Mechanism of gas permeation in processed HNBR/nanoclay composites

The influence of the layered silicate clay platelets on the nitrogen permeation properties of hydrogenated nitrile butadiene rubber (HNBR)/nanoclay nanocomposites has been investigated. Nanocomposites of HNBR modified with different percentages of the organoclay are processed through various routes. Commercially available organoclay (CLOISITE 15A) and various silane-coupling agents are used to improve the dispersion of the nanoclay in HNBR. A total of 10 different formulations of nanocomposites are manufactured. The addition of the organoclay has resulted in a significant enhancement of the nitrogen barrier properties of the manufactured nanocomposite. The mechanism of the reduction in the permeability is explained through the changes in the morphology and its bond to the filler. These changes are confirmed through examination of the morphology using x-ray diffraction, transmission electron microscope, and dynamic mechanical thermal analysis. There has been a drastic reduction up to 55.7% in nitrogen permeability. The reduction in gas permeation in HNBR is attributed to uniformly exfoliated clay platelets. Finally, three different permeability models, namely, the Nielsen model, modified Nielsen model, and Cussler model, have also been considered to predict the permeability behavior of nanocomposites with different volume filler fractions. The experimental values of gas permeability have been compared with theoretical models. It is observed that the modified Nielsen model closely matches with the measured permeation behavior. © 2011 Wiley Periodicals, Inc.

Multiferroic PbZrxTi1-xO3/Fe3O4 epitaxial sub-micron sized structures

Large range well ordered epitaxial ferrimagnetic nominally Fe3O4 structures were fabricated by pulsed-laser deposition and embedded in ferroelectric PbZrxTi1-xO3 (x = 0.2, 0.52) epitaxial films. Magnetite dots were investigated by magnetic force microscopy and exhibited magnetic domain contrast at room temperature (RT). Embedding ferroelectric PbZrxTi1-xO3 layers exhibit remnant polarization values close to the values of single epitaxial layers. Transmission electron microscopy demonstrated the epitaxial growth of the composites and the formation of the ferrimagnetic and ferroelectric phases. Physical and structural properties of these composites recommend them for investigations of stress mediated magneto-electric coupling at room temperature. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.3692583]

Characterization of the Kepler-101 planetary system with HARPS-N. A hot super-Neptune with an Earth-sized low-mass companion

We characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysisof Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and iscomposed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolvedand metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1+5.1−4.7 M⊕, radius Rp = 5.77+0.85−0.79 R⊕, and density ρp = 1.45+0.83 −0.48 g cm−3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements makeup a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25+0.19−0.17 R⊕, which implies theabsence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp < 3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 − containing aclose-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance − is certainly of interest for scenarios of planet formation and evolution. This system does not follow the previously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet.

Where are the mid-sized flares of ultracool M dwarfs?

We propose to observe the M8.5 dwarf SCR J1845-6357 with XMM-Newton EPIC for 60 ks. Very low-mass M dwarfs show a distinct drop in X-ray luminosity compared to slightly more massive M dwarfs. Surprisingly, this does not happen at the mass threshold where M dwarfs become fully convective (M4), but at significantly lower masses (M8). These very low mass stars seem to have a flaring behaviour different from earlier type stars: they display either occasional large flares or a very low-level "flickering" in their X-ray light curves, but not the canonical power-law flare-energy distribution observed for the Sun and other cool stars. Our aim is to collect a long-duration light curve for one of the most nearby ultracool dwarfs to quantify how its flare-energy distribution differs from earlier type stars.