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All sourcesNASA NTRSDOE OSTI
DOE OSTI2020

Materials Data on YSc(BO3)2 by Materials Project

YSc(BO3)2 is Calcite-derived structured and crystallizes in the trigonal R-3 space group. The structure is three-dimensional. Y3+ is bonded to six equivalent O2- atoms to form YO6 octahedra that share corners with six equivalent ScO6 octahedra. The corner-sharing octahedral tilt angles are 58°. All Y–O bond lengths are 2.32 Å. Sc3+ is bonded to six equivalent O2- atoms to form ScO6 octahedra that share corners with six equivalent YO6 octahedra. The corner-sharing octahedral tilt angles are 58°. All Sc–O bond lengths are 2.14 Å. B3+ is bonded in a trigonal planar geometry to three equivalent O2- atoms. All B–O bond lengths are 1.39 Å. O2- is bonded in a distorted trigonal planar geometry to one Y3+, one Sc3+, and one B3+ atom.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Materials Data on YSc by Materials Project

YSc crystallizes in the hexagonal P-6m2 space group. The structure is three-dimensional. Y is bonded to six equivalent Y and six equivalent Sc atoms to form YY6Sc6 cuboctahedra that share corners with eighteen equivalent YY6Sc6 cuboctahedra, edges with six equivalent YY6Sc6 cuboctahedra, edges with twelve equivalent ScY6Sc6 cuboctahedra, faces with eight equivalent YY6Sc6 cuboctahedra, and faces with twelve equivalent ScY6Sc6 cuboctahedra. All Y–Y bond lengths are 3.48 Å. All Y–Sc bond lengths are 3.40 Å. Sc is bonded to six equivalent Y and six equivalent Sc atoms to form ScY6Sc6 cuboctahedra that share corners with eighteen equivalent ScY6Sc6 cuboctahedra, edges with six equivalent ScY6Sc6 cuboctahedra, edges with twelve equivalent YY6Sc6 cuboctahedra, faces with eight equivalent ScY6Sc6 cuboctahedra, and faces with twelve equivalent YY6Sc6 cuboctahedra. All Sc–Sc bond lengths are 3.48 Å.

36 MATERIALS SCIENCE↗
DOE OSTI2020

Observations of Binary Stars with the Differential Speckle Survey Instrument. IX. Observations of Known and Suspected Binaries, and a Partial Survey of Be Stars

We report 370 measures of 170 components of binary and multiple-star systems, obtained from speckle imaging observations made with the Differential Speckle Survey Instrument at Lowell Observatory’s Discovery Channel Telescope in 2015 through 2017. Of the systems studied, 147 are binary stars, 10 are seen as triple systems, and 1 quadruple system is measured. Seventy-six high-quality nondetections and 15 newly resolved components are presented in our observations. The uncertainty in relative astrometry appears to be similar to our previous work at Lowell, namely, linear measurement uncertainties of approximately 2 mas, and the relative photometry appears to be uncertain at the 0.1–0.15 mag level. Using these measures and those in the literature, we calculate six new visual orbits, including one for the Be star 66 Oph and two combined spectroscopic–visual orbits. The latter two orbits, which are for HD 22451 (YSC 127) and HD 185501 (YSC 135), yield individual masses of the components at the level of 2% or better, and independent distance measures that in one case agrees with the value found in the Gaia DR2 and in the other disagrees at the 2σ level. We find that HD 22451 consists of an F6V+F7V pair with orbital period of 2401.1 ± 3.2 days and masses of 1.342 ± 0.029 and 1.236±0.026 M{sub ⊙}. For HD 185501, both stars are G5 dwarfs that orbit one another with a period of 433.94 ± 0.15 days, and the masses are 0.898 ± 0.012 and 0.876±0.012 M{sub ⊙}. We discuss the details of both the new discoveries and the orbit objects.

79 ASTRONOMY AND ASTROPHYSICS↗