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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 109 records · Page 6

Measurements of ${\mathrm{p}} {\mathrm{p}} \rightarrow {\mathrm{Z}} {\mathrm{Z}} $ production cross sections and constraints on anomalous triple gauge couplings at $\sqrt{s} = 13\,\text {TeV} $

The production of Z boson pairs in proton–proton (${\mathrm{p}} {\mathrm{p}} $) collisions, ${{\mathrm{p}} {\mathrm{p}} \rightarrow ({\mathrm{Z}}/\gamma ^*)({\mathrm{Z}}/\gamma ^*) \rightarrow 2\ell 2\ell '}$, where ${\ell ,\ell ' = {\mathrm{e}}}$ or ${{\upmu }}$, is studied at a center-of-mass energy of 13$\,\text {TeV}$ with the CMS detector at the CERN LHC. The data sample corresponds to an integrated luminosity of 137$\,\text {fb}^{-1}$, collected during 2016–2018. The ${\mathrm{Z}} {\mathrm{Z}} $ production cross section, $\sigma _{\text {tot}} ({\mathrm{p}} {\mathrm{p}} \rightarrow {\mathrm{Z}} {\mathrm{Z}} ) = 17.4 \pm 0.3 \,\text {(stat)} \pm 0.5 \,\text {(syst)} \pm 0.4 \,\text {(theo)} \pm 0.3 \,\text {(lumi)} \text { pb} $, measured for events with two pairs of opposite-sign, same-flavor leptons produced in the mass region ${60< m_{\ell ^+\ell ^-} < 120\,\text {GeV}}$ is consistent with standard model predictions. Differential cross sections are also measured and agree with theoretical predictions. The invariant mass distribution of the four-lepton system is used to set limits on anomalous ${\mathrm{Z}} {\mathrm{Z}} {\mathrm{Z}} $ and ${{\mathrm{Z}} {\mathrm{Z}} \gamma }$ couplings.

72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS↗

Kinetic Model of HoxEFU reduction by NADH [SWR-26-087]

This repository is used to release code generated for manuscripts on the Photosynthetic Energy Transduction core program. This code simulates the reduction of HoxEFU by NADH. The electro transfer rate constants for the simulation are specified in the .csv files. The two .csv files correspond tot he two models described in Dawson et al. Cell. Rep. Phys. Sci. 2026. The code utilizes a chemical master equation, a set of differential equations, defining the time evolution of the oxidation and reduction kinetics of NAD+, NADH, a FMN flavin, and a set of iron sulfur clusters. The kinetics of HoxEFU reduction by NADH are evaluated by numerical integration of the chemical master equation using a variable-time-step Runge-Kutta algorithm.

Dahl, Peter [National Laboratory of the Rockies (N↗

Neutron Imaging dataset for SMC 2021 data challenge

The neutron radiography (nR) dataset provides information of the neutron events as measured for the Siemens star mask using the Timepix3 detector. The recordings consist of the position (x and y axes), the time-stamp, and time-over-threshold (TOT) values of each neutron event.

Peterson, Peter↗

Deployment of ADTimePix3 areaDetector Driver at Neutron and X-ray User Facilities

TimePix3 is a 65k hybrid pixel readout chip with simultaneous Time-of-Arrival (ToA) and Time-over-Threshold (ToT) recording in each pixel*. The chip operates without a trigger signal with a sparse readout where only pixels containing events are read out. The flexible architecture allows 40 MHits/s/cm² readout throughput, using simultaneous readout and acquisition by sharing readout logic with transport logic of superpixel matrix formed using 2x4 structure. The chip ToA records 1.5625 ns time resolution. The X-ray and charged particle events are counted directly. However, indirect neutron counts use 6Li fission in a scintillator matrix, such as ZnS(Ag). The fission space-charge region is limited to 5-9 um. A photon from scintillator material excites a photocathode electron, which is further multiplied in dual-stack MCP. The neutron count event is a cluster of electron events at the chip. We report on the EPICS areaDetector** ADTimePix3 driver that controls Serval*** using json commands. The driver directs data to storage and to a real-time processing pipeline and configures the chip. The time-stamped data are stored in raw .tpx3 file format and passed through a socket where the clustering software identifies individual neutron events. The conventional 2D images are available as images for each exposure frame, and a preview is useful for sample alignment. The areaDetector driver allows integration of time-enhanced capabilities of this detector into SNS beamlines controls and unprecedented time resolution.

Gofron, Kaz↗

Identification of interstratified mica and pyrophyllite monolayers within chlorite using advanced scanning/transmission electron microscopy

Interstratified clay minerals reflect the weathering degree and record climatic conditions and the pedogenic processes in the soil. It is hard to distinguish a few layers of interstratified clay minerals from the chlorite matrix, due to their similar two-dimensional tetrahedral-octahedral-tetrahedral (TOT) structure and electron-beam sensitive nature during transmission electron microscopy (TEM) imaging. In this study, we used multiple advanced TEM techniques including low-dose high-resolution TEM (HRTEM), high-angle annular dark-field scanning transmission electron microscopy (HAADF-STEM) imaging combined with energy-dispersive spectroscopic (EDS) mapping to study interstratified layers in a chlorite sample from Changping, Beijing, China. We demonstrated an interstratified mica or pyrophyllite monolayer could be well distinguished from the chlorite matrix by projected atomic structures, lattice spacings, and chemical compositions with advanced TEM techniques. Further investigation showed two different transformation mechanisms from mica or pyrophyllite to chlorite: either a 4 A increase or decrease in the lattice spacing. Lastly, this characterization approach can be extended to the studies of other electron-beam sensitive minerals.

36 MATERIALS SCIENCE↗

Preparation of Nuclear Data Libraries for Web Release [Slides] and Tutorial for Generating Correlated Random Samples and Propagation of Uncertainty [Slides]

The first presentation discuses moving distribution of nuclear data to an online platform which allows ore frequent nuclear data updates, greater ease of acquiring nuclear data, and user flexibility in what nuclear data to download. The second presentation illustrates uncertainties without correlation, uncertainties without correlation with negative samples, uncertainties with correlation, uncertainties with a χ-like constraint, uncertainties with a Σ tot -like constraint, sampling using different distributions, and dealing with negative eigenvalues in a covariance matrix.

42 ENGINEERING↗

LANL-TAMUS Graduate Fellowship Report

The goal of this project is to conduct analysis of 147 Sm neutron transmission (n,tot) data at DICER alongside previously collected neutron capture (n,γ) data and report updated resonance parameters and spins. Measurement and analysis of neutron-capture data, without neutron transmission data, has been conducted before and showed that the gamma widths, Γ γ , and neutron widths, Γn, both deviate from the distributions predicted by well-established theory. Γ γ is expected to follow a narrow Gaussian distribution independent of energy but instead a broadening of the distribution around 350 eV incident neutron energy was observed (P. E. Koehler et al. Phys. Rev. C 108, 142502 (2012)). Γ n is predicted to follow a chi-squared distribution with one degree of freedom known as the Porter-Thomas distribution but this prediction also failed above 350 eV incident neutron energy (P. E. Koehler et al. Phys. Rev. C 76, 025804 (2007)). This project seeks to reassess this past measurement by including neutron transmission data and simultaneously analyzing them alongside the neutron capture data to extract the most accurate measure of Γ γ and Γ n ever taken for the resonances of 147 Sm and see if theory holds or fails under a more refined measurement with newer data.

73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗

Performance Validation of Endcap Timing Layer Detector Modules for CMS Phase-2 Upgrade

The High-Luminosity Large Hadron Collider (HL-LHC) will operate up to 200 simultaneous collisions per bunch crossing, which is a significant jump from the current value of about 30 collisions per bunch crossing, producing significant pileup that challenges accurate event reconstruction. To address this, the Compact Muon Solenoid (CMS) experiment is implementing the Endcap Timing Layer (ETL), a precision timing detector designed to provide timing measurements with a resolution of approximately 50 ps per hit and 35 ps per reconstructed track. This project focuses on the characterization and validation of ETL detector modules using laboratory laser test data. ETL performance is evaluated by analyzing key quantities such as Bunch Crossing Identification (BCID), Time-of-Arrival (TOA), Time-over-Threshold (TOT), Noise Stability etc. The resulting analysis provides insight into the timing performance and operational stability of ETL modules, contributing to the quality assurance process req uired before their installation in the CMS experiment and ensure that the modules can meet the long-term reliability requirements of approximately 10 years of operation without replacement.

Chipara, Munashe [Fermilab]↗

FERC Licensing Proceeding Environmental Study Determination Letter

This dataset summarized the back-and-forth of study submittals and issuances from Aldrovandi et al. (2021) for seven licensed hydropower projects presented as case studies in Aldrovandi et al. (2021), leveraging information from six of the seven case study projects documented in Pracheil et al. (2019), Sci Tot Env 687: 1245-1260. This information was mined from documents containing information on environmental studies conducted for US federal hydropower licensing. Documents included were found in the FERC eLibrary and was summarized and presented in Aldrovandi et al. (2021). A description of the types of documents used in this dataset can be found in Aldrovandi et al. (2021).

13 HYDRO ENERGY↗

FERC Licensing Proceeding Environmental Study Life Cycle

This dataset summarized the back-and-forth of study submittals and issuances from Aldrovandi et al. (2021) for seven licensed hydropower projects presented as case studies in Aldrovandi et al. (2021), leveraging information from six of the seven case study projects documented in Pracheil et al. (2019), Sci Tot Env 687: 1245-1260. This information was mined from documents containing information on environmental studies conducted for US federal hydropower licensing. Documents included were found in the FERC eLibrary and was summarized and presented in Aldrovandi et al. (2021). A description of the types of documents used in this dataset can be found in Aldrovandi et al. (2021).

13 HYDRO ENERGY↗

The realm of the galactic globular clusters and the mass of their primordial clouds

By adopting the empirical constraints related to the estimates of helium enhancement (ΔY), the present mass ratio between first and second stellar generations (M{sub 1G}/M{sub 2G}), and the actual mass of Galactic globular clusters (M {sub GC}), we envisage a possible scenario for the formation of these stellar systems. Our approach allows for the possible loss of stars through evaporation or tidal interactions and different star-formation efficiencies. In our approach, the star-formation efficiency of the first generation (ϵ {sub 1G}) is the central factor that links the stellar generations because it not only defines both the mass in stars of the first generation and the remaining mass available for further star formation, but it also fixes the amount of matter required to contaminate the second stellar generation. In this way, ϵ {sub 1G} is fully defined by the He enhancement between successive generations in a GC. We also show that globular clusters fit well within a ΔY versus M{sub 1G}/M{sub 2G} diagram that indicates three different evolutionary paths. The central one is for clusters that have not lost stars through tidal interactions from either of their stellar generations, and thus their present M {sub GC} value is identical to the amount of low-mass stars (M {sub *} ≤ 1 M {sub ⊙}) that resulted from both stellar generations. Other possible evolutions imply either the loss of first-generation stars or the combination of a low star-formation efficiency in the second stellar generation and a loss of stars from the second generation. From these considerations, we derive a lower limit to the mass (M {sub tot}) of the individual primordial clouds that gave origin to globular clusters.

79 ASTRONOMY AND ASTROPHYSICS↗

SDSS J0159+0105: a radio-quiet quasar with a centi-parsec supermassive black hole binary candidate

We report a candidate centi-parsec supermassive black hole binary (SMBHB) in the radio-quiet quasar SDSS J0159+0105 at z = 0.217. With a modified Lomb–Scargle code (GLSdeDRW) and auto-correlation analysis, we detect two significant (at P > 99%) periodic signals at ∼741 day and ∼1500 day from the 8.1 yr Catalina V-band light curve of this quasar. The period ratio, which is close to 1:2, is typical of a black hole binary system with a mass ratio of 0.05 < q < 0.8 according to recent numerical simulations. SDSS J0159+0105 has two SDSS spectroscopic observations separated by ∼10 yr. There is a significant change in the broad Hβ profile between the two epochs, which can be explained by a single broad-line region (BLR) around the binary system illuminated by the aforementioned mini-disks, or a stream of gas flowing from the circumbinary disk to one of the SMBHs. From the single BLR assumption and the orbital period t {sub orb} ∼ 1500 day, we estimate the total virial masses of M {sub SMBHB} ∼ 1.3 × 10{sup 8} M {sub ⊙}, the average distances of BLR of ∼0.04 pc (∼50 lt-day, with ±0.3 dex uncertainty), and an SMBHB separation of d = (0.01 pc)M{sub 8,tot}{sup 1/3} (T {sub rest}/3.3 yr){sup 2/3} ∼ 0.013 pc (15 lt-day). Based on analytical work, the postulated circumbinary disk has an inner radius of 2d = 0.026 pc (30 lt-day). SDSS J0159+0105 also displays unusual spectral energy distribution. The unique properties of SDSS J0159+0105 are consistent with it being a centi-parsec SMBHB.

79 ASTRONOMY AND ASTROPHYSICS↗

Einstein@Home discovery of a double neutron star binary in the PALFA survey

We report here the Einstein@Home discovery of PSR J1913+1102, a 27.3 ms pulsar found in data from the ongoing Arecibo PALFA pulsar survey. The pulsar is in a 4.95 hr double neutron star (DNS) system with an eccentricity of 0.089. From radio timing with the Arecibo 305 m telescope, we measure the rate of advance of periastron to be ω-dot =5.632(18)° yr{sup −1}. Assuming general relativity accurately models the orbital motion, this corresponds to a total system mass of M {sub tot} = 2.875(14) M{sub ⊙}, similar to the mass of the most massive DNS known to date, B1913+16, but with a much smaller eccentricity. The small eccentricity indicates that the second-formed neutron star (NS) (the companion of PSR J1913+1102) was born in a supernova with a very small associated kick and mass loss. In that case, this companion is likely, by analogy with other systems, to be a light (∼1.2 M{sub ⊙}) NS; the system would then be highly asymmetric. A search for radio pulsations from the companion yielded no plausible detections, so we cannot yet confirm this mass asymmetry. By the end of 2016, timing observations should permit the detection of two additional post-Keplerian parameters: the Einstein delay (γ), which will enable precise mass measurements and a verification of the possible mass asymmetry of the system, and the orbital decay due to the emission of gravitational waves ( P-dot {sub b}), which will allow another test of the radiative properties of gravity. The latter effect will cause the system to coalesce in ∼0.5 Gyr.

79 ASTRONOMY AND ASTROPHYSICS↗

The Late-Type Extension to MoVeRS (LaTE-MoVeRS): Proper Motion Verified Low-mass Stars and Brown Dwarfs from SDSS, 2MASS, and WISE

We present the Late-Type Extension to the Motion Verified Red Stars (LaTE-MoVeRS) catalog, containing 46,463 photometric late-type (>M5) dwarfs within the Sloan Digital Sky Survey (SDSS) footprint. Proper motions were computed for objects combining astrometry from the SDSS Data Release 12 (DR12), the Two-micron All-Sky Survey (2MASS) Point Source Catalog, and the Wide-field Infrared Survey Explorer (WISE) AllWISE data sets. LaTE-MoVeRS objects were required to have significant proper motion (μ{sub tot}≥2σ{sub μ{sub t{sub o{sub t}}}}). Using the LaTE-MoVeRS sample and Gaia Data Release 1, we estimate Gaia will be ~64% complete for very low-mass objects (>M5) in comparison to the combined SDSS+2MASS+WISE data set (i<21.3). We computed photometric distances and estimated stellar effective temperatures for the LaTE-MoVeRS catalog. The majority of the dwarfs in the sample have distances <150 pc and T{sub eff}<3000 K. Thirteen objects that have not been previously identified as nearby objects were identified within LaTE-MoVeRS with estimated photometric distances within 25 pc. We also identified one new object that has not been previously identified with a large amount of excess mid-infrared flux (2MASS J11151597+1937266). This object appears to be an L2γ at ~50 pc showing spectroscopic signs of a flaring event (e.g., strong hydrogen Balmer emission lines). This object does not exhibit kinematics similar to any known kinematic association. The LaTE-MoVeRS catalog is available through SDSS CasJobs and VizieR.

79 ASTRONOMY AND ASTROPHYSICS↗

Kiloparsec-Scale Variations in the Star Formation Efficiency of Dense Gas: The Antennae Galaxies (NGC 4038/39)

We study the relationship between dense gas and star formation in the Antennae galaxies by comparing Atacama large millimeter/submillimeter array (ALMA) observations of dense-gas tracers (HCN, HCO{sup +}, and HNC J = 1–0) with the total infrared luminosity (L {sub TIR}) calculated using data from the Herschel Space Observatory and the Spitzer Space Telescope. We compare the luminosities of our star formation rate (SFR) and gas tracers using aperture photometry and employing two methods for defining apertures. We taper the ALMA data set to match the resolution of our L {sub TIR} maps and present new detections of dense-gas emission from complexes in the overlap and western arm regions. Using Owens Valley Radio Observatory CO J = 1–0 data, we compare with the total molecular gas content, M(H{sub 2}){sub tot}, and calculate star formation efficiencies and dense-gas mass fractions for these different regions. We derive HCN, HCO{sup +}, and HNC upper limits for apertures where emission was not significantly detected, because we expect that emission from dense gas should be present in most star-forming regions. The Antennae extends the linear L{sub TIR}--L{sub HCN} relationship found in previous studies. The L{sub TIR}--L{sub HCN} ratio varies by up to a factor of ∼10 across different regions of the Antennae, implying variations in the star formation efficiency of dense gas, with the nuclei, NGC 4038 and NGC 4039, showing the lowest SFE{sub dense} (0.44 and 0.70 × 10{sup −8} yr{sup −1}). The nuclei also exhibit the highest dense-gas fractions (∼9.1% and ∼7.9%).

79 ASTRONOMY AND ASTROPHYSICS↗

η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity

Infrared observations of the dusty, massive Homunculus Nebula around the luminous blue variable η Carinae are crucial to characterize the mass-loss history and help constrain the mechanisms leading to the great eruption. We present the 2.4–670 μm spectral energy distribution, constructed from legacy Infrared Space Observatory observations and new spectroscopy obtained with the Herschel Space Observatory. Using radiative transfer modeling, we find that the two best-fit dust models yield compositions that are consistent with CNO-processed material, with iron, pyroxene and other metal-rich silicates, corundum, and magnesium-iron sulfide in common. Spherical corundum grains are supported by the good match to a narrow 20.2 μm feature. Our preferred model contains nitrides AlN and Si{sub 3}N{sub 4} in low abundances. Dust masses range from 0.25 to 0.44 M{sub ⊙}, but M{sub tot}⩾45 M{sub ⊙} in both cases, due to an expected high Fe gas-to-dust ratio. The bulk of dust is within a 5{sup ′′}×7{sup ′′} central region. An additional compact feature is detected at 390 μm. We obtain L{sub IR} = 2.96 × 10{sup 6} L{sub ⊙}, a 25% decline from an average of mid-IR photometric levels observed in 1971–1977. This indicates a reduction in circumstellar extinction in conjunction with an increase in visual brightness, allowing 25%–40% of optical and UV radiation to escape from the central source. We also present an analysis of {sup 12}CO and {sup 13}CO J = 5–4 through 9–8 lines, showing that the abundances are consistent with expectations for CNO-processed material. The [{sup 12}C ii] line is detected in absorption, which we suspect originates in foreground material at very low excitation temperatures.

79 ASTRONOMY AND ASTROPHYSICS↗

The Survey of Lines in M31 (SLIM): The Drivers of the [C ii]/TIR Variation

The ratio of the [C ii] 158 μm emission line over the total infrared emission (TIR) is often used as a proxy for the photoelectric (PE) heating efficiency (ϵ{sub PE}) of the far-ultraviolet (FUV) photons absorbed by dust in the interstellar medium. In the nearby galaxy M31, we measure a strong radial variation of [C ii]/TIR that we rule out as being due to an intrinsic variation in ϵ{sub PE}. [C ii]/TIR fails as a proxy for ϵ{sub PE}, because the TIR measures all dust heating, not just the contribution from FUV photons capable of ejecting electrons from dust grains. Using extensive multi-wavelength coverage from the FUV to far-infrared, we infer the attenuated FUV emission (UV{sub att}), and the total attenuated flux (TOT{sub att}). We find [C ii]/TIR to be strongly correlated with UV{sub att}/TOT{sub att}, indicating that, in M31 at least, one of the dominant drivers for [C ii]/TIR variation is the relative hardness of the absorbed stellar radiation field. We define ϵ{sub PE}{sup UV}, [C ii]/UV{sub att} which should be more closely related to the actual PE efficiency, which we find to be essentially constant (1.85±0.8%) in all explored fields in M31. This suggests that part of the observed variation of [C ii]/TIR in other galaxies is likely due to a change in the relative hardness of the absorbed stellar radiation field, caused by a combination of variations in the stellar population, dust opacity, and galaxy metallicity, though PE efficiency may also vary across a wider range of environments.

79 ASTRONOMY AND ASTROPHYSICS↗