Catalytic Transformations of Alkynes via Ruthenium Vinylidene and Allenylidene Intermediates

NOTICE: This is the peer reviewed version of the following book chapter: Varela J. A., González-Rodríguez C., Saá C. (2014). Catalytic Transformations of Alkynes via Ruthenium Vinylidene and Allenylidene Intermediates. In: Dixneuf P., Bruneau C. (eds) Ruthenium in Catalysis. Topics in Organometallic Chemistry, vol 48, pp. 237-287. Springer, Cham. [doi: 10.1007/3418_2014_81]. This article may be used for non-commercial purposes in accordance with Springer Verlag Terms and Conditions for self-archiving.Vinylidenes are high-energy tautomers of terminal alkynes and they can be stabilized by coordination with transition metals. The resulting metal-vinylidene species have interesting chemical properties that make their reactivity different to that of the free and metal π-coordinated alkynes: the carbon α to the metal is electrophilic whereas the β carbon is nucleophilic. Ruthenium is one of the most commonly used transition metals to stabilize vinylidenes and the resulting species can undergo a range of useful transformations. The most remarkable transformations are the regioselective anti-Markovnikov addition of different nucleophiles to catalytic ruthenium vinylidenes and the participation of the π system of catalytic ruthenium vinylidenes in pericyclic reactions. Ruthenium vinylidenes have also been employed as precatalysts in ring closing metathesis (RCM) or ring opening metathesis polymerization (ROMP). Allenylidenes could be considered as divalent radicals derived from allenes. In a similar way to vinylidenes, allenylidenes can be stabilized by coordination with transition metals and again ruthenium is one of the most widely used metals. Metalallenylidene complexes can be easily obtained from terminal propargylic alcohols by dehydration of the initially formed metal-hydroxyvinylidenes, in which the reactivity of these metal complexes is based on the electrophilic nature of Cα and Cγ, while Cβ is nucleophilic. Catalytic processes based on nucleophilic additions and pericyclic reactions involving the π system of ruthenium allenylidenes afford interesting new structures with high selectivity and atom economy

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Relativistic Binaries in Globular Clusters

Galactic globular clusters are old, dense star systems typically containing 10\super{4}--10\super{7} stars. As an old population of stars, globular clusters contain many collapsed and degenerate objects. As a dense population of stars, globular clusters are the scene of many interesting close dynamical interactions between stars. These dynamical interactions can alter the evolution of individual stars and can produce tight binary systems containing one or two compact objects. In this review, we discuss theoretical models of globular cluster evolution and binary evolution, techniques for simulating this evolution that leads to relativistic binaries, and current and possible future observational evidence for this population. Our discussion of globular cluster evolution will focus on the processes that boost the production of hard binary systems and the subsequent interaction of these binaries that can alter the properties of both bodies and can lead to exotic objects. Direct {\it N}-body integrations and Fokker--Planck simulations of the evolution of globular clusters that incorporate tidal interactions and lead to predictions of relativistic binary populations are also discussed. We discuss the current observational evidence for cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries as well as possible future detection of relativistic binaries with gravitational radiation.Comment: 88 pages, 13 figures. Submitted update of Living Reviews articl

Localization and broadband follow-up of the gravitational-wave transient GW150914

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams

Multi-messenger astrophysics with THESEUS in the 2030s

Multi-messenger astrophysics is becoming a major avenue to explore the Universe, with the potential to span a vast range of redshifts. The growing synergies between different probes is opening new frontiers, which promise profound insights into several aspects of fundamental physics and cosmology. In this context, THESEUS will play a central role during the 2030s in detecting and localizing the electromagnetic counterparts of gravitational wave and neutrino sources that the unprecedented sensitivity of next generation detectors will discover at much higher rates than the present. Here, we review the most important target signals from multi-messenger sources that THESEUS will be able to detect and characterize, discussing detection rate expectations and scientific impact

Influência do resfriamento dinâmico na medição da tensão limite de escoamento

Non-Newtonian fluids may present several complex characteristics, such as viscoelasticity, plasticity and thixotropy. Understanding the behaviour of these materials is essential to facilitate its applicability, since many of them are present in daily life, such as gels, chocolate, and mayonnaise. The material studied on the present work was an waxy crude oil. The oil, present in reservoirs located in deep water, when subjected to low temperatures during production shutdowns, precipitates its paraffin, creating a structure which may be very resistant to flow. Thus, the formed material may represent a great difficulty to production restart. The design of pumps and compressors used in these systems depend on a rheological property called yield stress and therefore, it is essential to obtain reliable values of this rheological parameter. However, the complex behaviour, and the dependence of the crude oil characteristics on the shearing and temperature history make this a challenging task. Besides these, other factors may influence the measurement of yield stress, as the effect of wall slip and if the cooling is static or dynamic. This work shows the variation of yield stress for tests with dynamic cooling. The imposition of a stress during cooling caused the reduction in yield stress 0. Increasing the imposed stress, 0 decreased until it reached a minimum. Next, it was noticed an increase in yield stress with increasing imposed stress. The experiments carried out in this work were made in a commercial stress control rheometer. The effect of wall slip was tested by comparing smooth and rough geometries and it was verified signs of its presence, with the reduction of yield stress for smooth geometries. The equation of Weissenberg-Rabinowitsch, used for correction of the inhomogeneity of the shear stress along the radius geometry, seemed to be not necessary for the demonstrated results.Fluidos não newtonianos podem apresentar diversas características complexas, como a viscoelasticidade, plasticidade e tixotropia. Entender o comportamento de materiais tão complexos é fundamental para facilitar sua aplicabilidade, já que muitos estão presentes no cotidiano das pessoas, como géis, chocolate e maionese. O material estudado no presente trabalho foi um petróleo parafínico. O petróleo, presente em bacias localizadas em águas profundas, quando submetido a baixas temperaturas durante paradas de produção, precipita suas parafinas dando origem a uma estrutura que pode ser muito resistente ao escoamento. Dessa forma, o material formado pode representar uma grande dificuldade para o reinício da produção. O dimensionamento das bombas e compressores utilizados para retomada da produção depende de uma propriedade reológica denominada tensão limite de escoamento e, por isso, é fundamental obter valores confiáveis desse parâmetro reológico. No entanto, o comportamento complexo, e a dependência das características do petróleo com o histórico de cisalhamento e temperatura tornam a tarefa desafiadora. Outros fatores podem influenciar na medição da tensão limite de escoamento, como o efeito do escorregamento na parede do sensor da geometria e se o resfriamento é estático ou dinâmico. Este trabalho mostra a variação da tensão limite de escoamento para ensaios com resfriamento dinâmico. A imposição de tensão durante o resfriamento causou a redução da tensão limite de escoamento 0. Elevando-se a tensão imposta, 0 reduziu até atingir um valor mínimo. Em seguida, percebeu-se um aumento da tensão limite de escoamento com o aumento da tensão imposta. Os experimentos realizados neste trabalho foram feitos em um reômetro comercial do tipo tensão controlada (“stress controlled”). O efeito de escorregamento da amostra foi testado comparando geometrias com superfícies lisas e ranhuradas e foi possível verificar sinais de sua presença, com a redução da tensão limite de escoamento para geometrias lisas. A equação de Weissenberg-Rabinowitsch, utilizada para correção da não homogeneidade da tensão de cisalhamento ao longo do raio da geometria, mostrou-se não necessária para os resultados demonstrados

Localization and broadband follow-up of the gravitational-wave transient GW150914

A gravitational-wave transient was identified in data recorded by the Advanced LIGO detectors on 2015 September 14. The event candidate, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the gravitational wave data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network Circulars, giving an overview of the participating facilities, the gravitational wave sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the electromagnetic data and results of the electromagnetic follow-up campaign will be disseminated in the papers of the individual teams