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At least 253 records · Page 14
All sourcesNASA NTRSDOE OSTI
DOE OSTI2020

Materials Data on ZnH12(NO3)2 by Materials Project

ZnNHO3(H2)5HNO3 crystallizes in the monoclinic P2_1/c space group. The structure is zero-dimensional and consists of sixteen hydrogen molecules, four molecular hydrogen molecules, four nitric acid molecules, and four ZnNHO3 clusters. In each ZnNHO3 cluster, Zn2+ is bonded in a distorted linear geometry to one H1+ and one O2- atom. The Zn–H bond length is 1.51 Å. The Zn–O bond length is 1.89 Å. N1- is bonded in a trigonal planar geometry to three O2- atoms. There are a spread of N–O bond distances ranging from 1.23–1.37 Å. H1+ is bonded in a single-bond geometry to one Zn2+ atom. There are three inequivalent O2- sites. In the first O2- site, O2- is bonded in a bent 120 degrees geometry to one Zn2+ and one N1- atom. In the second O2- site, O2- is bonded in a single-bond geometry to one N1- atom. In the third O2- site, O2- is bonded in a single-bond geometry to one N1- atom.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on UH14(SeO5)2 by Materials Project

(UH3(SeO5)2)2(H2)11 crystallizes in the monoclinic P2_1/c space group. The structure is two-dimensional and consists of sixteen hydrogen molecules; four molecular hydrogen molecules; and one UH3(SeO5)2 sheet oriented in the (1, 0, 0) direction. In the UH3(SeO5)2 sheet, U4+ is bonded to seven O2- atoms to form distorted UO7 pentagonal bipyramids that share corners with three equivalent SeO4 tetrahedra and corners with two equivalent SeO4 trigonal pyramids. There are a spread of U–O bond distances ranging from 1.80–2.49 Å. There are three inequivalent H1+ sites. In the first H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 1.00 Å. In the second H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 1.01 Å. In the third H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.98 Å. There are two inequivalent Se1+ sites. In the first Se1+ site, Se1+ is bonded to four O2- atoms to form SeO4 tetrahedra that share corners with three equivalent UO7 pentagonal bipyramids. There are a spread of Se–O bond distances ranging from 1.65–1.76 Å. In the second Se1+ site, Se1+ is bonded to four O2- atoms to form distorted SeO4 trigonal pyramids that share corners with two equivalent UO7 pentagonal bipyramids. There are a spread of Se–O bond distances ranging from 1.69–1.97 Å. There are ten inequivalent O2- sites. In the first O2- site, O2- is bonded in a distorted bent 150 degrees geometry to one U4+ and one Se1+ atom. In the second O2- site, O2- is bonded in a distorted single-bond geometry to one H1+ and one Se1+ atom. In the third O2- site, O2- is bonded in a water-like geometry to one H1+ and one Se1+ atom. In the fourth O2- site, O2- is bonded in a 2-coordinate geometry to one U4+ and one Se1+ atom. In the fifth O2- site, O2- is bonded in a bent 150 degrees geometry to one U4+ and one Se1+ atom. In the sixth O2- site, O2- is bonded in a single-bond geometry to one U4+ atom. In the seventh O2- site, O2- is bonded in a distorted water-like geometry to one H1+ and one Se1+ atom. In the eighth O2- site, O2- is bonded in a distorted bent 120 degrees geometry to one U4+ and one Se1+ atom. In the ninth O2- site, O2- is bonded in a distorted bent 150 degrees geometry to one U4+ and one Se1+ atom. In the tenth O2- site, O2- is bonded in a distorted single-bond geometry to one U4+ atom.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on Fe6P4H23O21 by Materials Project

Fe6P4(H3O7)3(H2)7 crystallizes in the monoclinic C2/c space group. The structure is three-dimensional and consists of sixteen hydrogen molecules, eight molecular hydrogen molecules, and one Fe6P4(H3O7)3 framework. In the Fe6P4(H3O7)3 framework, there are four inequivalent Fe+2.50+ sites. In the first Fe+2.50+ site, Fe+2.50+ is bonded to four O2- atoms to form distorted FeO4 tetrahedra that share corners with two FeO6 octahedra, a cornercorner with one FeO4 tetrahedra, a cornercorner with one PO4 tetrahedra, and a cornercorner with one PO4 trigonal pyramid. The corner-sharing octahedra tilt angles range from 54–63°. There are a spread of Fe–O bond distances ranging from 1.97–2.09 Å. In the second Fe+2.50+ site, Fe+2.50+ is bonded to six O2- atoms to form distorted FeO6 octahedra that share a cornercorner with one FeO4 tetrahedra, corners with two equivalent PO4 tetrahedra, corners with two equivalent PO4 trigonal pyramids, and a faceface with one FeO6 octahedra. There are a spread of Fe–O bond distances ranging from 2.00–2.29 Å. In the third Fe+2.50+ site, Fe+2.50+ is bonded to six O2- atoms to form FeO6 octahedra that share corners with two equivalent FeO4 tetrahedra, corners with four equivalent PO4 tetrahedra, and faces with two equivalent FeO6 octahedra. There are a spread of Fe–O bond distances ranging from 2.02–2.11 Å. In the fourth Fe+2.50+ site, Fe+2.50+ is bonded in a square co-planar geometry to four O2- atoms. There are two shorter (1.98 Å) and two longer (2.14 Å) Fe–O bond lengths. There are two inequivalent P1+ sites. In the first P1+ site, P1+ is bonded to four O2- atoms to form PO4 tetrahedra that share corners with four FeO6 octahedra and a cornercorner with one FeO4 tetrahedra. The corner-sharing octahedra tilt angles range from 28–57°. There are a spread of P–O bond distances ranging from 1.54–1.57 Å. In the second P1+ site, P1+ is bonded to four O2- atoms to form PO4 trigonal pyramids that share corners with two equivalent FeO6 octahedra and a cornercorner with one FeO4 tetrahedra. The corner-sharing octahedra tilt angles range from 32–61°. There are a spread of P–O bond distances ranging from 1.49–1.91 Å. There are five inequivalent H1+ sites. In the first H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.98 Å. In the second H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.99 Å. In the third H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.97 Å. In the fourth H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.98 Å. In the fifth H1+ site, H1+ is bonded in a single-bond geometry to one O2- atom. The H–O bond length is 0.99 Å. There are eleven inequivalent O2- sites. In the first O2- site, O2- is bonded in a distorted single-bond geometry to two Fe+2.50+ and one H1+ atom. In the second O2- site, O2- is bonded in a bent 120 degrees geometry to one Fe+2.50+ and one P1+ atom. In the third O2- site, O2- is bonded in a distorted single-bond geometry to three Fe+2.50+ and one H1+ atom. In the fourth O2- site, O2- is bonded in a bent 150 degrees geometry to one Fe+2.50+ and one P1+ atom. In the fifth O2- site, O2- is bonded in a distorted trigonal non-coplanar geometry to one P1+ and two H1+ atoms. In the sixth O2- site, O2- is bonded in a 3-coordinate geometry to two Fe+2.50+ and one P1+ atom. In the seventh O2- site, O2- is bonded in a distorted trigonal planar geometry to two equivalent Fe+2.50+ and one H1+ atom. In the eighth O2- site, O2- is bonded in a 3-coordinate geometry to two Fe+2.50+ and one P1+ atom. In the ninth O2- site, O2- is bonded in a bent 120 degrees geometry to one Fe+2.50+ and one P1+ atom. In the tenth O2- site, O2- is bonded in a distorted bent 150 degrees geometry to one Fe+2.50+ and one P1+ atom. In the eleventh O2- site, O2- is bonded in a bent 150 degrees geometry to one Fe+2.50+ and one P1+ atom.

36 MATERIALS SCIENCE↗
NASA NTRS1973

Chemical evolution of cosmic clouds

Reaction rate characteristics of interstellar matter were studied by the reaction of hydrogen cyanide and molecular hydrogen at about 1000 K at an HCN to H2 ratio of 1 to 100 to simulate the large excess of cosmic hydrogen. It was found that HCN decays with a half life of about 20 hours and that a large surface increases the reaction rate as a function of temperature. Reaction rates may be considerable increased by energetic processes that produce free radicals and ions.

Down, B. D.↗
NASA NTRS1972

Excitation of the Werner bands of H2 by electron impact.

Absolute cross sections for the excitation of the Werner band system of molecular hydrogen have been measured from energy threshold to 300 eV for electron impact on molecular hydrogen. The bands were observed in emission in the wavelength region of 1100 to 1250 A. From a comparison of the measured cross sections with previously calculated transition probabilities, it is concluded that the Werner bands are suitable as the basis for relative spectral response calibration only when the bands are observed under sufficiently high resolution. The effect of the perturbation interaction between the B and C states of the hydrogen molecule was observed in the rotational intensity distribution of the Werner (3,7) and (3,6) bands.

Stone, E. J.↗
NASA NTRS1984

Photochemistry of porphyrins: a model for the origin of photosynthesis

A series of porphyrins and catalysts has been prepared as a model for the origin of photosynthesis on the primordial earth. These compounds have been used to test the hypotheses that (1) the biosynthetic pathway to chlorophyll recapitulates the evolutionary history of photosynthesis, and (2) the proto-photosythetic function of biogenetic porphyrins (biosynthetic chlorophyll precursors) was the oxidation of organic molecules by photoexcited porphyrins with the attendant emission of molecular hydrogen. This paper describes experiments in which photoexcited biogenetic porphyrins oxidize ethylenediamine tetraacetic acid (EDTA). The concomitant reduction of protons to hydrogen gas occurs in the presence of a colloidal platinum catalyst. The addition of methyl viologen, a one-electron shuttle, increases the amount of molecular hydrogen generated during long irradiations and the quantum yield of hydrogen production. When the porphyrin and catalyst are held in association by molecular complexes, the increased efficiency of electron transfer produces higher yields of hydrogen gas.

Hydrogen/chemistry↗
NASA NTRS1984

The Draco Nebula, a Molecular Cloud Associated with a High Velocity Cloud?

Extended and very faint bright nebulae are found in high galactic latitudes at the Palomar Observatory Sky Survey. Such a nebula, located in the constellation Draco and called Draco Nebula or Dracula, was found to be in detailed positional coincidence with a 21 cm emission line feature. Estimates of the minimum visual extinction from star counts ON and OFF Dracula and an estimated visual surface brightness indicate that Dracula fits the relation SBV = 24.2 - 2.5 log AV for dust clouds located above the galactic plane and reflecting the integrated starlight of the galactic disk. Hence Dracula is probably a reflection nebula. Indicators of molecular hydrogen in Dracula, molecules such as CO, were searched for by using a 2.5-m mm-telescope. Molecular hydrogen column densities were estimated. The dynamics of CO clumps was studied. Dracula has a close positional and possibly even astrophysical relationship to the high velocity cloud phenomenon.

Mebold, U.↗
NASA NTRS2000

NASA's Long Term Space Astrophysics Program

We have carried out a comprehensive, multiwavelength study of interstellar molecules using data obtained from the Infrared Space Observatory (ISO), the Hubble Space Telescope (HST), and the Submillimeter Wave Astronomy Satellite (SWAS). Molecular observations provide a unique probe of the astrophysical Universe and yield information of general astronomical importance that can obtained in no other way. Molecules are also of importance because they can dominate the cooling of astrophysical media. The key topics addressed by our study have been: (1) the cooling of the interstellar gas; (2) the chemistry and excitation of molecular hydrogen in shocks, diffuse molecular clouds, and X-ray heated regions; (3) the chemistry and excitation of interstellar halides in dense molecular clouds, and the discovery of interstellar hydrogen fluoride; (4) the chemistry and excitation of water vapor in shocks, circumstellar outflows, translucent molecular clouds, and dense molecular clouds; (5) future prospects for probing the high-redshift Universe with molecular and other spectroscopic observations.

Source record↗
NASA NTRS1973

Phase equilibria in molecular hydrogen-helium mixtures at high pressures

Experiments on phase behavior in hydrogen-helium mixtures have been carried out at pressures up to 9.3 kilobars, at temperatures from 26 to 100 K. Two distinct fluid phases are shown to exist at supercritical temperatures and high pressures. Both the trend of the experimental results and an analysis based on the van der Waals theory of mixtures suggest that this fluid-fluid phase separation persists at temperatures and pressures beyond the range of these experiments, perhaps even to the limits of stability of the molecular phases. The results confirm earlier predictions concerning the form of the hydrogen-helium phase diagram in the region of pressure-induced solidification of the molecular phases at supercritical temperatures. The implications of this phase diagram for planetary interiors are discussed.

Streett, W. B.↗
NASA NTRS1976

Interior models of Jupiter

Understanding the interior of Jupiter depends upon our knowledge of the thermodynamics and transport properties of hydrogen-helium mixtures at high pressures and temperatures. The current status of this knowledge is reviewed, and attention is given to the metallic-molecular hydrogen transition and the limited solubility of helium in hydrogen. Models of Jupiter are constructed which are consistent with all the observations to date, but which make various assumptions about the thermodynamics and composition of the interior. These models typically consist of a rocky core surrounded by a nearly-solar fluid mixture. In contrast to the models of Podolak and Cameron, a large enhancement of water or helium is not found to be essential. It is concluded that further progress in constructing interior models requires a better understanding of the thermodynamics of dense molecular hydrogen.

Stevenson, D. J.↗
NASA NTRS1993

A new near-infrared imaging study of AFGL 2688

The object AFGL 2688 is a bipolar nebula surrounding a post-asymptotic giant branch star and is in transition toward becoming a planetary nebula. We present new NIR images in the I, J, H, and K bandpasses. These images reveal a wealth of structure in the nebula not previously seen. We find that the northern lobe is not smooth, but clumpy. There is evidence in the I-band image for periodic variations in mass-loss rate. In addition, we present narrowband images centered on the V = 1 - 0 S(1) line of molecular hydrogen and nearby continuum. The narrowband images reveal that broadband flux found in the equatorial region is dominated by line emission from vibrationally excited molecular hydrogen. H2 emission is also present in the lobes. Our K-band images show the equatorial emission to be in the form of a ring or torus extending around the object at a distance R about 7 x 10 exp 16 (D/1 kpc) cm. Mechanisms for exciting the equatorial H2 emission are discussed; we conclude that shocks are the only plausible source. We have analyzed the broadband images using models which assume single scattering of photons from the central star. We find that the bipolar axis is inclined to the plane of the sky by i about 5 deg. The images are best reproduced by models in which the density of scattering dust decreases fairly rapidly with increasing stellar latitude, with little or no dust near the poles. Furthermore, the optical depth is found to have very little wavelength dependence, which implies that the dust in AFGL 2688 is different from that in the interstellar medium.

Latter, William B.↗
NASA NTRS1992

Near-infrared observations of the proto-planetary nebula AFGL 618

Near-IR images and spectroscopy of the bipolar protoplanetary nebula AFGL 618 are presented. Emission from molecular hydrogen is detected in the 0.90-1.34-micron spectrum. A visual extinction of 3.4 +4.0/-2.0 mag to the H2-emitting region is derived from molecular hydrogen line ratios. Models of collisionally excited and fluorescent H2 emission are compared with the data: the near-IR H2 spectrum is found to be dominated by emission from collisionally excited molecules at Tex of about 2000 K, but a component of fluorescent emission is also present. It is shown that this type of near-IR spectrum is an excellent tool for discriminating relatively low levels of fluorescent H2 emission from a strong collisionally excited component. Images in the H- and K-bandpasses are analyzed using models which assume single scattering of photons from the central objects. The models indicate that the bipolar axis is inclined to the plane of the sky by about 45 deg. The emission in the H- and K-bands is found to be consistent with single scattering of photons by dust with a distribution such that the dust density increases with increasing stellar latitude and is nearly zero at the poles.

Latter, William B.↗
NASA NTRS1973

Reactions of O/1D/ with methane and ethane.

Mixtures of nitrous oxide and methane and mixtures of nitrous oxide and ethane were photolyzed with 1849-A light. The reaction products were analyzed chromatographically. It was found that the reaction of the excited atomic oxygen with methane gives mainly CH3 and OH radicals as initial products, along with about 9% of formaldehyde and molecular hydrogen. The reaction of the excited atomic oxygen with ethane gives C2H5, OH, CH3 and CH2OH as major initial products, with only a few per cent of molecular hydrogen.

Lin, C.-L.↗
NASA NTRS2003

The Shock Structure of Supernova Remnant IC443

We present and discuss ISO observations of IC443, a supernova remnant interacting with a molecular cloud. An SWS spectrum centered on molecular hydrogen clump R10E (RA(2000) = 6 17 7.6, Decl(2000) = 22 25 34.6) is dominated by strong [SiII] (34 microns) emission and the pure rotational transitions of molecular hydrogen ranging from 0-0 S(1) to 0-0 S(13). Fits to these H$-2$ lines imply a large column (approx. 7E19 cm$ {-2)$) of warm (T approx. 700 K) gas and an ortho/para ratio for hydrogen near 3. LWS Fabry-Perot spectra of [OI] (63 microns) and [CII] (158 microns) at positions R10E and C (RA(2000) = 6 17 42.8, Decl(2000) = 22 21 38.1) find broad (approx. 75 km/s), blue-shifted (-40 km/s) line profiles; their similarity strongly suggests a common, shock-generated origin for these two lines. The surprisingly large [CII]/[OI] ratio (approx. 0.1 to 0.2) confirms previous observations with the Kuiper Airborne Observatory. These [CII] and [OI] line intensities, the [SiII] intensity (above), and LWS grating measurements of OH (119 microns) and [OI] (145 microns) are all readily fit by a single, fast J-shock model. Although the [OI] (63) emission can alternatively be produced by a slow C-shock, this ensemble of lines can not be produced by such a shock and provides strong evidence for the existence of a J-shock. A 24-arcmin strip map shows that this far-infrared line emission is spatially correlated with the H$-2$ 1-0 S(1) emission, which most likely arises in an associated C-shock. In addition to this spatially correlated shock emission, the strip map identifies extended [CII] and [OI] emission with a significantly larger line ratio (approx. 0.6); this 'background' component is compared with current J-shock, C-shock, photo-dissociation region (PDR), and X-ray dissociation region (XDR) models in an effort to explain its origin.

Haas, Michael R.↗
DOE OSTI2021

Basic Energy Sciences Roundtable: Foundational Science for Carbon-Neutral Hydrogen Technologies

The amount of molecular hydrogen used worldwide is enormous; about 70 million metric tons are produced globally every year, with approximately 10 million metric tons produced within the U.S. alone. 1 Hydrogen is used primarily by the industrial sector for oil refining; chemical production, especially for ammonia; steel manufacturing; and transportation fuels. With the recent announcement of the Hydrogen Shot, the first U.S. Department of Energy (DOE) Energy Earthshot, the DOE declared a near-term focus on “accelerating breakthroughs of more abundant, affordable, and reliable clean energy solutions within the decade.” Consequently, there is a compelling need for novel approaches to enable hydrogen processes and technologies that do not emit carbon dioxide (i.e., are carbon-neutral). Innovative hydrogen research and development is required to impact how hydrogen is produced, stored, transported, converted, and used. Although progress has been made over the previous two decades, fundamental research can play a critical role in overcoming the technical hurdles that continue to limit implementation of economically viable systems and processes for carbon-neutral hydrogen technologies.

08 HYDROGEN↗
NASA NTRS1994

PRISM project optical instrument

The scientific goal of the Passively-cooled Reconnaissance of the InterStellar Medium (PRISM) project is to map the emission of molecular hydrogen at 17.035 micrometers and 28.221 micrometers. Since the atmosphere is opaque at these infrared wavelengths, an orbiting telescope is being studied. The availability of infrared focal plane arrays enables infrared imaging spectroscopy at the molecular hydrogen wavelengths. The array proposed for PRISM is 128 pixels square, with a pixel size of 75 micrometers. In order to map the sky in a period of six months, and to resolve the nearer molecular clouds, each pixel must cover 0.5 arcminutes. This sets the focal length at 51.6 cm. In order for the pixel size to be half the diameter of the central diffraction peak at 28 micrometers would require a telescope aperture of 24 cm; an aperture of 60 cm has been selected for the PRISM study for greater light gathering power.

Taylor, Charles R.↗
NASA NTRS2023

Design of a Minimal di-Nickel Hydrogenase Peptide

The most ancient processes for energy production in the evolution of life involve the reversible oxidation of molecular hydrogen by hydrogenase. Extant hydrogenase enzymes are complex, comprising hundreds of amino acids and multiple cofactors. We designed a 13 amino acid nickel-binding peptide capable of robustly producing molecular hydrogen from protons under a wide variety of conditions. The peptide forms a di-nickel cluster structurally analogous to a Ni-Fe cluster in [NiFe]-hydrogenase and the Ni-Ni cluster in acetyl-CoA synthase (ACS), two ancient, extant proteins central to metabolism. These experimental results clearly demonstrate that modern enzymes, despite their enormous complexity, likely evolved from simple peptide precursors on early Earth. One Sentence Summary: Small metal-binding peptides were the likely precursors of modern enzymes.

Joshua A. Mancini↗