Search NASA⌕ Search

SEARCH · Search NASA

Results for “H- source”

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.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

At least 811 records · Page 45
All sourcesNASA NTRSDOE OSTI
DOE OSTI2011

A CANDIDATE FOR THE MOST LUMINOUS OB ASSOCIATION IN THE GALAXY

The Milky Way harbors giant H II regions, which may be powered by star complexes more luminous than any known Galactic OB association. Being across the disk of the Galaxy, however, these brightest associations are severely extinguished and confused. We present a search for one such association toward the most luminous H II region in the recent catalog by Murray and Rahman, which, at {approx}9.7 kpc, has a recombination rate of {approx}7 x 10{sup 51} s{sup -1}. Prior searches have identified only small-scale clustering around the rim of this shell-like region, but the primary association has not previously been identified. We apply a near-infrared color selection and find an overdensity of point sources toward its southern central part. The colors and magnitudes of these excess sources are consistent with O- and early B-type stars at extinctions 0.96 < A{sub K} < 1.2, and they are sufficiently numerous (406 {+-} 102 after subtraction of field sources) to ionize the surrounding H II region, making this a candidate for the most luminous OB association in the Galaxy. We reject an alternate theory, in which the apparent excess is caused by localized extinction, as inconsistent with source demographics.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2011

Operation of Negative Ion Sources at the Cooler Synchrotron COSY/Juelich

The Institute for Nuclear Physics at the Forschungszentrum Juelich is dedicated to fundamental research in the field of hadron, particle and nuclear physics. Main activities are the development of the High Energy Storage Ring for the Facility for Antiproton and Ion Research at Darmstadt and the operation and improvement of the cooler synchrotron COSY at Juelich. The injector, a cyclotron with polarized and unpolarized H{sup -} and D{sup -} sources, has exceeded 7000 hours availability per year, averaged over the last decade. Work in progress is the investigation of production, extraction and transport of the low energy 4.5 keV/u ion beams. A brief overview of the activities is presented.

43 PARTICLE ACCELERATORS↗
NASA NTRS2005

Informed Source Separation: A Bayesian Tutorial

Source separation problems are ubiquitous in the physical sciences; any situation where signals are superimposed calls for source separation to estimate the original signals. In h s tutorial I will discuss the Bayesian approach to the source separation problem. This approach has a specific advantage in that it requires the designer to explicitly describe the signal model in addition to any other information or assumptions that go into the problem description. This leads naturally to the idea of informed source separation, where the algorithm design incorporates relevant information about the specific problem. This approach promises to enable researchers to design their own high-quality algorithms that are specifically tailored to the problem at hand.

Knuth, Kevin H.↗
DOE OSTI2012

Summertime photochemistry during CAREBeijing-2007: ROx budgets and O3 formation

We analyze summertime photochemistry near the surface in Beijing, China, using a 1-D photochemical model (Regional chEmical and trAnsport Model, REAM-1D) constrained by in situ observations, focusing on the budgets of ROx (OH + HO2 + RO2) radicals and O3 formation. While the modeling analysis focuses on near-surface photochemical budgets, the implications for the budget of O3 in the planetary boundary layer are also discussed. In terms of daytime average, the total ROx primary production rate near the surface in Beijing is 6.6 ppbv per hour (ppbv h{sup 1}, among the highest found in urban atmospheres. The largest primary ROx source in Beijing is photolysis of oxygenated volatile organic compounds (OVOCs), which produces HO2 and RO2 at 2.5 ppbv h{sup 1}1 and 1.7 ppbv h{sup 1}, respectively. Photolysis of excess HONO from an unknown heterogeneous source is the predominant primary OH source at 2.2 ppbv h{sup 1}, much larger than that of O1D+H2O (0.4 ppbv h{sup 1}). The largest ROx sink is via OH + NO2 reaction (1.6 ppbv h{sup 1}), followed by formation of RO2NO2 (1.0 ppbv h{sup 1}) and RONO2 (0.7 ppbv h{sup 1}). Due to the large aerosol surface area, aerosol uptake of HO2 appears to be another important radical sink, although the estimate of its magnitude is highly variable depending on the uptake coefficient value used. The daytime average O3 production and loss rates near the surface are 32 ppbv h{sup 1} and 6.2 ppbv h{sup 1}, respectively. Assuming NO2 to be the source of excess HONO, the NO2 to HONO transformation leads to considerable O3 loss and reduction of its lifetime. Our observation-constrained modeling analysis suggests that oxidation of VOCs (especially aromatics) and heterogeneous reactions (e.g. HONO formation and aerosol uptake HO2) play potentially critical roles in the primary radical budget and O3 formation in Beijing. One important ramification is that O3 production is neither NOx nor VOC limited, but in a transition regime where reduction of either NOx or VOCs could result in reduction of O3 production. The transition regime implies more flexibility in the O3 control strategies than a binary system of either NOx or VOC limited regime. The co-benefit of concurrent reduction of both NOx and VOCs in reducing column O3 production integrated in the planetary boundary layer is significant. Further research on the spatial extent of the transition regime over the polluted eastern China is critically important for controlling regional O3 pollution.

54 ENVIRONMENTAL SCIENCES↗
DOE OSTI2015

Quartz enhanced photoacoustic H{sub 2}S gas sensor based on a fiber-amplifier source and a custom tuning fork with large prong spacing

A quartz enhanced photoacoustic spectroscopy (QEPAS) sensor, employing an erbium-doped fiber amplified laser source and a custom quartz tuning fork (QTF) with its two prongs spaced ∼800 μm apart, is reported. The sensor employs an acoustic micro-resonator (AmR) which is assembled in an “on-beam” QEPAS configuration. Both length and vertical position of the AmR are optimized in terms of signal-to-noise ratio, significantly improving the QEPAS detection sensitivity by a factor of ∼40, compared to the case of a sensor using a bare custom QTF. The fiber-amplifier-enhanced QEPAS sensor is applied to H{sub 2}S trace gas detection, reaching a sensitivity of ∼890 ppb at 1 s integration time, similar to those obtained with a power-enhanced QEPAS sensor equipped with a standard QTF, but with the advantages of easy optical alignment, simple installation, and long-term stability.

71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSIC↗
DOE OSTI2015

The radial variation of H i velocity dispersions in dwarfs and spirals

Gas velocity dispersions provide important diagnostics of the forces counteracting gravity to prevent collapse of the gas. We use the 21 cm line of neutral atomic hydrogen (H i) to study H i velocity dispersion (σ{sub H I}) and H i phases as a function of galaxy morphology in 22 galaxies from The H i Nearby Galaxy Survey. We stack individual H i velocity profiles and decompose them into broad and narrow Gaussian components. We study the H i velocity dispersion and the H i surface density, Σ{sub H I}, as a function of radius. For spirals, the velocity dispersions of the narrow and broad components decline with radius and their radial profiles are well described by an exponential function. For dwarfs, however, the profiles are much flatter. The single Gaussian dispersion profiles are, in general, flatter than those of the narrow and broad components. In most cases, the dispersion profiles in the outer disks do not drop as fast as the star formation profiles derived in the literature. This indicates the importance of other energy sources in driving σ{sub H I} in the outer disks. The radial surface density profiles of spirals and dwarfs are similar. The surface density profiles of the narrow component decline more steeply than those of the broad component, but not as steep as what was found previously for the molecular component. As a consequence, the surface density ratio between the narrow and broad components, an estimate of the mass ratio between cold H i and warm H i, tends to decrease with radius. On average, this ratio is lower in dwarfs than in spirals. This lack of a narrow, cold H i component in dwarfs may explain their low star formation activity.

79 ASTRONOMY AND ASTROPHYSICS↗
NASA NTRS1992

Warm neutral halos around molecular clouds. IV - H I and continuum: Aperture synthesis observations towards the molecular cloud B5

We present aperture synthesis observations of H I (21 cm) line radiation and continuum emission at 408 and 1420 MHz towards a field centered on the molecular cloud B5. The H I emission shows an extended atomic halo around the molecular cloud. The opacity of the halo is derived using H I absorption toward several background sources and a simple source model is presented. The model indicates that the halo is not gravitationally bound to the molecular cloud and that it is in fact expanding away from it. Approximately 350 solar masses are contained in the H I halo. Flux densities and spectral indices for the sources detected in both of the continuum bands are given.

Andersson, B.-G.↗
NASA NTRS1975

Relation of large-scale coronal X-ray structure and cosmic rays. I - Sources of solar wind streams as defined by X-ray emission and H-alpha absorption features

The large-scale structure of the corona and the interplanetary medium during Carrington rotations 1601-1607 is discussed relative to recurrent high-speed solar wind streams and their coronal sources. Only streams A, C, D, and F recur on more than one rotation. Streams A and D are associated with coronal holes, while C and F originate in the high corona (20-50 solar radii) over faint X-ray emissions. The association of the streams with holes is confirmed by earlier findings that there are no large equatorial holes without an associated high-speed stream and that the area of the equatorial region of coronal holes is highly correlated with the maximum velocity observed in the associated stream near 1 AU.

Krieger, A. S.↗
DOE OSTI2010

HIGH-RESOLUTION STUDY OF THE MASSIVE STAR-FORMING REGION IRAS 06061+2151

We present observations of 3.6 cm continuum and water maser emission toward the high-mass star-forming region IRAS 06061+2151 (AFGL 5182), made at {approx}0.''3 and {approx}0.''1 resolution, respectively, using the Very Large Array (VLA) in the A configuration. Continuum and maser emission are not detected toward the center of AFGL 5182. However, we detected two groups of continuum sources located {approx}12'' and {approx}3' to the west and northeast of AFGL 5182, respectively. The first group, labeled as the G188.79+1.03 complex, is composed of three continuum sources in a region of about 6'' x 10'', while the second group, associated with the source G188.77+1.07, is composed of at least two continuum sources in a region {approx}1'' in diameter. The physical parameters estimated, based on the morphology and the continuum emission, suggest that all the continuum sources in both groups are ultracompact H II regions, associated with ZAMS B-type stars. Water maser emission is only detected toward the compact source VLA N2, which is located in the G188.79+1.03 complex. Accuracy in the relative positions between the radio continuum source and the water masers is of the order of 15 mas. In addition, the observed spatial and kinematical distribution of the water maser features has remained stable for several years, and we confirm that they are tracing a bipolar outflow, where the best candidate of the source powering the water masers and the outflow is VLA 2N.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2014

FY 2014 Sodium-Supercritical CO 2 Interactions in the SNAKE Experiment Facility

One appealing feature of the supercritical carbon dioxide Brayton cycle energy conversion system is the small footprint that the hardware requires, which is in part due to the use of compact diffusion-bonded heat exchangers such as Printed Circuit Heat Exchanger (PCHEs) or Hybrid Heat Exchangers (H 2 X) as the heat source heat exchanger (sodium-to-CO 2 ) as well as the recuperator and cooler modules. Although PCHEs and H 2 Xs have a high degree of structural integrity, the potential for leaks to develop between the sodium and CO 2 coolant channels in the heat exchanger cannot be ruled out, and this would lead to discharge of high pressure CO 2 into the secondary coolant circuit. Due to the robustness of the PCHE design, catastrophic failure leading to CO 2 jet blowdown into the secondary sodium loop is not deemed likely. Rather, small cracks (or micro-leaks) may develop in which CO 2 will bleed into the secondary system at a relatively low rate and chemically react with the sodium. The goal of the sodium-CO 2 interaction tests is to gain a fundamental understanding of sodium-CO 2 interactions under prototypical conditions of compact diffusion-bonded heat exchanger failure, a fundamental understanding of self-plugging if it occurs, and the development of one-dimensional phenomenological models for the interactions between high-pressure CO 2 issuing into liquid sodium from a micro-leak across a stainless steel pressure boundary. These models will be validated using experiment data. Therefore, an experiment program at Argonne was initiated in Fiscal Year 2010 to investigate the reaction behavior between sodium and CO 2 under micro-leak conditions. Several reports have described the facility scaling rationale and design. Assembly of the SNAKE (S-CO 2 , Na Kinetics Experiment) began in Fiscal Year 2011 and was completed in July 2012. The sodium inventory in this facility consists of approximately 44 lbs (20 kg; ~21 L/5.5 gal).

21 SPECIFIC NUCLEAR REACTORS AND ASSOCIATED PLANTS↗
DOE OSTI2012

Effects of grain morphology, microstructure and dispersed metal cocatalyst on the photoreduction of water over impurity-doped LaInO{sub 3}

Graphical abstract: Grain morphology, doping of an impurity, microstructure, and metal/oxide contacts play a crucial role in the photocatalytic water decomposition activity of metal dispersed LaInO{sub 3}. Highlights: Black-Right-Pointing-Pointer LaInO{sub 3} displays two-step H{sub 2} evolution from UV-induced photoreduction of pure water. Black-Right-Pointing-Pointer Preparation-controlled particle morphology plays a key role in photoactivity. Black-Right-Pointing-Pointer Doping-induced activity enhancement relates to inter-bandgap charge trapping states. Black-Right-Pointing-Pointer Dispersion and metal/oxide contacts may govern the performance of a cocatalyst. -- Abstract: The single phase lanthanum indates doped with Ga (for La) and N (for O), i.e. La{sub 1-x}Ga{sub x}InO{sub 3} (0 {<=} x {<=} 0.2) and LaInO{sub 1-y}N{sub y} (y {approx} 0.6), exhibit significant activity for photoreduction of water; the yield of H{sub 2} produced depending on dopant, excitation source, and addition of a sacrificial reagent. The two-step H{sub 2} evolution observed for this reaction corresponds with the two distinct absorbance regimes displayed by these materials, one in UV-region due to bandgap excitation and the other in visible region arising from the transitions involving sub-bandgap donor or acceptor energy states. The photocatalytic activity of these d{sup 10} metal oxides increases on coating with a metal/metal oxide co-catalyst, gold exhibiting superior activity to Pt and NiO, irrespective of excitation source and sample composition. The preparation-controlled particle morphology, doping-induced lattice imperfections, and metal/semiconductor hetero-junctions are envisaged to play a key role in the absorption characteristics and photocatalytic water reduction activity of metal/LaInO{sub 3} nanocomposites.

36 MATERIALS SCIENCE↗
NASA NTRS1994

Comparative M-H Characteristics of 1-5 and 2-17 Type Samarium-Cobalt Permanent Magnets to 300 C

Recent consideration of the use of permanent magnets in space power converters at heat rejection temperatures exceeding 250 C and in miniature high temperature actuators is supporting a search for permanent magnets resistant to demagnetizing forces at high temperature. The present paper investigates the short-term demagnetization resistance to applied bucking fields and at temperatures up to 300 C of SmCo5 type magnets, in the form of 1-cm cubes, from several commercial sources. Quasistatic, 2nd quadrant M-H data taken at selected temperatures are the source of derived plots which are then compared to similar data for previously tested Sm2Co17 type magnets. The 1-5 magnet remanence tends to be about 1.5 kG below that of the 2-17 magnets throughout the temperature range. However, the intrinsic coercivities and M-H curve 'knee-fields' seen in particular 1-5 magnets were considerably above those seen previously in the 2-17 magnets. This superior resistance to demagnetizing fields attainable in 1-5 magnets is also illustrated by safe operating area plots based on the knee-field, the magnetic induction swing and temperature. Comments are made on the possibility that a remanence versus knee-field tradeoff can make 1-5 material competitive with 2-17 in applications where a magnet has to withstand large bucking fields at high temperature.

Niedra, Janis M.↗
DOE OSTI2013

THE ABUNDANCE, ORTHO/PARA RATIO, AND DEUTERATION OF WATER IN THE HIGH-MASS STAR-FORMING REGION NGC 6334 I

We present Herschel/HIFI observations of 30 transitions of water isotopologues toward the high-mass star-forming region NGC 6334 I. The line profiles of H{sup 16} {sub 2}O, H{sup 17} {sub 2}O, H{sup 18} {sub 2}O, and HDO show a complex pattern of emission and absorption components associated with the embedded hot cores, a lower-density envelope, two outflow components, and several foreground clouds, some associated with the NGC 6334 complex, others seen in projection against the strong continuum background of the source. Our analysis reveals an H{sub 2}O ortho/para ratio of 3 {+-} 0.5 in the foreground clouds, as well as the outflow. The water abundance varies from {approx}10{sup -8} in the foreground clouds and the outer envelope to {approx}10{sup -6} in the hot core. The hot core abundance is two orders of magnitude below the chemical model predictions for dense, warm gas, but within the range of values found in other Herschel/HIFI studies of hot cores and hot corinos. This may be related to the relatively low gas and dust temperature ({approx}100 K), or time-dependent effects, resulting in a significant fraction of water molecules still locked up in dust grain mantles. The HDO/H{sub 2}O ratio in NGC 6334 I, {approx}2 Multiplication-Sign 10{sup -4}, is also relatively low, but within the range found in other high-mass star-forming regions.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

Final Scientific/Technical Report

The potential for developing commercially viable microbial H 2 -production systems as a renewable source of biofuel has been limited by the need for an anaerobic environment to enable photobiological H 2 -production in capable bacterial and algal species. In this project, we have shown that the cyanobacterium Cyanothece sp. ATCC 51142 has the capacity for highly efficient H 2 -production under natural aerobic conditions. The marine cyanobacterium Cyanothece sp. ATCC 51142 has a diurnal metabolic cycle; photosynthesis and carbon fixation occur during daylight hours and then at night, high rates of respiration create a suboxic intracellular environment that enables O 2 -sensitive processes to occur, including N2-fixation and H 2 -production. We developed a two-stage approach to monitor H 2 -production by Cyanothece 51142. In the first stage, we grew the bacteria aerobically in an alternating 12 hour light/dark cycle. A second ‘incubation’ stage was then carried out in which we took cells from the end of a 12 hour light growth period and incubated them in air-tight vials for a further 12 hours under continuous illumination. Analysis of the headspace in the vial revealed high specific rates of H 2 -production (>150 μmol of H 2 per mg chlorophyll per hour) during this incubation period. Furthermore, the rate of H 2 -production could be enhanced by growing the cells in the presence of high levels of CO 2 or glycerol. We also confirmed that H 2 -production was mediated by the nitrogenase system found in these Cyanothece cells. Interestingly, in the absence of molecular N 2 , nitrogenase systems channel all available electrons towards H 2 -production. Accordingly, when we incubated glycerol-supplemented Cyanothece 51142 cells in the absence of N 2 , the rate of H 2 -production increased up to 467 μmol of H 2 per mg chlorophyll per hour, which is an order of magnitude greater than those rates previously observed in other wild type H 2 producing model photosynthetic microorganisms under anaerobic conditions. As glycerol and CO 2 are both abundantly available as industrial waste products, the fact that they substantially enhance aerobic H 2 -production suggests that Cyanothece 51142 is a potentially viable system for producing biohydrogen as a renewable fuel source. During this project, we have conducted a detailed systems level analysis of this interesting cyanobacterial system, and have created a rich knowledgebase for the use of Cyanothece cells as efficient biohydrogen producers in large scale.

08 HYDROGEN↗
DOE OSTI2019

The Arecibo Pisces–Perseus Supercluster Survey. I. Harvesting ALFALFA

We report a multi-objective campaign of targeted 21 cm H i line observations of sources selected from the Arecibo Legacy Fast Arecibo L-band Feed Array (ALFALFA) survey and galaxies identified by their morphological and photometric properties in the Sloan Digital Sky Survey. The aims of this program have been (1) to confirm the reality of some ALFALFA sources whose enigmatic nature suggest additional multiwavelength observations; (2) to probe the low signal-to-noise ratio (S/N) regime, below the ALFALFA reliability limit; and (3) to explore the feasibility of using optical morphology, color, and surface brightness to identify gas-rich objects in the region of the Pisces–Perseus Supercluster (PPS) whose H i fluxes are below the ALFALFA sensitivity limit at that distance. As expected, the reliability of ALFALFA detections depends strongly on the S/N of the H i line signal and its coincidence with a probable stellar counterpart identified by its optical properties, suggestive of ongoing star formation. The identification of low-mass, star-forming populations enables targeted H i line observations to detect galaxies with H i line fluxes below the ALFALFA sensitivity limits in fixed local volumes (D < 100 Mpc). The method explored here serves as the basis for extending the sample of gas-bearing objects as part of the ongoing Arecibo Pisces–Perseus Supercluster Survey (APPSS).

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2020

Square Kilometre Array Science Data Challenge 1: analysis and results

ABSTRACT As the largest radio telescope in the world, the Square Kilometre Array (SKA) will lead the next generation of radio astronomy. The feats of engineering required to construct the telescope array will be matched only by the techniques developed to exploit the rich scientific value of the data. To drive forward the development of efficient and accurate analysis methods, we are designing a series of data challenges that will provide the scientific community with high-quality data sets for testing and evaluating new techniques. In this paper, we present a description and results from the first such Science Data Challenge 1 (SDC1). Based on SKA MID continuum simulated observations and covering three frequencies (560, 1400, and 9200 MHz) at three depths (8, 100, and 1000 h), SDC1 asked participants to apply source detection, characterization, and classification methods to simulated data. The challenge opened in 2018 November, with nine teams submitting results by the deadline of 2019 April. In this work, we analyse the results for eight of those teams, showcasing the variety of approaches that can be successfully used to find, characterize, and classify sources in a deep, crowded field. The results also demonstrate the importance of building domain knowledge and expertise on this kind of analysis to obtain the best performance. As high-resolution observations begin revealing the true complexity of the sky, one of the outstanding challenges emerging from this analysis is the ability to deal with highly resolved and complex sources as effectively as the unresolved source population.

Bonaldi, A.↗
DOE OSTI2010

A CLUSTER OF COMPACT RADIO SOURCES IN W40

We present deep 3.6 cm radio continuum observations of the H II region W40 obtained using the Very Large Array (VLA) in its A and B configurations. We detect a total of 20 compact radio sources in a region of 4' x 4', with 11 of them concentrated in a band with 30'' of extent. We also present JHK photometry of the W40 cluster taken with the QUIRC instrument on the University of Hawaii 2.2 m telescope. These data reveal that 15 of the 20 VLA sources have infrared counterparts, and 10 show radio variability with periods less than 20 days. Based on these combined radio and IR data, we propose that eight of the radio sources are candidate ultracompact H II regions, seven are likely to be young stellar objects, and two may be shocked interstellar gas.

79 ASTRONOMY AND ASTROPHYSICS↗
NASA NTRS1972

Infrared objects in H II regions.

The discovery of 2-micron emission sources in NGC 2264, IC 2087, and M1-82, and of prominent infrared emission in Lk H-alpha 198 and V376 Cas is reported. Of the 25 objects found by scanning around the H II regions, less than half would appear to be late-type stars.

Allen, D. A.↗