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Materials Data on VSiNi by Materials Project

VNiSi crystallizes in the orthorhombic Amm2 space group. The structure is three-dimensional. there are two inequivalent V2+ sites. In the first V2+ site, V2+ is bonded in a 5-coordinate geometry to five Si4- atoms. There are three shorter (2.65 Å) and two longer (2.75 Å) V–Si bond lengths. In the second V2+ site, V2+ is bonded in a 7-coordinate geometry to seven Si4- atoms. There are a spread of V–Si bond distances ranging from 2.69–2.75 Å. There are two inequivalent Ni2+ sites. In the first Ni2+ site, Ni2+ is bonded in a 4-coordinate geometry to four Si4- atoms. There are three shorter (2.26 Å) and one longer (2.33 Å) Ni–Si bond lengths. In the second Ni2+ site, Ni2+ is bonded in a linear geometry to two equivalent Si4- atoms. There are one shorter (2.29 Å) and one longer (2.43 Å) Ni–Si bond lengths. There are three inequivalent Si4- sites. In the first Si4- site, Si4- is bonded to six V2+ and six Ni2+ atoms to form SiV6Ni6 cuboctahedra that share corners with fourteen SiV6Ni6 cuboctahedra, edges with six SiV6Ni6 cuboctahedra, and faces with four equivalent SiV6Si4Ni2 cuboctahedra. In the second Si4- site, Si4- is bonded to six V2+, two equivalent Ni2+, and four Si4- atoms to form SiV6Si4Ni2 cuboctahedra that share corners with eight SiV6Si4Ni2 cuboctahedra, edges with two equivalent SiV6Si4Ni2 cuboctahedra, and faces with ten SiV6Ni6 cuboctahedra. There are a spread of Si–Si bond distances ranging from 2.29–2.46 Å. In the third Si4- site, Si4- is bonded to six V2+, two equivalent Ni2+, and four equivalent Si4- atoms to form SiV6Si4Ni2 cuboctahedra that share corners with six SiV6Ni6 cuboctahedra, edges with six SiV6Ni6 cuboctahedra, and faces with eight equivalent SiV6Si4Ni2 cuboctahedra.

36 MATERIALS SCIENCE↗

X-ray observations of rapidly rotating O stars

HEAO-2 results suggest that high vsini O stars appear to be significantly fainter x-ray sources. We proposed to observe additional high vsini O stars to test this hypothesis. Unfortunately, the PSPC was shot down during our scheduled observation time, and the observation was not re-scheduled. The contract work was modified to carry out other related x-ray tasks.

Waldron, Wayne L.↗

The use of robotic telescopes for detecting planetary systems

It is argued that increases in the precision of photometric measurements and the development of fully automatic photometric telescopes (APTs) now make possible the detection of Jupiter-size objects around other stars. The two most promising approaches are to monitor binary stars that have their orbital plane nearly in our line of sight and to measure the rotation periods of stars that are known to have dark companions and have very accurate values for Vsini. Differential photometry with APTs, based on a rapid comparison among a group of stars, provides a precision of 2 parts in 1000. Transits of solar-type stars by planets or brown dwarfs the size of Jupiter or Saturn will produce brightness variations of about 10 parts per 1000.

Borucki, William J.↗

(abstract) The Absorption Line Spectra of Herbig-Hiro Object Exciting Stars at 1.6 and 2 Microns

We observed six Herbig-Hiro object exciting stars with the IRTF CSHELL cryogenic echelle spectrometer at 1.6 and 2 microns with the intent of determining effective temperatures and vsini's from the absorption lines in these spectral regions. In all of these objects, the photospheric absorption lines were either very weak or undetectable with our modest S/N high spectral resolution data. Using this information, constraints can be placed on the veiling continuum present at these wavelengths for embedded low-mass YSOs.

Herbig-Hiro object exciting stars spectrometry abs↗

I Zw 18, a Template for Star-Forming, z is Greater than 7 Galaxies

I Zw 18-NW, one of the most primitive nearby dwarf galaxies, is arguably the best template we have for star-forming, very high-redshift galaxies (z>7). We have therefore obtained a far-UV spectrum of I Zw 18-NW using Hubble's Cosmic Origins Spectrograph (COS). The spectrum indicates star-formation over the past approx.10 Myr, a very low stellar metallicity, log Z/Zsun approx. -1.7, and high average stellar rotation rate, Vsini approx.200 km/s. Stellar wind lines are very weak, and the edge velocity of wind lines is very low (approx.250 km/s). The overall properties of I Zw 18-NW are consistent with theories of very low metallicity, rapidly rotating stars, e.g. Meynet et al. (2006).

Heap, Sara R.↗