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PCL was blended with pristine multiwalled carbon nanotubes (MWCNT) and with a nanohybrid obtained from the same MWCNT but grafted with low molecular weight PCL, employing concentrations of 0.25 to 5 wt % of MWCNT and MWCNT-g-PCL. Excellent CNT dispersion was found in all samples leading to supernucleation of both nanofiller types. Nanohybrids with 1 wt % or less MWCNTs crystallize faster than nanocomposites (due to supernucleation), while the trend eventually reverses at higher nanotubes content (because of plasticization). Rheological results show that yield-like behavior develops in both nanocomposites, even for the minimum content of carbon nanotubes. In addition, the MWCNT-g-PCL family, when compared with the neat polymer, exhibits lower values of viscosity and modulus in oscillatory shear, and higher compliance in creep. These rheological differences are discussed in terms of the plasticization effect caused by the existence of low molecular weight free and grafted PCL chains in the nanohybrids. © 2017 Wiley Periodicals, Inc. J. Polym. Sci., Part B: Polym. Phys. 2017, 55, 1310–1325.

The influence of composition and crystallization conditions on the behavior of double crystalline poly (ethylene oxide-b-l-lactide) (PEO-b-PLLA) diblock copolymers is investigated. Poly(l-lactide) contents in the synthesized copolymers vary from 50 to 91%, and the molecular weight of the PLLA block ranges from 2 to 20 kg mol-1, while that of the PEO block is kept constant at 2 kg mol-1. In bulk samples, DSC results show a synergistic interaction between the crystallization processes of the two blocks. The PEO block provides heterogeneities and exerts a plasticizing action which favors the crystallization of the PLLA block with a nucleation efficiency of 30%. In contrast, the subsequent crystallization of the PEO block is subject to two opposing effects: (a) the nucleating action of PLLA crystals and (b) the topological and geometrical constraints imposed by PLLA crystals, especially when the PEO content is 20 wt% or less. In the case of ultra thin films, block copolymers with PEO contents equal or smaller than 20 wt% form distorted PLLA single crystals when crystallized from the melt. However, upon increasing the PEO content in the system to 33 wt% (by blending or copolymerization), the distortions disappear and the angle between the {110} growth faces changes from 140° to 121°, since the PEO block acts as a solvent or plasticizer for the PLLA block during the crystallization process. PEO incorporation can therefore tailor the rate and morphology of PLLA block crystallization. TEM and AFM studies allowed direct observation of the PEO block dendritic crystals on the surface of lozenge-shaped PLLA crystals previously formed during cooling from the melt., SCOPUS: ar.j, info:eu-repo/semantics/published

In this paper, the synergistic effects that carbon nanotubes (CNTs) produce on the basic rheological properties and crystallization of polyethylenes with different branch contents and molecular weights was investigated. Multiwalled carbon nanotubes coated with polyethylene (as produced by in situ polymerization) were blended in the melt (in a 1% wt. ratio) with three polyethylene matrices of different molecular weights and branch contents. Transmission electron micrographs demonstrated excellent carbon nanotube dispersion in all samples and the existence of a geometrical percolation network. The rheological and calorimetric properties of the nanocomposites were determined and the results compared to those obtained for neat polyethylene resins. Both Newtonian viscosity and steady-state shear recoverable compliance increased with the addition of CNTs in all cases. However, the increase was strongly dependent on the molecular weight (and dispersity index) of the matrices regardless of the branch content. A novel screening effect of the CNTs network due to the high relaxation times of the matrix with the highest molecular weight was detected. This important result demonstrates that viscoelasticity can hinder the measurement of the rheological percolation threshold of CNTs network depending on the scale of relaxation times involved. Additionally, it was found that in relative terms (comparing each nanocomposite with its neat polyethylene matrix), the Mw values also play a vital role in CNT nucleation besides chain branching content. Both nonisothermal and isothermal nucleation effects caused by CNTs increased as the Mw of the polyethylene matrix decreased in spite of the role played by short chain branches in decelerating their overall crystallization kinetics. The capability for producing more stable lamellae through successive annealing of the nanocomposites as compared to their neat matrices also followed a decreasing trend with molecular weight increases, as indicate

We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K absorption, which has a signal-to-noise (S/N) ratio of 610. The star has a spectroscopically determined distance of 2.7-kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185), HI at +122 km/s and NHI=1.2x10^19 cm-2 is seen. The CaII K spectrum has a S/N = 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9-kpc towards this parcel of gas that may be an intermediate velocity cloud. The lack of intermediate velocity (IV) CaII K absorption towards HD 196426 at a S/N = 500 reinforces a lower distance limit of 700-pc towards this part of Complex gp, where NHI is 1.1x10^19 cm-2 and velocity is +78 km/s. Additionally, no IV CaII K is seen in absorption in the spectrum of HD 19445, which is strong in HI with NHI=8x10^19 cm-2 at -42 km/s, placing a firm although uninteresting lower distance limit of 39-pc to this part of IV South. Finally, no HV CaII K absorption is seen towards HD 115363 at a S/N = 410, placing a lower distance of 3.2-kpc towards the HVC gas at velocity of +224 km/s and NHI=5.2x10^19 cm-2. This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of CaII K absorption sets a lower distance of 3.2-kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System., Comment: Accepted by MNRAS

We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K absorption, which has a signal-to-noise (S/N) ratio of 610. The star has a spectroscopically determined distance of 2.7-kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185), HI at +122 km/s and NHI=1.2x10^19 cm-2 is seen. The CaII K spectrum has a S/N = 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9-kpc towards this parcel of gas that may be an intermediate velocity cloud. The lack of intermediate velocity (IV) CaII K absorption towards HD 196426 at a S/N = 500 reinforces a lower distance limit of 700-pc towards this part of Complex gp, where NHI is 1.1x10^19 cm-2 and velocity is +78 km/s. Additionally, no IV CaII K is seen in absorption in the spectrum of HD 19445, which is strong in HI with NHI=8x10^19 cm-2 at -42 km/s, placing a firm although uninteresting lower distance limit of 39-pc to this part of IV South. Finally, no HV CaII K absorption is seen towards HD 115363 at a S/N = 410, placing a lower distance of 3.2-kpc towards the HVC gas at velocity of +224 km/s and NHI=5.2x10^19 cm-2. This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of CaII K absorption sets a lower distance of 3.2-kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System., Comment: Accepted by MNRAS

We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K absorption, which has a signal-to-noise (S/N) ratio of 610. The star has a spectroscopically determined distance of 2.7-kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185), HI at +122 km/s and NHI=1.2x10^19 cm-2 is seen. The CaII K spectrum has a S/N = 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9-kpc towards this parcel of gas that may be an intermediate velocity cloud. The lack of intermediate velocity (IV) CaII K absorption towards HD 196426 at a S/N = 500 reinforces a lower distance limit of 700-pc towards this part of Complex gp, where NHI is 1.1x10^19 cm-2 and velocity is +78 km/s. Additionally, no IV CaII K is seen in absorption in the spectrum of HD 19445, which is strong in HI with NHI=8x10^19 cm-2 at -42 km/s, placing a firm although uninteresting lower distance limit of 39-pc to this part of IV South. Finally, no HV CaII K absorption is seen towards HD 115363 at a S/N = 410, placing a lower distance of 3.2-kpc towards the HVC gas at velocity of +224 km/s and NHI=5.2x10^19 cm-2. This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of CaII K absorption sets a lower distance of 3.2-kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System., Comment: Accepted by MNRAS