Compatibilização de blendas de poliamida 6/ABS usando os copolímeros acrílicos reativos MMA-GMA e MMA-MA. Parte 2: Comportamento termomecânico e morfológico das blendas Compatibilization of Polyamide 6/ABS blends using MMA-GMA and MMA-MA reactive acrylic copolymers. Part 2. Thermal-mechanical and morphological behavior of blends

Blendas poliméricas de poliamida 6 (PA6) com acrilonitrila-butadieno-estireno (ABS) foram preparadas em extrusora de rosca dupla, utilizando-se os copolímeros metacrilato de metila - metacrilato de glicidila (MMA-GMA) e metacrilato de metila-anidrido maléico (MMA-MA) como agentes de compatibilização. O ABS, por si só, não foi capaz de tenacificar a PA6, apresentando uma morfologia de fases com grandes e pequenos aglomerados na matriz PA6. A introdução do copolímero MMA-GMA, como compatibilizante do sistema, não melhorou significativamente as propriedades de impacto da blenda PA6/ABS. As fotomicrografias obtidas por microscopia eletrônica de transmissão (MET) indicaram uma morfologia com duas populações distintas de ABS: aglomerados e pequenas partículas dispersas, resultando em uma distribuição não-uniforme de domínios de ABS. A blenda compatibilizada com MMA-MA foi supertenaz (> 800 J/m) na temperatura ambiente e em baixas temperaturas (~ -10 °C), com baixas concentrações de compatibilizante e baixos teores de MA no copolímero. As blendas PA6/ABS compatibilizadas com MMA-MA apresentaram uma morfologia de partículas bem dispersas e adequadamente distribuídas na matriz, evidenciando a presença efetiva do copolímero como agente de compatibilização reativo deste sistema.<br>Blends of Polyamide 6 (PA6) with acrylonitrile-butadiene-styrene (ABS) were prepared in a corotating twin-screw extruder, using the poly(methyl methacrylate-co-glycidyl methacrylate) (MMA-GMA) and poly(methyl methacrylate-co-maleic anhydride) (MMA-MA) copolymers as compatibilizing agents. The ABS by itself was not capable to toughen PA6 and showed a phase morphology with large and small agglomerates in the PA6 matrix. The introduction of MMA-GMA copolymer as a compatibilizing agent in the system did not significantly improve the impact properties of PA6/ABS blend. Transmission electron microscope (TEM) photomicrographs indicated a morphology with two distinct populations of ABS: agglomerates and small dispersed particles resulting in a non-uniform distribution of ABS domains. The compatibilized blend with MMA-MA was super-tough (> 800 J/m) at room temperature and low temperature (~ -10 °C) with small amounts of MA in the copolymer and small amounts of compatibilizer in the blend. The PA6/ABS compatibilized blends with MMA-MA showed a morphology of well dispersed and distributed rubber particles in PA6 matrix, thus demonstrating the effective presence of the copolymer as a compatibilizing reactive agent of this system

GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run

The third Gravitational-Wave Transient Catalog (GWTC-3) describes signals detected with Advanced LIGO and Advanced Virgo up to the end of their third observing run. Updating the previous GWTC-2.1, we present candidate gravitational waves from compact binary coalescences during the second half of the third observing run (O3b) between 1 November 2019, 15∶00 Coordinated Universal Time (UTC) and 27 March 2020, 17∶00 UTC. There are 35 compact binary coalescence candidates identified by at least one of our search algorithms with a probability of astrophysical origin pastro>0.5. Of these, 18 were previously reported as low-latency public alerts, and 17 are reported here for the first time. Based upon estimates for the component masses, our O3b candidates with pastro>0.5 are consistent with gravitational-wave signals from binary black holes or neutron-star-black-hole binaries, and we identify none from binary neutron stars. However, from the gravitational-wave data alone, we are not able to measure matter effects that distinguish whether the binary components are neutron stars or black holes. The range of inferred component masses is similar to that found with previous catalogs, but the O3b candidates include the first confident observations of neutron-star-black-hole binaries. Including the 35 candidates from O3b in addition to those from GWTC-2.1, GWTC-3 contains 90 candidates found by our analysis with pastro>0.5 across the first three observing runs. These observations of compact binary coalescences present an unprecedented view of the properties of black holes and neutron stars. © 2023 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the "https://creativecommons.org/licenses/by/4.0/"Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI.Open access articleThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at [email protected]

Search for gravitational waves associated with fast radio bursts detected by CHIME/FRB during the LIGO-Virgo observing run O3a

We search for gravitational-wave (GW) transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project, during the first part of the third observing run of Advanced LIGO and Advanced Virgo (2019 April 1 15:00 UTC–2019 October 1 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets both binary neutron star (BNS) and neutron star– black hole (NSBH) mergers. A targeted search for generic GW transients was conducted on 40 FRBs. We find no significant evidence for a GW association in either search. Given the large uncertainties in the distances of our FRB sample, we are unable to exclude the possibility of a GW association. Assessing the volumetric event rates of both FRB and binary mergers, an association is limited to 15% of the FRB population for BNS mergers or 1% for NSBH mergers. We report 90% confidence lower bounds on the distance to each FRB for a range of GW progenitor models and set upper limits on the energy emitted through GWs for a range of emission scenarios. We find values of order 1051–1057 erg for models with central GW frequencies in the range 70–3560 Hz. At the sensitivity of this search, we find these limits to be above the predicted GW emissions for the models considered. We also find no significant coincident detection of GWs with the repeater, FRB 20200120E, which is the closest known extragalactic FRB

First joint observation by the underground gravitational-wave detector KAGRA with GEO 600

International audienceWe report the results of the first joint observation of the KAGRA detector with GEO 600. KAGRA is a cryogenic and underground gravitational-wave detector consisting of a laser interferometer with 3 km arms, located in Kamioka, Gifu, Japan. GEO 600 is a British–German laser interferometer with 600 m arms, located near Hannover, Germany. GEO 600 and KAGRA performed a joint observing run from April 7 to 20, 2020. We present the results of the joint analysis of the GEO–KAGRA data for transient gravitational-wave signals, including the coalescence of neutron-star binaries and generic unmodeled transients. We also perform dedicated searches for binary coalescence signals and generic transients associated with gamma-ray burst events observed during the joint run. No gravitational-wave events were identified. We evaluate the minimum detectable amplitude for various types of transient signals and the spacetime volume for which the network is sensitive to binary neutron-star coalescences. We also place lower limits on the distances to the gamma-ray bursts analyzed based on the non-detection of an associated gravitational-wave signal for several signal models, including binary coalescences. These analyses demonstrate the feasibility and utility of KAGRA as a member of the global gravitational-wave detector network