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At least 433 records · Page 24
All sourcesNASA NTRSDOE OSTI
NASA NTRS1991

Microstructure-property relationships in Al-Cu-Li-Ag-Mg Weldalite (tm) alloys, part 2

The microstructure and mechanical properties of the ultrahigh strength Al-Cu-Li-Ag-Mg alloy, Weldalite (tm) 049, were studied. Specifically, the microstructural features along with tensile strength, weldability, Young's modulus and fracture toughness were studied for Weldalite (tm) 049 type alloys with Li contents ranging from 1.3 to 1.9 wt. pct. The tensile properties of Weldalite 049 and Weldalite 049 reinforced with TiB2 particles fabricated using the XD (tm) process were also evaluated at cryogenic, room, and elevated temperatures. In addition, an experimental alloy, similar in composition to Weldalite 049 but without the Ag+Mg, was fabricated. The microstructure of this alloy was compared with that of Weldalite 049 in the T6 condition to assess the effect of Ag+Mg on nucleation of strengthening phases in the absence of cold work.

Langan, T. J.↗
NASA NTRS1990

The Mg II h and k interstellar lines in the spectrum of the G-type giant HD 156854

The results of the measurements and analysis of the IUE observations of the 2800 Mg II doublet in the spectrum of HD 156854, a G9 III star, are presented. The relative power of the magnesium chromosphere, R(Mg) = 0.00001, is in agreement with the known data for giants of the same class. The emission profiles of this doublet present absorption cores, which are of interstellar origin. Taking into account the interstellar depletion of Mg, the derived density of interstellar hydrogen is n(H) = 0.001/cu cm, which agrees with the conclusion (Paresce 1984) about the possibility of large hydrogen concentrations in some directions of the Galaxy far from the sun.

Gurzadian, G. A.↗
NASA NTRS1991

The bonding of multiple ligands to Mg(+) and Al(+)

The bonding of one to four waterligands to Mg(+) and Al(+) is studied. The bonding is very different from that found for multiple ligands bound to Na(+) or Cu(+). All the waters bind on the same side of the Mg or Al because of the polarization of the 3s orbital away from the ligands. Two benzene and methanol molecules also have a ligand-Mg-ligand angle of less than 180 deg with the angle determined by ligand-ligand repulsion.

Bauschlicher, Charles W., Jr.↗
NASA NTRS1992

Mg II absorption in the spectra of 103 QSOs - Implications for the evolution of gas in high-redshift galaxies

Spectra of 103 low- and intermediate-redshift QSOs with a resolution of 4-6 A were obtained in order to investigate the statistics of the M II 2796, 2803 absorption systems over the redshift range of 0.2-2.2. New emission-line redshifts, based mostly on Mg II 2800 and semiforbidden 1909, were determined for the QSOs. The mean number density of Mg II absorbers per unit redshift range decreased from 0.97 +/-0.10 for a rest equivalent width threshold of 0.3 A to 0.27 +/-0.05 for a threshold of 1.0 A. The results are in agreement with comparable previous work. The observed equivalent width distribution could be fitted with either exponential or power-law analytic distributions, with parameters in line with those found in earlier studies. Statistical tests show that the Mg II absorbers are uniformly distributed in both comoving coordinates and velocity relative to the QSO.

Steidel, Charles C.↗
NASA NTRS1992

Calculation of Mg(+)-ligand relative binding energies

The calculated relative binding energies of 16 organic molecules to Mg(+) are compared with experimental results where available. The geometries of the ligands and the Mg(+)-ligand complexes arc optimized at the self-consistent field level using a 6-31G* basis set. The Mg(+) binding energies are evaluated using second-order perturbation theory and basis sets of triple-sigma quality augmented with two sets of polarization functions. This level of theory is calibrated against higher levels of theory for selected systems. The computed binding energies are accurate to about 2 kcal/mol.

Partridge, Harry↗
NASA NTRS1993

Mg II and Ly-alpha fluxes in M dwarfs - Evaluation of an acoustic model

Surface fluxes of Mg II and Ly-alpha from a sample of M dwarfs have been reported by Panagi and Mathioudakis (PM, 1992). In order to determine if acoustic effects can reproduce the fluxes in the least active ('basal') stars in the PM sample, we have constructed steady state models of plane-parallel atmospheres with T(eff) = 3000 and 4000 K including heating by shock dissipation. The models incorporate radiative losses in the chromosphere by solving the transfer equation for two strong lines (Mg II k and Ly-alpha). Predictions of standard weak shock theory are expected to overestimate the rate of energy deposition in the chromospheres of M dwarfs compared to the rate of deposition in F, G, or K dwarfs. In order to incorporate this effect in M dwarfs, we compute a series of atmospheric models in which, for a given T(eff), the standard weak shock dissipation rate is reduced by a series of factors F(r). Although the input acoustic flux F(mech) may in principle be determined uniquely by T(eff) and log g, the correct value to use in any particular case is not well known. We therefore use F(mech) and F(r) as parameters to construct a family of M dwarf models at various T(eff) and g. Comparing with the observed fluxes in the least active M dwarfs of the PM sample, we find that our models reproduce the observed fluxes of both Mg II and Ly-alpha best if F(mech) is close to the value predicted by Bohn (1984) and if F(r) is approximately equal to 10-20.

Mullan, D. J.↗
NASA NTRS1993

Zaoyang chondrite cooling history from pyroxene Fe(2+)-Mg intracrystalline ordering and exolutions

The Zaoyang ordinary chondrite fell as a single 14.15-kg mass in Hubey province (China) in October 1984 and was classified as a non-brecciated H5 chondrite, shock facies b. Cooling rate in pyroxenes can be calculated down to about 1000 C by using fine textures and at still lower temperatures (700 to 200 C) by intracrystalline ordering processes. The crystal chemistry of clinopyroxene and orthopyroxene from the matrix of the H5 Zaoyang chondrite has been investigated by X-ray structure refinement and detailed microprobe analysis. By comparison with terrestrial pyroxenes cell and polyhedral volumes in clino- and orthopyroxenes show a low crystallization pressure. Fe(2+) and Mg are rather disordered in M1 and M2 sites of clino- and orthopyroxenes; the closure temperatures of the exchange reaction are 600 and 512 C respectively, which is consistent with a quite fast cooling rate, estimated of the order of one degree per day. The closure temperature for the intercrystalline Ca-Mg exchange reaction for clino- and orthopyroxene showing clinopyroxene lamellae about 10 microns thick. Kinetic evaluations based on the thickness of exolved lamellae give a cooling rate of not more than a few degrees per 10(exp 4) years. The different cooling rates obtained from Fe(2+)-Mg intracrystalline partitioning and exolution lamellae suggest an initial episode of slow cooling at 900 C, followed by faster cooling at temperatures of 600-500 C at low pressure conditions. The most probable scenario of the meteorite history seems that the exolved orthopyroxene entered the parental chondrite body after exolution had taken place at high temperature. Subsequent fast cooling occurred at low temperature after the formation of the body.

Molin, G. M.↗
NASA NTRS1994

Heating during solar nebula formation and Mg isotopic fractionation in precursor grains of CAIs and chondrules

In some Ca-Al-rich inclusion (CAI) grains, mass-dependent isotopic fractionations of Mg, Si, and O are observed and large Mg isotopic fractionation is interpreted to have been produced by cosmochemical processes such as evaporation and condensation. Mass-dependent Mg isotopic fractionation was found in olivine chondrules of Allende meteorites. Presented is an approximate formula for the temperature of the solar nebula that depends on heliocentric distance and the initial gas distribution. Shock heating during solar nebula formation can cause evaporative fractionation within interstellar grains involved in a gas at the inner zone (a less than 3 AU) of the disk. Alternatively collision of late-accreting gas blobs might cause similar heating if Sigma(sub s) and Sigma are large enough. Since the grain size is small, the solid/gas mass ratio is low and solar (low P(sub O2)), and the ambient gas pressure is low, this heating event could not produce chondrules themselves. Chondrule formation should proceed around the disk midplane after dust grains would grow and sediment to increase the solid/gas ratio there. The heating source there is uncertain, but transient rapid accretion through the disk could release a large amount of heat, which would be observed as FU Orionis events.

Sasaki, S.↗
NASA NTRS1994

Mg II chromospheric-emission dating of HR 1614 moving-group stars

A 2800 A Mg II line index I(Mg II) that is sensitive to chromospheric activity has been measured from International Ultraviolet Explorer spectra of a sample of eight HR 1614 moving-group dwarfs. All of these dwarfs have values of I(Mg II) indicative of ages greater than or equal to 3 Gyr. The relatively old ages of these dwarfs, together with their similar and peculiar kinematics and high metal abundance, is consistent with, although not conclusive proof of, coeval formation in close physical proximity to each other. The age, chemical abundance, and kinematics of the HR 1614 moving group -- with the notable exception of height above the Galactic plane -- are similar to the properties of the old open cluster NGC 6791.

Hufnagel, Beth↗
NASA NTRS2010

MG Isotopic Measurement of FIB-Isolated Presolar Silicate Grains

The majority of presolar oxide and silicate grains are ascribed to origins in low-mass red giant and asymptotic giant branch (AGB) stars based on their O isotopic ratios. However, a minor population of these grains (< 10%) has O isotopic ratios incompatible with these sources. Two principle alternative sources are higher-than-solar metallicity (Z) stars or, more likely, supernovae (SN) [1-3]. These rare (Group 4) grains [3] are characterized by enrichments in O-18, and typically also enrichments in O-17. An even rarer subset of grains with extremely large enrichments in O-17 and smaller depletions in O-18 were suggested to come from binary star systems [2]. To establish the origins of these isotopically unusual grains, it is necessary to examine isotopic systems in addition to O. Presolar silicates offer several elements diagnostic of their stellar sources and nuclear processes, including O, Si, Mg, Fe and Ca. However, the database for minor element isotopic compositions in silicates is seriously lacking. To date only two silicate grains have been analyzed for Mg [4] or Fe [5]. One major complicating factor is their small size (average ~230 nm), which greatly limits the number of measurements that can be performed on any one grain and makes it more difficult to obtain statistically relevant data. This problem is compounded because the grains are identified among isotopically solar silicates, which contribute a diluting signal in isotopic measurements [1]. Thus, relatively small isotopic anomalies are missed due to this dilution effect. By applying focused ion beam (FIB) milling, we obtain undiluted Mg isotopic ratios of isolated rare presolar silicate grains to investigate their sources.

Messenger, Scott R.↗
NASA NTRS2010

Discovery of X-Ray-Emitting O-Ne-Mg-Rich Ejecta in the Galactic Supernova Remnant Puppis A

We report on the discovery of X-ray-emitting O-Ne-Mg-rich ejecta in the middle-aged Galactic O-rich supernova remnant Puppis A with Chandra and XMM-Newton. We use line ratios to identify a low-ionization filament running parallel to the northeastern edge of the remnant that requires super-solar abundances, particularly for O, Ne, and Mg, which we interpret to be from O-Ne-Mg-rich ejecta. Abundance ratios of Ne/O, Mg/O, and Fe/O are measured to be [approx]2, [approx]2, and <0.3 times the solar values. Our spatially resolved spectral analysis from the northeastern rim to the western rim otherwise reveals sub-solar abundances consistent with those in the interstellar medium. The filament is coincident with several optically emitting O-rich knots with high velocities. If these are physically related, the filament would be a peculiar fragment of ejecta. On the other hand, the morphology of the filament suggests that it may trace ejecta heated by a shock reflected strongly off the dense ambient clouds near the northeastern rim.

Katsuda, Satoru↗
NASA NTRS2011

FE and MG Isotopic Analyses of Isotopically Unusual Presolar Silicate Grains

Interstellar and circumstellar silicate grains are thought to be Mg-rich and Fe-poor, based on astronomical observations and equilibrium condensation models of silicate dust formation in stellar outflows. On the other hand, presolar silicates isolated from meteorites have surprisingly high Fe contents and few Mg-rich grains are observed. The high Fe contents in meteoritic presolar silicates may indicate they formed by a non-equilibrium condensation process. Alternatively, the Fe in the stardust grains could have been acquired during parent body alteration. The origin of Fe in presolar silicates may be deduced from its isotopic composition. Thus far, Fe isotopic measurements of presolar silicates are limited to the Fe-54/Fe-56 ratios of 14 grains. Only two slight anomalies (albeit solar within error) were observed. However, these measurements suffered from contamination of Fe from the adjacent meteorite matrix, which diluted any isotopic anomalies. We have isolated four presolar silicates having unusual O isotopic compositions by focused ion beam (FIB) milling and obtained their undiluted Mg and Fe isotopic compositions. These compositions help to identify the grains stellar sources and to determine the source of Fe in the grains.

Nguyen, A. N.↗
NASA NTRS2024

Evaluation of an Al-Cu-Zn-Mg Alloy for Wire-Fed Additive Manufacturing

A collaborative research study was conducted to evaluate an experimental Al-Cu-Zn-Mg alloy, designated Al C380H, developed by Arconic Corporation for wire-fed additive manufacturing (AM) techniques such as NASA’s electron beam freeform fabrication (EBF 3 ) process and the wire arc additive manufacturing (WAAM) process. The goal of the study was to determine, based upon metallurgical properties, whether additively manufactured Al C380H represented a viable alternative for applications currently using wrought 7xxx series aluminum. Al 2319 and Al 7075 were also deposited as AM-compatible and non-AM-compatible baselines, respectively. Evaluation was based on tensile, fracture, and corrosion properties. The strength and ductility of Al C380H-T6 materials produced by EBF3 and WAAM were sufficiently lower than typical values for Al 7050-T7 to indicate that additively manufactured Al C380H is not a viable replacement for current parts fabricated with Al 7050, due largely to the significant losses in Zn and Mg and development of porosity during deposition. EBF 3 parameters that reduced porosity, such as increasing electron beam current, higher raster frequency, sharper beam focus, and slower travel speed, augmented de-alloying of fugitive solute. Further enhancement of Zn and Mg content in Al C380H feedstock wire combined with adjustments to deposition conditions to minimize porosity may enable production of Al C380H parts by EBF 3 or WAAM that are viable replacements for current Al 7050 wrought products.

electron beam freeform fabrication (EBF3)↗
DOE OSTI2020

Materials Data on Mg(C2N3)2 by Materials Project

Mg(C2N3)2 crystallizes in the orthorhombic Pnnm space group. The structure is three-dimensional. Mg2+ is bonded in an octahedral geometry to six N3- atoms. There are four shorter (2.13 Å) and two longer (2.31 Å) Mg–N bond lengths. C4+ is bonded in a linear geometry to two N3- atoms. There is one shorter (1.17 Å) and one longer (1.31 Å) C–N bond length. There are two inequivalent N3- sites. In the first N3- site, N3- is bonded in a trigonal planar geometry to one Mg2+ and two equivalent C4+ atoms. In the second N3- site, N3- is bonded in a linear geometry to one Mg2+ and one C4+ atom.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on Mg(BeN)2 by Materials Project

Mg(BeN)2 crystallizes in the trigonal P-3m1 space group. The structure is three-dimensional. Mg2+ is bonded to six equivalent N3- atoms to form MgN6 octahedra that share corners with twelve equivalent BeN4 tetrahedra, edges with six equivalent MgN6 octahedra, and edges with six equivalent BeN4 tetrahedra. All Mg–N bond lengths are 2.22 Å. Be2+ is bonded to four equivalent N3- atoms to form BeN4 tetrahedra that share corners with six equivalent MgN6 octahedra, corners with six equivalent BeN4 tetrahedra, edges with three equivalent MgN6 octahedra, and edges with three equivalent BeN4 tetrahedra. The corner-sharing octahedra tilt angles range from 24–50°. There is three shorter (1.77 Å) and one longer (1.78 Å) Be–N bond length. N3- is bonded in a 7-coordinate geometry to three equivalent Mg2+ and four equivalent Be2+ atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on Mg(ScS2)2 by Materials Project

Mg(ScS2)2 is Spinel structured and crystallizes in the cubic Fd-3m space group. The structure is three-dimensional. Mg2+ is bonded to four equivalent S2- atoms to form MgS4 tetrahedra that share corners with twelve equivalent ScS6 octahedra. The corner-sharing octahedral tilt angles are 57°. All Mg–S bond lengths are 2.46 Å. Sc3+ is bonded to six equivalent S2- atoms to form ScS6 octahedra that share corners with six equivalent MgS4 tetrahedra and edges with six equivalent ScS6 octahedra. All Sc–S bond lengths are 2.59 Å. S2- is bonded to one Mg2+ and three equivalent Sc3+ atoms to form a mixture of distorted corner and edge-sharing SMgSc3 trigonal pyramids.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on Mg(InTe2)2 by Materials Project

Mg(InTe2)2 crystallizes in the monoclinic Cm space group. The structure is three-dimensional. Mg2+ is bonded to four Te2- atoms to form MgTe4 tetrahedra that share corners with eight equivalent InTe4 tetrahedra. There are three shorter (2.83 Å) and one longer (2.84 Å) Mg–Te bond lengths. In3+ is bonded to four Te2- atoms to form InTe4 tetrahedra that share corners with four equivalent MgTe4 tetrahedra and corners with four equivalent InTe4 tetrahedra. All In–Te bond lengths are 2.85 Å. There are three inequivalent Te2- sites. In the first Te2- site, Te2- is bonded in a distorted trigonal non-coplanar geometry to one Mg2+ and two equivalent In3+ atoms. In the second Te2- site, Te2- is bonded in a distorted trigonal non-coplanar geometry to one Mg2+ and two equivalent In3+ atoms. In the third Te2- site, Te2- is bonded in a distorted trigonal non-coplanar geometry to one Mg2+ and two equivalent In3+ atoms.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on Mg(BC)2 by Materials Project

MgB2C2 crystallizes in the orthorhombic Cmce space group. The structure is three-dimensional. there are two inequivalent Mg2+ sites. In the first Mg2+ site, Mg2+ is bonded in a distorted hexagonal planar geometry to six C4- atoms. There are a spread of Mg–C bond distances ranging from 2.43–2.50 Å. In the second Mg2+ site, Mg2+ is bonded in a 6-coordinate geometry to six C4- atoms. There are a spread of Mg–C bond distances ranging from 2.26–2.51 Å. There are three inequivalent B3+ sites. In the first B3+ site, B3+ is bonded in a trigonal planar geometry to three C4- atoms. There are a spread of B–C bond distances ranging from 1.56–1.60 Å. In the second B3+ site, B3+ is bonded in a trigonal planar geometry to three C4- atoms. All B–C bond lengths are 1.58 Å. In the third B3+ site, B3+ is bonded in a trigonal planar geometry to three C4- atoms. All B–C bond lengths are 1.59 Å. There are three inequivalent C4- sites. In the first C4- site, C4- is bonded in a distorted trigonal planar geometry to four Mg2+ and three B3+ atoms. In the second C4- site, C4- is bonded in a distorted trigonal planar geometry to three Mg2+ and three B3+ atoms. In the third C4- site, C4- is bonded in a distorted trigonal planar geometry to two equivalent Mg2+ and three B3+ atoms.

36 MATERIALS SCIENCE↗