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At least 235 records · Page 13
All sourcesNASA NTRSDOE OSTI
NASA NTRS2013

Inclusion of Linearized Moist Physics in Nasa's Goddard Earth Observing System Data Assimilation Tools

Inclusion of moist physics in the linearized version of a weather forecast model is beneficial in terms of variational data assimilation. Further, it improves the capability of important tools, such as adjoint-based observation impacts and sensitivity studies. A linearized version of the relaxed Arakawa-Schubert (RAS) convection scheme has been developed and tested in NASA's Goddard Earth Observing System data assimilation tools. A previous study of the RAS scheme showed it to exhibit reasonable linearity and stability. This motivates the development of a linearization of a near-exact version of the RAS scheme. Linearized large-scale condensation is included through simple conversion of supersaturation into precipitation. The linearization of moist physics is validated against the full nonlinear model for 6- and 24-h intervals, relevant to variational data assimilation and observation impacts, respectively. For a small number of profiles, sudden large growth in the perturbation trajectory is encountered. Efficient filtering of these profiles is achieved by diagnosis of steep gradients in a reduced version of the operator of the tangent linear model. With filtering turned on, the inclusion of linearized moist physics increases the correlation between the nonlinear perturbation trajectory and the linear approximation of the perturbation trajectory. A month-long observation impact experiment is performed and the effect of including moist physics on the impacts is discussed. Impacts from moist-sensitive instruments and channels are increased. The effect of including moist physics is examined for adjoint sensitivity studies. A case study examining an intensifying Northern Hemisphere Atlantic storm is presented. The results show a significant sensitivity with respect to moisture.

Convection↗
NASA NTRS2020

Mg Isotopic Compositions of Fine-Grained Ca-Al-Rich Inclusions from Reduced CV3 Chondrites and Implications on the Timescale of Nebular Condensation

Fine-grained Ca-Al-rich inclusions (FGIs) in carbonaceous chondrites are interpreted as aggregates of nebular gas-solid condensates that escaped significant melting [1]. Recent Al-Mg isotopic studies of small FGIs (<200 µm in size) from pristine CO3 chondrites have revealed significant variations in initial 26Al/27Al ratio, (26Al/27Al)(sub 0), spanning from 5.73×10(exp ˗5) to 8×10(exp ˗6) [2,3]. Importantly, [3] found a main CAI population characterized by (26Al/27Al)(sub 0) = 5.4×10(exp ˗5) that likely record the onset of dust condensation and initial coagulation events, followed by multiple thermal events over an extended time period. Thus far, a small number of large FGIs from CV3 chondrites have been analyzed, showing a narrower range of ( 26Al/27Al)(sub 0) = 5.27×10(exp ˗5) to 3.35×10(exp ˗5) [4-6], similar to those inferred from coarse-grained, igneous CAIs (CGIs) from CV3 chondrites [7]. These observed different ratios may raise a question if large FGIs in CV3 chondrites record a time interval from primary direct condensation of refractory solids to their aggregation and growth into larger inclusions. In this study, we present Al-Mg isotopic compositions of FGIs from reduced CV3 chondrites to better constrain their formation timescale relative to smaller FGIs in CO3 chondrites, as well as to CGIs in CV3 chondrites. This isotopic study is coordinated with a microstructural study to elucidate the origin and nature of FGIs in the petrologic and mineralogical context.

Han, J.↗
NASA NTRS2020

Mineralogy and Petrology of Fine-Grained Calcium-Aluminum-Rich Inclusions from the Reduced CV3 Chondrite Thiel Mountains 07007

Calcium-Aluminum-rich inclusions (CAIs) are among the oldest Solar System solids, and studies of these objects have played an essential role in developing an understanding of chemical and physical processes that initiated and characterized key events related to the Solar System’s formation and evolution. CAIs occur as μm- to cm-sized inclusions in chondritic meteorites, particularly in carbonaceous chondrites, and consist of various refractory silicate and oxide phases (e.g., melilite, spinel, Al-Ti-rich diopside, hibonite, and corundum) that are predicted by thermodynamic models to be among the first solids to con-dense from a cooling gas of solar composition. Fine grained CAIs (FGIs) are important samples to probe volatility-driven condensation processes in the solar nebula, because they have escaped thermal processes (e.g., melting) experienced by coarse-grained CAIs. In order to explore the primary nebular history of FGIs, a detailed mineralogical and petrologic study is necessary. In this research effort, we constrained the mineralogy and petrology of two CAIs 07-10 and -11 from the reduced CV3 chondrite Thiel Mountains (TIL) 07007, with the aim of evaluating their provenance as nebular condensates.

Anderkin, C. J.↗
NASA NTRSDate not supplied

A Record of Nebular and Parent Body Processes of Grossite-Bearing, Fine-Grained Refractory Inclusions from Reduced CV3 Chondrites

Grossite (CaAl4O7) is predicted to condense as the third major phase, after corundum and hibonite, from a cooling gas of solar composition and likely preserves an important record of physico-chemical conditions in the early Solar System. However, this mineral is relatively rare in CAIs from most carbonaceous chondrite groups, except for CH chondrites. In particular, from CV3 chondrites where CAIs are large and abundant, only six grossitebearing CAIs have been reported and studied, and most of them were coarse-grained Type A inclusions. Here, we report the occurrence of grossite-bearing, fine-grained inclusions (FGIs) from reduced CV3 chondrites. We present preliminary results of a FIB/TEM study of one grossite-bearing FGI that provide clues to constrain its formation and alteration history in the solar nebula and on the parent body and to address the overall rarity of grossite in CAIs.

J. Han↗
NASA NTRS2022

Cultivating A Culture of Inclusivity in Heliophysics

The decadal survey will help guide the Heliophysics community to create opportunities for future success. A uniquely fundamental question will drive science innovations and discoveries in the coming decades: What research environment and community will we build? The most innovative scientific ideas and discoveries develop in safe, inclusive, diverse, accessible, and collaborative environments. These environments strengthen all types of collaborations and advance innovations in concepts and applications. If we ignore this critical aspect of science, current issues regarding diversity, retention, and succession will persist. This paper discusses current critical problems and introduces actionable steps that can cultivate a culture of inclusivity.

A.J. Halford↗
NASA NTRSDate not supplied

Al-Mg Isotopic Constraints on the Condensation Age of Fine-Grained Refractory Inclusions in Reduced Cv3 Chondrites

Fine-grained Ca-Al-rich inclusions (FGIs) in carbonaceous chondrites are interpreted as aggregates of direct condensates from the solar nebula that escaped extensive melting. Thus far, a few high-precision SIMS Al-Mg chronology studies of FGIs from CV3 chondrites have been reported. Argued that (26Al/27Al)0 of all FGIs are close to the bulk refractory inclusion value of ~5.2×10−5 which may define a time zero for the FGI condensation. A similar (26Al/27Al)0 value was also inferred from an amoeboid olivine aggregate (AOA), which also represents a direct condensate from the solar nebula. In contrast, reported significant variations in (26Al/27Al)0 of FGIs, ranging from ~5.2×10−5 to ~3.4×10−5, and concluded that their formation continued over at least ~0.4 Ma after the canonical value. These contrasting results suggest that the chronological significance for the formation age spread of FGIs in CV3 chondrites is still poorly constrained.

J. Han↗
NASA NTRS2019

Grossite-Rich Refractory Inclusions in Carbonaceous Chondrites: Evidence for Early Generation of Different O-Isotope Reservoirs in the Protoplanetary Disk and O-Isotope Exchange During Fluid-Rock Interaction

The oxygen isotopic composition of the Sun inferred from the measurements of the solar wind returned by the Genesis spacecraft is O-16-enriched (△O-17 = -28.4±3.6‰) relative to the whole-rock O-isotope compositions of chondrites and achondrites, and chondrule phenocrysts, which all plot close to the terrestrial fractionation line (△O-17 ∼ ±5‰). Vast majority of refractory inclusions (CAIs and AOAs) in carbonaceous chondrites of petrologic types 2-3.0 are iso-topically uniform and have solar-like △O-17. In contrast, CAIs and AOAs in metamorphosed CV and CO chondrites are isotopically heterogeneous with melilite, anorthite, perovskite, Zr- and Sc-rich oxides and silicates, and occasionally Al, Ti-diopside being O-16-depleted relative to hibonite, spinel, Al-diopside, and forsterite. The timing of generation of different O-isotope reservoirs and the nature of O-isotope heterogeneity in refractory inclusions in CO3 and CV3 chondrites are poorly known. Grossite (CaAl4O7) is one of the first minerals predicted to condense from a gas of solar composition and therefore it could have recorded isotopic compositions of reservoirs during the earliest stages of the Solar System evolution. Here we report on O-isotope compositions of grossite-rich CAIs in CH3 and CO3 chondrites measured in situ with the UH Cameca ims-1280. For analytical procedures see [9].

A N Krot↗
NASA NTRSDate not supplied

Early History of the Solar System Revealed By Calcium-48 Heterogeneity in Calcium-Aluminium-Rich Inclusions

Introduction: Calcium-aluminum-rich inclusions (CAIs) are the earliest formed solids in the solar system. Although the mineralogy of CAIs is consistent with condensation from a solar composition gas, textural, elemental and isotopic signatures point to CAIs having more complicated thermal histories rather than simply being primary condensates. Untangling the condensation record in these refractory inclusions and the associated physicochemical environment, can provide insights into temporal and/or spatial reservoirs in the protoplanetary disk where solids were forming.

R M G Armytage↗
NASA NTRSDate not supplied

Insights Into Reconstructing REE Compositions of Melt From Zircon-Melt Partition Coefficients Using Zircon-Hosted Melt Inclusions From the Yellowstone Volcanic Province

Establishing the major and trace element composition of the Earth’s melts (Hadean to recent) is essential for understanding crustal evolution. Due to its physical-chemical resilience, zircon spans the complete age spectra of Earth’s history, and thus provides the only physical record from the early Earth. However, the petrological context i.e., the melt from which zircon crystallised, is often lost, except for inclusions of melt preserved within zircon. Melt inclusions in zircon (MI) provide a valuable tool to constrain zircon-melt REE partition coefficients (D REE ), which are used with the zircon REE chemistry to reconstruct melt compositions. Such reconstruction requires accurate partition coefficients, which are particularly sensitive to temperature, but also to pressure and melt composition. We determined the major and trace element compositions of 60 co-existing zircon-MI pairs from two ~ 2 Ma age rhyolites (the caldera-forming Huckleberry Ridge Tuff; HRT-C and the post-caldera Blue Creek Flow; BC-1) of the Yellowstone Plateau volcanic field by EPMA and SIMS, and calculated a set of 60 zircon-MI partition coefficients. The MI from both units are glassy with average silica contents of 78.30 ± 0.74 and 77.19 ± 1.11 wt %, and Ti-in-zircon crystallisation temperatures are 839 ± 36 and 835 ± 35 oC. Measured D REE patterns for each population (n = 30) are tightly constrained and exhibit a smooth pattern spanning ~ six orders of magnitude from La to Lu, (with exceptions at Ce and Eu), and for the HRT exhibit greater curvature (i.e., flatter) between the MREE to HREE compared to the BC-1. D REE patterns for the HRT have small to moderate Ce anomalies (Ce/Ce* Di 50 ± 40), whereas those in the BC-1 are larger (98 ± 45), and both units exhibit negligible to positive Eu anomalies (Eu/Eu* Di 1.07 ± 0.89 and 1.80 ± 2.01, respectively). We compare the trace element compositions of the MI to bulk-glass compositions from Yellowstone to assess any differences, which are small, then compare the measured MI compositions to those reconstructed using published partition coefficients (natural, empirical and experimental). The choice of D REE for reconstruction of the melt REE pattern results in differing petrogenetic interpretations.

Laura J. Crisp↗
NASA NTRS1994

Optimal Low Thrust Trajectories Using Differential Inclusion Concepts

A direct optimization method based on differential inclusion concepts has been developed and used to compute low thrust trajectories. This new formulation removes explicit control dependence from the problem statement thereby reducing the dimension of the parameter space of the resulting nonlinear programming problem. A simple example of a two-dimensional gravity-free trajectory involving a maximum velocity transfer to a rectilinear path is discussed. Three interplanetary trajectory examples, an Earth-Mars constant specific impulse transfer, and Earth-Jupiter constant specific impulse transfer, and an Earth-Venus-Mars variable specific impulse gravity assist, are also included. An analysis of the technique's performance is provided.

low↗
NASA NTRS1994

(abstract) Optimal Low Thrust Trajectories Using Differential Inclusion Concepts

Low thrust propulsion systems typically have their greatest benefit for high energy missions or missions with large post-launch maneuver requirements. Missions which have been examined include main belt asteroid rendezvous, comet rendezvous, outer planet and Mercury orbiters, Pluto flyby, and solar probe missions. Low thrust mission design software used to determine these trajectories is based on two distinct formulations of the optimal control problem: the indirect and direct methods. The traditional approach (indirect) is to use the calculus of variations to obtain first order necessary conditions on the states and costates. In contrast, direct methods are conceptually different in that no explicit integration takes place. A direct method based on differential inclusion concepts has been developed and successfully used to compute low thrust trajectories. This new approach removes explicit control dependence from the problem thereby reducing the dimension of the parameter space for the nonlinear programming problem. Also when compared to other direct methods, fewer nonlinear constraints are required to represent the dynamics of the problem.

low↗
NASA NTRS2018

Adrianite, Ca12(Al4Mg3Si7)O32Cl6, a New Cl-rich Silicate Mineral from the Allende Meteorite: An Alteration Phase in a Ca-Al-rich Inclusion

Adrianite (IMA 2014-028), Ca12 (Al4Mg3Si7)O32Cl6, is a new Cl-rich silicate mineral and the Si, Mg analog of wadalite. It occurs with monticellite, grossular, wadalite, and hutcheonite in altered areas along some veins between primary melilite, spinel, and Ti, Al-diopside in a Type B1 FUN (Fractionation and Unidentified Nuclear effects) Ca-Al-rich inclusion (CAI), Egg-3, from the Allende CV3 carbonaceous chondrite. The mean chemical composition of type adrianite by electron probe microanalysis is (wt%) CaO 41.5, SiO2 27.5, Al2O3 12.4, MgO 7.3, Na2O 0.41, Cl 13.0, O=Cl –2.94, total 99.2, giving rise to an empirical formula of (Ca11.69Na0.21) (Al3.85Mg2.88Si7.23) O32Cl5.80. The end-member formula is Ca12 (Mg5Si9) O32Cl6. Adrianite has the I43d wadalite structure with a = 11.981 Å, V = 1719.8 Å3, and Z = 2, as revealed by electron backscatter diffraction. The calculated density using the measured composition is 3.03 g/cm3. Adrianite is a new secondary mineral in Allende, apparently formed by alkali-halogen metasomatic alteration of primary CAI minerals such as melilite, anorthite, perovskite, and Ti,Al-diopside on the CV chondrite parent asteroid. Formation of secondary Cl-rich minerals sodalite, adrianite, and wadalite during metasomatic alteration of the Allende CAIs suggests that the metasomatic fluids had Cl-rich compositions. The mineral name is in honor of Adrian J. Brearley, mineralogist at the University of New Mexico, U.S.A., in recognition of his many contributions to the understanding of secondary mineralization in chondritic meteorites.

Adrianite↗