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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 55 records · Page 3
All sourcesNASA NTRSDOE OSTI
DOE OSTI2015

Point kinetics and coupled neutron transport - CFD modeling of criticality excursions in fissile solutions - 14584

The UK version of the CRITEX code is used to analyze criticality transients in Uranyl nitrate fissile solutions in the TRACY experimental facility. The CRITEX model consists of a point kinetics model of neutronic behavior coupled to a 1D thermal hydraulic model of a cylindrical system. The model is found to estimate the magnitude of the first power peak well. It is also found to be capable of representing subsequent oscillations if the bubble rise speed is suitably adjusted. The need to adjust the rise speed prevents the code from having a fully predictive capability, however with appropriate benchmarking the code is a useful tool for parametric studies. Imperial College's FETCH code consists of a coupling of the EVENT transient radiation transport code to the FLUIDITY CFD code. The EVENT code is an even parity Pn code for transient neutron and photon transport. The FLUIDITY code is a CFD code capable of handling multi-phase fluid flows in 2D and 3D. This includes modeling of the nucleation, growth and transport of radiolytic gas bubbles. The FETCH code is used to model axisymmetric transients in fissile solutions in the TRACY experimental facility. The use of a 2D CFD calculation allows inhomogeneous phenomena to be studied. The power is found to be deposited heterogeneously in the fluid, resulting in an inhomogeneous distribution of radiolytic gas bubbles, which is subsequently homogenized by natural convection. The mechanistic modeling in the FETCH code holds the promise of a fully predictive capability for criticality excursion analysis, based on the modeling of bubble nucleation, growth and advection by the liquid. Further development of the modeling is required and this is discussed in the paper. The multi-dimensional analysis provides important insights into the transient behavior. (authors)

42 ENGINEERING↗
DOE OSTI2019

Constraining the magnitude of the carbon isotope excursion during the Paleocene-Eocene thermal maximum using larger benthic foraminifera

The Paleocene-Eocene thermal maximum (PETM) was an extraordinary pulse of global warming approximately 56 Ma. This warmingevent is associated with an addition of large amounts of 13C-depleted carbon into the atmosphere-ocean system, but the magnitude of the negative carbon isotope excursion (CIE)signaling the PETMand often used to estimate mass of the released carbonis still debated. Here we gauge the CIE magnitude usingsecondary ion mass spectrometry (SIMS) to perform in situ δ 13 C measurements within individual larger benthic foraminifera preserved in a tropical shallow marine limestone section in south Tibet. This SIMS-based δ 13 C record yields a negative CIE (Δ~7‰) comparable in magnitude to that registered by terrestrial records but larger than the ~4‰CIE returned by surface-dwelling planktonic foraminiferain deep-sea records. We therefore posit that the CIE magnitude was~7‰ in the surface ocean, and that theprevious~4‰ estimates for the CIE areattenuated by incomplete preservation and diagenetic overprinting. The large CIE magnitude in the surface ocean (~7‰) and the evidently smaller CIE magnitude registeredby deep-sea benthic foraminifera(~2-3.5‰) arelikely a function of rateand duration of carbon release as well as ocean stratification during the PETM.

58 GEOSCIENCES↗
DOE OSTI2012

STATISTICAL PROPERTIES OF THE DISK COUNTERPARTS OF TYPE II SPICULES FROM SIMULTANEOUS OBSERVATIONS OF RAPID BLUESHIFTED EXCURSIONS IN Ca II 8542 AND H{alpha}

Spicules were recently found to exist as two different types when a new class of so-called type II spicules was discovered at the solar limb with the Solar Optical Telescope on board the Hinode spacecraft. These type II spicules have been linked with on-disk observations of rapid blueshifted excursions (RBEs) in the H{alpha} and Ca II 8542 lines. Here we analyze observations optimized for the detection of RBEs in both H{alpha} and Ca II 8542 lines simultaneously at a high temporal cadence taken with the Crisp Imaging Spectropolarimeter at the Swedish Solar Telescope on La Palma. In this study, we used a high-quality time sequence for RBEs at different blueshifts and employed an automated detection routine to detect a large number of RBEs in order to expand on the statistics of RBEs. We find that the number of detected RBEs is strongly dependent on the associated Doppler velocity of the images on which the search is performed. Automatic detection of RBEs at lower velocities increases the estimated number of RBEs to the same order of magnitude expected from limb spicules. This shows that RBEs and type II spicules are indeed exponents of the same phenomenon. Furthermore, we provide solid evidence that Ca II 8542 RBEs are connected to H{alpha} RBEs and are located closer to the network regions with the H{alpha} RBEs being a continuation of the Ca II 8542 RBEs. Our results show that RBEs have an average lifetime of 83.9 s when observed in both spectral lines and that the Doppler velocities of RBEs range from 10 to 25 km s{sup -1} in Ca II 8542 and 30 to 50 km s{sup -1} in H{alpha}. In addition, we automatically determine the transverse motion of a much larger sample of RBEs than previous studies, and find that, just like type II spicules, RBEs undergo significant transverse motions of the order of 5-10 km s{sup -1}. Finally, we find that the intergranular jets discovered at Big Bear Solar Observatory are a subset of RBEs.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2013

STATISTICS OF DARK MATTER HALOS FROM THE EXCURSION SET APPROACH

We exploit the excursion set approach in integral formulation to derive novel, accurate analytic approximations of the unconditional and conditional first crossing distributions for random walks with uncorrelated steps and general shapes of the moving barrier; we find the corresponding approximations of the unconditional and conditional halo mass functions for cold dark matter (DM) power spectra to represent very well the outcomes of state-of-the-art cosmological N-body simulations. In addition, we apply these results to derive, and confront with simulations, other quantities of interest in halo statistics, including the rates of halo formation and creation, the average halo growth history, and the halo bias. Finally, we discuss how our approach and main results change when considering random walks with correlated instead of uncorrelated steps, and warm instead of cold DM power spectra.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

CHROMOSPHERIC RAPID BLUESHIFTED EXCURSIONS OBSERVED WITH IBIS AND THEIR ASSOCIATION WITH PHOTOSPHERIC MAGNETIC FIELD EVOLUTION

Chromospheric rapid blueshifted excursions (RBEs) are suggested to be the disk counterparts of type II spicules at the limb and believed to contribute to the coronal heating process. Previous identification of RBEs was mainly based on feature detection using Dopplergrams. In this paper, we study RBEs on 2011 October 21 in a very quiet region at the disk center, which were observed with the high-cadence imaging spectroscopy of the Ca II 8542 Å line from the Interferometric Bidimensional Spectrometer (IBIS). By using an automatic spectral analysis algorithm, a total of 98 RBEs are identified during an 11 minute period. Most of these RBEs have either a round or elongated shape, with an average area of 1.2 arcsec{sup 2}. The detailed temporal evolution of spectra from IBIS makes possible a quantitative determination of the velocity (∼16 km s{sup –1}) and acceleration (∼400 m s{sup –2}) of Ca II 8542 RBEs, and reveals an additional deceleration (∼–160 m s{sup –2}) phase that usually follows the initial acceleration. In addition, we also investigate the association of RBEs with the concomitant photospheric magnetic field evolution, using coordinated high-resolution and high-sensitivity magnetograms made by Hinode. Clear examples are found where RBEs appear to be associated with the preceding magnetic flux emergence and/or the subsequent flux cancellation. However, further analysis with the aid of the Southwest Automatic Magnetic Identification Suite does not yield a significant statistical association between these RBEs and magnetic field evolution. We discuss the implications of our results in the context of understanding the driving mechanism of RBEs.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

THE DYNAMICS OF RAPID REDSHIFTED AND BLUESHIFTED EXCURSIONS IN THE SOLAR Hα LINE

We analyze high temporal and spatial resolution time-series of spectral scans of the Hα line obtained with the CRisp Imaging SpectroPolarimeter instrument mounted on the Swedish Solar Telescope. The data reveal highly dynamic, dark, short-lived structures known as Rapid Redshifted and Blueshifted Excursions (RREs, RBEs) that are on-disk absorption features observed in the red and blue wings of spectral lines formed in the chromosphere. We study the dynamics of RREs and RBEs by tracking their evolution in space and time, measuring the speed of the apparent motion, line of sight (LOS) Doppler velocity, and transverse velocity of individual structures. A statistical study of their measured properties shows that RREs and RBEs have similar occurrence rates, lifetimes, lengths, and widths. They also display non-periodic, nonlinear transverse motions perpendicular to their axes at speeds of 4–31 km s{sup −1}. Furthermore, both types of structures either appear as high speed jets and blobs that are directed outwardly from a magnetic bright point with speeds of 50–150 km s{sup −1}, or emerge within a few seconds. A study of the different velocity components suggests that the transverse motions along the LOS of the chromospheric flux tubes are responsible for the formation and appearance of these redshifted/blueshifted structures. The short lifetime and fast disappearance of the RREs/RBEs suggests that, similar to type II spicules, they are rapidly heated to transition region or even coronal temperatures. We speculate that the Kelvin–Helmholtz instability triggered by observed transverse motions of these structures may be a viable mechanism for their heating.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2010

NGC 404: A REJUVENATED LENTICULAR GALAXY ON A MERGER-INDUCED, BLUEWARD EXCURSION INTO THE GREEN VALLEY

We have discovered recent star formation in the outermost portion ((1-4) x R {sub 25}) of the nearby lenticular (S0) galaxy NGC 404 using Galaxy Evolution Explorer UV imaging. FUV-bright sources are strongly concentrated within the galaxy's H I ring (formed by a merger event according to del RIo et al.), even though the average gas density is dynamically subcritical. Archival Hubble Space Telescope imaging reveals resolved upper main-sequence stars and conclusively demonstrates that the UV light originates from recent star formation activity. We present FUV, NUV radial surface brightness profiles, and integrated magnitudes for NGC 404. Within the ring, the average star formation rate (SFR) surface density ({Sigma}{sub SFR}) is {approx}2.2 x 10{sup -5} M {sub sun} yr{sup -1} kpc{sup -2}. Of the total FUV flux, 70% comes from the H I ring which is forming stars at a rate of 2.5 x 10{sup -3} M {sub sun} yr{sup -1}. The gas consumption timescale, assuming a constant SFR and no gas recycling, is several times the age of the universe. In the context of the UV-optical galaxy color-magnitude diagram, the presence of the star-forming H I ring places NGC 404 in the green valley separating the red and blue sequences. The rejuvenated lenticular galaxy has experienced a merger-induced, disk-building excursion away from the red sequence toward bluer colors, where it may evolve quiescently or (if appropriately triggered) experience a burst capable of placing it on the blue/star-forming sequence for up to {approx}1 Gyr. The green valley galaxy population is heterogeneous, with most systems transitioning from blue to red but others evolving in the opposite sense due to acquisition of fresh gas through various channels.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

Scope Complexity Options Risks Excursions (SCORE) Factor Mathematical Description.

The purpose of the Scope, Complexity, Options, Risks, Excursions (SCORE) model is to estimate the relative complexity of design variants of future warhead options, resulting in scores. SCORE factors extend this capability by providing estimates of complexity relative to a base system (i.e., all design options are normalized to one weapon system). First, a clearly defined set of scope elements for a warhead option is established. The complexity of each scope element is estimated by Subject Matter Experts (SMEs), including a level of uncertainty, relative to a specific reference system. When determining factors, complexity estimates for a scope element can be directly tied to the base system or chained together via comparable scope elements in a string of reference systems that ends with the base system. The SCORE analysis process is a growing multi-organizational Nuclear Security Enterprise (NSE) effort, under the management of the NA-12 led Enterprise Modeling and Analysis Consortium (EMAC). Historically, it has provided the data elicitation, integration, and computation needed to support the out-year Life Extension Program (LEP) cost estimates included in the Stockpile Stewardship Management Plan (SSMP).

45 MILITARY TECHNOLOGY, WEAPONRY, AND NATIONAL DEF↗
DOE OSTI2017

Scope Complexity Options Risks Excursions (SCORE) Version 3.0 Mathematical Description.

The purpose of the Scope, Complexity, Options, Risks, Excursions (SCORE) model is to estimate the relative complexity of design variants of future warhead options. The results of this model allow those considering these options to understand the complexity tradeoffs between proposed warhead options. The core idea of SCORE is to divide a warhead option into a well- defined set of scope elements and then estimate the complexity of each scope element against a well understood reference system. The uncertainty associated with estimates can also be captured. A weighted summation of the relative complexity of each scope element is used to determine the total complexity of the proposed warhead option or portions of the warhead option (i.e., a National Work Breakdown Structure code). The SCORE analysis process is a growing multi-organizational Nuclear Security Enterprise (NSE) effort, under the management of the NA- 12 led Enterprise Modeling and Analysis Consortium (EMAC), that has provided the data elicitation, integration and computation needed to support the out-year Life Extension Program (LEP) cost estimates included in the Stockpile Stewardship Management Plan (SSMP).

45 MILITARY TECHNOLOGY, WEAPONRY, AND NATIONAL DEF↗