanism [2, 7]. Mount Etna on Earth is a potential analogue to Venus that can aid our understanding. The composite volcano is currently active and exhibits a progression of dated lava flows with a range of textures (‘a‘¯a versus p¯ahoehoe flows) and degrees of alteration [8]. While not a perfect analogue due to differing weathering environments, Mount Etna represents a natural age progression of altered basaltic rock [8] that can provide a useful comparison to volcanic structures on Venus. Here we will determine if spectroscopy can determine the alteration state of these flows as a proxy for their age. Future missions to Venus such as VERITAS, En- Vision, and DAVINCI will observe the surface in NIR emissivity. Kirchhoff’s Law holds that e = 1−r, where e is the emissivity and r is the reflectance. NIR emissivity can be reliably calculated from reflectance measurements of rocks [9], so laboratory reflectance spectroscopy is useful to rapidly test potential Venus analogue materials.

Gabriel L. Eggers↗
NASA NTRSDate not supplied

Boninites from Cyprus Island as Mercury Lava Analogues

Mercurian meteorites have never been found on Earth. However, thanks to the NASA’s MESSENGER mission, some constraints on the geochemistry and mineralogy of Mercurian rocks are now available. Results from the Xand Gamma-ray Spectrometers onboard the MESSENGER mission suggest a surface composition with Mg/Si ratio within 0.33-0.67 and a Fe/Si ratio within 0.03-0.15, characterized by extremely reduced (IW -6) rocks. Experimental petrology studies show that the most appropriate Mercurian rock-type should be a Mg-rich, Fe-poor basalt, mainly composed of orthopyroxene and plagioclase. Visible/near-infrared (VNIR) spectroscopy of terrestrial basalts can help contextualize acquired MESSENGER spectra. The most Mg-rich, Al-poor regions on Mercury, are suggested to be orthopyroxene-rich lavas analogous to terrestrial boninites and/or komatiites. At present, there are no studies on the geochemistry and mineralogy of boninites for their possible association with Mercurian material. In addition, there are still no information about the VNIR spectral properties of boninitic material. In this work, we investigate the VNIR and Raman spectroscopy and X-Ray Fluorescence (XRF) of a series of boninitic pillow lavas that were collected on the Upper Pillow Lavas unit of the Troodos Massif, located on the island of Cyprus. Data are then discussed in order to reveal potential classification as Mercury analog.

Nicola Mari↗
NASA NTRSDate not supplied

Comparing the Volatile Contents of Basaltic Rocks Through the Inner Solar System

Volatiles in planetary interiors play important roles in magma genesis, crust formation, eruption style, and even habitability of planetary surfaces. Allan Treiman’s career has touched on volatiles in the Moon, Mars, HED-parent body, the Earth, Venus, and other planetary bodies through studies of igneous rocks, volatile-bearing igneous minerals within these rocks, and the secondary alteration products produced from these rocks and minerals. His seminal work in many of these fields has inspired our careers and many others in our field. Here, we will build on and summarize what we know of the volatile content of basaltic rocks in the inner solar system. Specifically, this talk will focus on using volatile-bearing minerals (amphibole and apatite) along with bulk compositions to constrain the pre-eruptive, and potentially predegassed, volatile content of the magma and their source regions. We will then use these estimates to compare the volatile content of the Earth, Moon, Mars, Venus, and Mercury and what open questions there are for each planetary body.

Justin Filiberto↗
NASA NTRSDate not supplied

Phase Transitions and Melting in the Venusian Basaltic Crust: Implications for Crustal Recycling

Understanding phase transitions and melting in the Venusian crust and the associated changes in density are critical to constrain crustal thickness, recycling, and remelting processes. For example, average surface conditions on Venus of 92 bars and 460 °C correspond to low-grade metamorphic conditions on Earth equivalent to hornfels- and greenschist-facies. Further, the primary igneous mineralogy in the Venusian crust should be replaced by metamorphic minerals over time and potentially melt, as temperatures and pressures increase with depth along geothermal gradients. Here, we use Perple_X (Connolly, 2005), a Gibbs free energy minimization program to calculates table phase equilibria over a range of pressure and temperature conditions for whole-rock compositions of a dry basalt, alkali basalt, and peridotite. Further, we extract mineral abundancies along five geotherms of 5, 10, 15, 20 and 25 °C/km and calculate the rock density after the extraction of melt. On the coldest geotherm of 5 °C/km, melting would start at ~ 197 km and ~121 km in the basalt and alkali basalt, respectively, and therefore at depths that significantly exceed the estimated thickness of the Venusian crust (8-25 km). A density cross-over, where the crustal density would exceed that of the mantle could potentially induce delamination and is estimated to occur at ~ 40 km for both compositions. On the 10 °C/km geotherm, melting of the basalt starts at 65 km and melt extraction only causes a gradual densification due the formation of initially lower melt proportions. In contrast, the alkali basalt starts to melt at a depth of ~ 57 km and the subsequent densification of the residual composition could trigger delamination at ~ 60km depth. For hotter geotherms (i.e., 25 °C/km gradient), melting would occur at shallower depths of 21 – 23 km. However, the basalt will not get significantly denser than the mantle while the residuum of the alkali basalt would reach a density cross-over at 30 km. Hence, differences in Venusian crustal compositions can significantly influence the thickness of the crust on individual geotherms. Our results demonstrate that phase transitions and melting are strongly dependent on the assumed geotherm and could, combined with geodynamic models, further constrain crustal parameters.

Julia Semprich↗
NASA NTRSDate not supplied

Evidence for Present Day Volcanism on Venus: A Case Study of Idunn Mons

Idunn Mons in Imdr Regio on Venus is perhaps one of the best studied volcanoes on Venus in part due to having both radar and night-time emissivity data of the region [1-3]. Smrekar et al. [1] first presented night-time emissivity data of Idunn Mons from the VIRTIS instrument on Venus Express, which showed that some lava flows have high emissivity consistent with unweathered basalt. Smrekar et al. [1], based on known weathering rates at that time, suggested that the lava flows were less than 2.5 million years old and possible as young as 250,000 years old. However, recent experimental work has shown that basaltic rocks and associated minerals in contact with the Venusian caustic atmosphere would react quickly to produce rinds of alteration materials coating the surface and obscure emissivity signatures of igneous minerals within a few to ~10,000 years [4-9]. These new experimentally derived weathering and oxidation rates were used to suggest that lava flows at Idunn Mons with unweathered signatures are quite young and Idunn Mons may be volcanically active today [4, 8]. Independent geologic mapping and related stratigraphic reconstruction over the study area is consistent with the experimental results [2, 10]. Considering all the available evidence, we have taken a comprehensive approach combining these recent experimental results with previous orbital night-time emissivity, as well as atmospheric measurements, to constrain the evolution of Idunn Mons [3,10]. Our results suggest that Idunn Mons is both volcanically and tectonically active today, and that volcanism and tectonic activity are likely related [11]. Venus being volcanically active has been suggested at other volcanic centers, as well [e.g. 12-17]. Therefore, we use Idunn Mons specifically as a case study of a potentially active volcano that may be detectable by the upcoming fleet of missions that will be arriving at Venus in the next decade.

Justin Filiberto↗
NASA NTRSDate not supplied

Evidence for Early Extension and Pressure Drop Related to Magma Plumbing in Noctis Labyrinthus (Mars)

Noctis Labyrinthus is a complex district located between the western side of Valles Marineris’ large outflow channel and the Tharsis volcanic plateau. This region is characterized by a system of steep-walled canyons and an inter-connected network of scalloped pits that manifest in various orientations and size. The formation history of this area has been a topic of substantial discussion in the past. Previous studies have proposed a karst landscape with associated caves and water-related processes [1,2,3] a network of lava tubes [4,5], or a volcano-tectonic activity as a driving process for the formation of Noctis Labyrinthus [6,7,8,9]. However, none of these models have been confirmed or entirely accepted; although, the erosional nature of Noctis Labyrinthus is supported by the presence of channelized lava flows still visible on its floor [5]. In this work, we use MOLA and HRSC data to produce a new structural map of the region, we analyse fault systems (chronology and orientation), the relationships between faults and pit chains, and we finally propose a deformational model that can explain the sequences of events responsible about the formation of Noctis Labyrinthus.

M. El Yazidi↗
NASA NTRSDate not supplied

Spectroscopy of Mount Etna Lava Flows as A Proxy for Age: A Potential Analogue to Recent Volcanism on Venus

There is growing evidence of geologically recent volcanism at Venus [1–3], a question that may be resolved by forthcoming missions to our sister planet that will make spectroscopic measurements of the surface. The thick, relatively opaque atmosphere of Venus makes observation difficult, but a few key atmospheric windows in the near-infrared (NIR) around 1 μm make emission from the surface detectable [4]. At these wavelengths, the spectroscopic signature of rocks are due to its primary mineralogy and chemistry, as well as the presence of secondary weathering minerals [2, 5, 6]. If the degree of alteration can be tied to the spectroscopy of Venus analogue materials, then spectroscopy of venusian lava flows can potentially reveal their degree of weathering and thus their age, which in turn gives an estimate of the extent of recent volcanism [2, 7]. A potential Earth analogue to volcanoes on Venus is Mount Etna in Sicily, Italy [8]. This composite volcano is among the most active in the world and features mafic lava flows with definitive ages that exhibit varying degrees of alteration [9]. While Mount Etna is not a perfect analogue due to its different weathering environment, the natural age progression of altered basaltic rock can be a useful comparison. Here, we will investigate how weathering at Mount Etna affects spectroscopic measurements and if this can be used as a proxy for Venus. While planned missions to Venus such as DAVINCI, VERITAS, and EnVision will measure NIR emissivity from the surface, Kirchhoff’s Law states that e = 1 − r, where e is emissivity and r is reflectance, meaning that NIR emissivity can be estimated from reflectance measurements [10]. Given its relative ease, laboratory reflectance spectroscopy is a useful tool to efficiently test potential Venus analogue materials.

Gabriel L Eggers↗