ALBERT

Description: 〈div data-abstract-type="normal"〉 〈p〉Agmantinite, ideally Ag〈span〉2〈/span〉MnSnS〈span〉4〈/span〉, is a new mineral from the Uchucchacua polymetallic deposit, Oyon district, Catajambo, Lima Department, Peru. It occurs as orange–red crystals up to 100 μm across. Agmantinite is translucent with adamantine lustre and possesses a red streak. It is brittle. Neither fracture nor cleavage were observed. Based on the empirical formula the calculated density is 4.574 g/cm〈span〉3〈/span〉. On the basis of chemically similar compounds the Mohs hardness is estimated at between 2 to 2½. In plane-polarised light agmantinite is white with red internal reflections. It is weakly bireflectant with no observable pleochroism with red internal reflections. Between crossed polars, agmantinite is weakly anisotropic with reddish brown to greenish grey rotation tints. The reflectances (〈span〉R〈/span〉〈span〉min〈/span〉 and 〈span〉R〈/span〉〈span〉max〈/span〉) for the four standard wavelengths are: 19.7 and 22.0 (470 nm); 20.5 and 23.2 (546 nm); 21.7 and 2.49 (589 nm); and 20.6 and 23.6 (650 nm), respectively.〈/p〉 〈p〉Agmantinite is orthorhombic, space group 〈span〉P〈/span〉2〈span〉1〈/span〉〈span〉nm〈/span〉, with unit-cell parameters: 〈span〉a〈/span〉 = 6.632(2), 〈span〉b〈/span〉 = 6.922(2), 〈span〉c〈/span〉 = 8.156(2) Å, 〈span〉V〈/span〉 = 374.41(17) Å〈span〉3〈/span〉, 〈span〉a〈/span〉:〈span〉b〈/span〉:〈span〉c〈/span〉 0.958:1:1.178 and 〈span〉Z〈/span〉 = 2. The crystal structure was refined to 〈span〉R〈/span〉 = 0.0575 for 519 reflections with 〈span〉I 〉〈/span〉 2σ(〈span〉I〈/span〉). Agmantinite is the first known mineral of 〈span〉〈span〉〈img data-mimesubtype="gif" data-type="simple" src="http://static.cambridge.org/resource/id/urn:cambridge.org:id:binary:20190522072108342-0385:S0026461X18001391:S0026461X18001391_inline1.gif"〉 〈span data-mathjax-type="texmath"〉 〈/span〉 〈/span〉〈/span〉〈span〉M〈/span〉〈span〉II〈/span〉〈span〉M〈/span〉〈span〉IV〈/span〉S〈span〉4〈/span〉 type that is derived from wurtzite rather than sphalerite by ordered substitution of Zn, analogous to the substitution pattern for deriving stannite from sphalerite. The six strongest X-ray powder-diffraction lines derived from single-crystal X-ray diffraction data [〈span〉d〈/span〉 in Å (intensity)] are: 3.51 (s), 3.32 (w), 3.11 (vs), 2.42 (w), 2.04 (m) and 1.88 (m). The empirical formula (based on 8 apfu) is (Ag〈span〉1.94〈/span〉Cu〈span〉0.03〈/span〉)〈span〉Σ1.97〈/span〉(Mn〈span〉0.98〈/span〉Zn〈span〉0.05〈/span〉)〈span〉Σ1.03〈/span〉Sn〈span〉0.97〈/span〉S〈span〉4.03〈/span〉.The crystal structure-derived formula is Ag〈span〉2〈/span〉(Mn〈span〉0.69〈/span〉Zn〈span〉0.31〈/span〉)〈span〉Σ1.00〈/span〉SnS〈span〉4〈/span〉 and the simplified formula is Ag〈span〉2〈/span〉MnSnS〈span〉4〈/span〉.〈/p〉 〈p〉The name is for the composition and the new mineral and mineral name have been approved by the International Mineralogical Association Commission on New Minerals, Nomenclature and Classification (IMA2014-083).〈/p〉 〈/div〉

Description: The young (~16 Myr) pre-main-sequence star in Sco–Cen 1SWASP J140747.93–394542.6, hereafter referred to as J1407, underwent a deep eclipse in 2007 April, bracketed by several shallower eclipses in the surrounding 54 d. This has been interpreted as the first detection of an eclipsing ring system circling a substellar object (dubbed J1407b). We report on a search for this companion with Sparse Aperture Mask imaging and direct imaging with both the UT4 VLT and Keck telescopes. Radial velocity measurements of J1407 provide additional constraints on J1407b and on short period companions to the central star. Follow-up photometric monitoring using the Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT)-4 and ROAD observatories during 2012–2014 has not yielded any additional eclipses. Large regions of mass–period space are ruled out for the companion. For circular orbits the companion period is constrained to the range 3.5–13.8 yr ( a ~= 2.2–5.6 au), and stellar masses (〉80 M Jup ) are ruled out at 3 significance over these periods. The complex ring system appears to occupy more than 0.15 of its Hill radius, much larger than its Roche radius and suggesting a ring structure in transition. Further, we demonstrate that the radial velocity of J1407 is consistent with membership in the Upper Cen–Lup subgroup of the Sco–Cen association, and constraints on the rotation period and projected rotational velocity of J1407 are consistent with a stellar inclination of i * ~= 68° ± 10°.

Description: 〈div data-abstract-type="normal"〉〈p〉Structural data for weishanite, an alloy of Au, Ag and Hg, were collected for the first time from a crystal from the Keystone Mine, Colorado, USA. The structure was solved in the space group 〈span〉P〈/span〉6〈span〉3〈/span〉/〈span〉mmc〈/span〉 with the unit cell 〈span〉a〈/span〉 = 2.9348(8) and 〈span〉c〈/span〉 = 4.8215(18) Å] and refined to 〈span〉R〈/span〉 = 0.0299 for 40 observed reflections [4σ(〈span〉F〈/span〉) level] and four parameters and to 〈span〉R〈/span〉 = 0.0356 for all 47 independent reflections. The weishanite structure can be considered a derivative of the zinc structure, with Au, Ag and Hg disordered in the same structural position. On this basis, we suggest that the formula is normalized to 1 atom with 〈span〉Z〈/span〉 = 2, leading, for the sample investigated, to Au〈span〉0.41〈/span〉Ag〈span〉0.31〈/span〉Hg〈span〉0.28〈/span〉 (electron microprobe data). Accordingly, weishanite can be considered the Au-rich isotype of schachnerite. A comparison with other Au/Ag-Hg alloys is presented together with a critical discussion about the nomenclature rules to be applied to alloys and simple metals.〈/p〉〈/div〉

Description: Gamma-ray bursts (GRBs) are the most luminous explosions in the Universe, yet the nature and physical properties of their energy sources are far from understood. Very important clues, however, can be inferred by studying the afterglows of these events. We present optical and X-ray observations of GRB 130831A obtained by Swift, Chandra , Skynet, Reionization And Transients Infra-Red camera, Maidanak, International Scientific Optical-Observation Network, Nordic Optical Telescope, Liverpool Telescope and Gran Telescopio Canarias. This burst shows a steep drop in the X-ray light curve at ~=10 5  s after the trigger, with a power-law decay index of α ~ 6. Such a rare behaviour cannot be explained by the standard forward shock (FS) model and indicates that the emission, up to the fast decay at 10 5  s, must be of ‘internal origin’, produced by a dissipation process within an ultrarelativistic outflow. We propose that the source of such an outflow, which must produce the X-ray flux for ~=1 d in the cosmological rest frame, is a newly born magnetar or black hole. After the drop, the faint X-ray afterglow continues with a much shallower decay. The optical emission, on the other hand, shows no break across the X-ray steep decrease, and the late-time decays of both the X-ray and optical are consistent. Using both the X-ray and optical data, we show that the emission after ~=10 5  s can be explained well by the FS model. We model our data to derive the kinetic energy of the ejecta and thus measure the efficiency of the central engine of a GRB with emission of internal origin visible for a long time. Furthermore, we break down the energy budget of this GRB into the prompt emission, the late internal dissipation, the kinetic energy of the relativistic ejecta, and compare it with the energy of the associated supernova, SN 2013 fu.