Atributos químicos e físicos de um Argissolo Vermelho-Amarelo em sistema integrado de produção agroecológica Chemical and physical attributes of an Udult soil in agroecological production systems

O objetivo deste trabalho foi avaliar a influência de sistemas de manejo agroecológico sobre os atributos físicos e químicos de um Argissolo Vermelho-Amarelo. Foram selecionadas as seguintes áreas: preparo convencional (milho/feijão); plantio direto (berinjela/milho); consórcio maracujá/Desmodium sp.; área cultivada com figo; e sistema agroflorestal (SAF). Amostras indeformadas de solo foram coletadas em duas profundidades (0-5 e 5-10 cm) e em duas épocas (verão/2005 e inverno/2006). As propriedades edáficas analisadas foram: densidade do solo (Ds); volume total de poros; diâmetro médio ponderado (DMP) e diâmetro médio geométrico (DMG) de agregados; pH, Al, Ca+Mg, K, H+Al, P e carbono orgânico total (COT). Os maiores valores de Ds, P e K foram verificados na área de figo. O sistema milho/feijão apresentou os menores valores de DMP e DMG. Os maiores valores de DMP e DMG foram observados nos sistemas maracujá/Desmodium e berinjela/milho. As diferenças entre os valores de COT foram maiores à profundidade de 5-10 cm. O SAF apresentou maiores percentuais de porosidade total. A análise de componentes principais mostrou que a área cultivada com figo está associada a maiores índices de fertilidade do solo.<br>The objective of this study was to evaluate the influence of agroecological management systems on physical and chemical attributes of an Udult soil. The following areas were selected: conventional tillage (corn/beans); no tillage (eggplant/corn); consortium of passion fruit/Desmodium sp.; fig cultivation; and an agroforestry system (AFS). The undisturbed soil samples were taken from two layers (0-5 and 5-10 cm) and in two periods, the summer of 2005 and the winter of 2006. The soil properties analyzed were: bulk density (Ds), total pore volume, mean weight diameter (MWD) and mean geometric diameter (MGD) of aggregates, pH, Al, Ca+Mg, K, H+Al, P, and total organic carbon (TOC). The highest values of Ds, P and K were observed in the fig area. The system with corn/beans had the lowest MWD and MGD values. The highest values of MWD and MGD were observed in the passion fruit/Desmodium and eggplant/corn systems. Differences in TOC were greater at the 5-10 cm depth. Soil in the AFS had the highest percentage of total porosity. The analysis of main components showed that the area cultivated with fig had the highest soil fertility

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 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 $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) 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 $\,{M}_{\odot }$. 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 $\sim 40\,{\rm{Mpc}}$) 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 $\sim 9$ and $\sim 16$ 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 NGC 4993 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