Search NASA⌕ Search

SEARCH · Search NASA

Results for “WN”

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 19 records

Synthesis and Properties of Bulk Mg 3 WN 4 in a Wurtzite-Derived Structure

Experimental synthesis of theoretically predicted materials with controlled elemental coordination environments can lead to the realization of useful properties, such as facile ion transport or ferroelectric switching. Among such materials are ternary nitrides in the Mg−W−N composition space, where several stable and metastable compounds have been predicted and synthesized recently in bulk and film forms. Here, we report for the first time on the bulk synthesis of Mg 3 WN 4 in a wurtzite-derived crystal structure via a solid-state metathesis reaction. In situ synchrotron powder X-ray diffraction shows how the ion exchange proceeds from Li 6 WN 4 + MgCl 2 precursors to Mg 3 WN 4 + LiCl products, with the reaction starting slowly near 380 °C and completing by 600 °C, including the presence of a competing disordered rocksalt-derived phase (Mg,W)N above 440 °C. The follow-up ex situ powder synthesis at 400 °C for 0.5 h with 10% excess MgCl 2 reveals the cation-ordered nature of the wurtzite-derived Mg 3 WN 4 structure with polar symmetry confirmed by second-harmonic generation measurements. Optical absorption spectra, chemical composition analysis, and electron microscopy imaging suggest that bulk Mg 3 WN 4 obtained via metathesis reaction is prone to defect formation. Overall, this study shows that selective ex situ synthesis of the phase-pure ternary nitrides, informed by in situ measurements, is possible by carefully controlling the thermal budget of the reaction and paves the way toward property characterization of the Mg 3 WN 4 wurtzite-derived material.

36 MATERIALS SCIENCE↗

Of-type stars HD 16691 and HD 190429 show WN-like spectra in infrared K band

We present 2 micrometer K-band spectra of two early-type Of stars that have infrared emission-line morphology similar to that of WN stars. Archival International Ultraviolet Explorer (IUE) spectra of these two stars indicate they appear to be Of type, rather than WN. Recently acquired optical spectra of these stars are quantitatively similar to that in the past, namely, Of attributes. We suggest that these two Of stars have stellar wind characteristics closer to WN type than other Of stars. We discuss the consequences for K-band classification of highly obscured hot stars that might not otherwise be visible in optical or UV wavelengths.

Conti, Peter S.↗

Materials Data on Ca(WN)2 by Materials Project

Ca(WN)2 crystallizes in the tetragonal P-4m2 space group. The structure is two-dimensional and consists of one Ca(WN)2 sheet oriented in the (0, 0, 1) direction. Ca2+ is bonded to four equivalent N3- atoms to form distorted corner-sharing CaN4 tetrahedra. All Ca–N bond lengths are 2.33 Å. W2+ is bonded in a bent 120 degrees geometry to two equivalent N3- atoms. Both W–N bond lengths are 1.92 Å. N3- is bonded to two equivalent Ca2+ and two equivalent W2+ atoms to form corner-sharing NCa2W2 tetrahedra.

36 MATERIALS SCIENCE↗

Materials Data on Zn(WN)2 by Materials Project

Zn(WN)2 crystallizes in the tetragonal P-4m2 space group. The structure is two-dimensional and consists of one Zn(WN)2 sheet oriented in the (0, 0, 1) direction. W2+ is bonded in a bent 120 degrees geometry to two equivalent N3- atoms. Both W–N bond lengths are 1.93 Å. Zn2+ is bonded to four equivalent N3- atoms to form corner-sharing ZnN4 tetrahedra. All Zn–N bond lengths are 2.07 Å. N3- is bonded to two equivalent W2+ and two equivalent Zn2+ atoms to form corner-sharing NZn2W2 tetrahedra.

36 MATERIALS SCIENCE↗

Free geometric adjustment of the OSU/NGSP global network /solution WN-4/

The paper presents the results of the OSU WN 4 geometric adjustment for the coordinates of 152 satellite tracking stations. The results, when referred to the WN 4 ellipsoid of a = 6,378,127.8 m and 1/f = 298.25 produce geoid undulations consistent with dynamically determined ones. The average standard deviation in a Cartesian coordinate is plus or minus 4.0 m; in height, plus or minus 2.7 m. Comparisons with coordinates obtained from dynamic solutions show significant inconsistencies in the orientation of the coordinate systems.

Mueller, I. I.↗

A new method to determine the interstellar reddening towards WN stars

An empirical approach to determine the redding in WN stars is presented, in which the measured strengths of the emission lines of He II at 1640 and 4686 A are used to estimate the extinction. The He II emission lines at these wavelengths are compared for a number of WN stars in the Galaxy and the LMC. It is shown that the equivalent width ratios are single valued and are independent of the spectral subtypes. The reddening for stars in the Galaxy is derived using a Galactic extinction law and observed line flux ratios, showing good agreement with previous determinations of reddening. The possible application of the method to study the absorption properties of the interstellar medium in more distant galaxies is discussed.

Conti, Peter S.↗

Classification and distribution of WR stars and an interpretation of the WN sequence.

New observational data for Wolf-Rayet stars are interpreted in areas of atmospheric abundances, absolute magnitudes, Galactic distribution, distribution in M33, and bolometric luminosities. The observational data are used in support of arguments (1) that WN stars are helium stars of eight to fourteen solar masses with atmospheres which contain only a very low proportion of hydrogen, (2) that the properties of the stars are very sensitive to this very small amount of hydrogen, and (3) that consequently this structure explains many of the general properties of the subclasses.

Smith, L. F.↗

IUE observations of phase-dependent variations in WN + O systems

IUE observations of six WN + O Wolf-Rayet (W-R) systems are reported. The periodic variations in five of the systems are shown to result primarily from selective atmospheric eclipses of the O star continuum by the W-R wind. An optical depth distribution of the form tau inversely proportional to radius is suggested for radii greater than 14 solar radii. Phase-dependent variations in the C IV 1550 absorption components in V444 Cyg, HD 90657, and HD 211853 are interpreted as wind-wind collision effects.

Koenigsberger, G.↗

He 3-519 - A peculiar post-LBV, pre-WN star?

We report IUE and ground-based data indicating that the star He 3-519 has a distance of roughly 8 kpc and an absolute bolometric magnitude of about -11, comparable to AG Car. Its luminosity, spectrum, and large, massive circumstellar shell indicate that this may be a post-LBV object which has not yet become a full-fledged WN star. One notable peculiarity of He 3-519 is its prominent Fe III (?) 3008 A emission; the reason why this feature is so bright in this star's dense envelope or wind, but not in other related stars, is not yet clear.

Davidson, Kris↗

Materials Data on WN by Materials Project

NW1 is Zincblende, Sphalerite structured and crystallizes in the cubic F-43m space group. The structure is three-dimensional. W3+ is bonded to four equivalent N3- atoms to form corner-sharing WN4 tetrahedra. All W–N bond lengths are 2.02 Å. N3- is bonded to four equivalent W3+ atoms to form corner-sharing NW4 tetrahedra.

36 MATERIALS SCIENCE↗

Materials Data on WN by Materials Project

NW1 is Halite, Rock Salt structured and crystallizes in the cubic Fm-3m space group. The structure is three-dimensional. W3+ is bonded to six equivalent N3- atoms to form a mixture of edge and corner-sharing WN6 octahedra. The corner-sharing octahedral tilt angles are 0°. All W–N bond lengths are 2.18 Å. N3- is bonded to six equivalent W3+ atoms to form a mixture of edge and corner-sharing NW6 octahedra. The corner-sharing octahedral tilt angles are 0°.

36 MATERIALS SCIENCE↗

Materials Data on WN by Materials Project

NW1 is Boron Nitride structured and crystallizes in the hexagonal P6_3mc space group. The structure is three-dimensional. W3+ is bonded in a rectangular see-saw-like geometry to four equivalent N3- atoms. There are one shorter (2.00 Å) and three longer (2.08 Å) W–N bond lengths. N3- is bonded in a rectangular see-saw-like geometry to four equivalent W3+ atoms.

36 MATERIALS SCIENCE↗

Materials Data on WN by Materials Project

NW1 is Tungsten Carbide structured and crystallizes in the hexagonal P-6m2 space group. The structure is three-dimensional. W3+ is bonded to six equivalent N3- atoms to form a mixture of distorted corner, edge, and face-sharing WN6 pentagonal pyramids. All W–N bond lengths are 2.21 Å. N3- is bonded to six equivalent W3+ atoms to form a mixture of distorted corner, edge, and face-sharing NW6 pentagonal pyramids.

36 MATERIALS SCIENCE↗

Materials Data on WN by Materials Project

NW1 is Tungsten Carbide-like structured and crystallizes in the orthorhombic Pmn2_1 space group. The structure is three-dimensional. W3+ is bonded to six equivalent N3- atoms to form a mixture of distorted edge and corner-sharing WN6 octahedra. The corner-sharing octahedra tilt angles range from 3–30°. There are a spread of W–N bond distances ranging from 2.16–2.33 Å. N3- is bonded to six equivalent W3+ atoms to form a mixture of distorted edge and corner-sharing NW6 octahedra. The corner-sharing octahedra tilt angles range from 3–30°.

36 MATERIALS SCIENCE↗

Global satellite triangulation and trilateration for the National Geodetic Satellite Program (solutions WN 12, 14 and 16)

A multi-year study and analysis of data from satellites launched specifically for geodetic purposes and from other satellites useful in geodetic studies was conducted. The program of work included theoretical studies and analysis for the geometric determination of station positions derived from photographic observations of both passive and active satellites and from range observations. The current status of data analysis, processing and results are examined.

Ivan I Mueller↗