Fifty years of wheat breeding in Southern Brazil: yield improvement and associated changes Cinqüenta anos de melhoramento de trigo no Sul do Brasil: melhoramento na produção e mudanças associadas

The objective of this study was to assess the impact of genetic breeding on grain yield, and to identify the physiological traits associated to the increment in yield and their related growth processes, for wheat cultivars grown in Southern Brazil, in the past five decades. Seven wheat cultivars released between 1940 and 1992, were compared for physiological aspects associated with grain yield. Grain yield, biological yield, biomass partitioning, harvest index and grain yield components were also determined. The number of grains per square meter was more affected by plant breeding and was better correlated with grain yield (r = 0.94, p<0.01) than with grain weight (r = -0.39ns). The higher number of grains per square meter was better correlated with the number of grains per spike in the modern cultivars than in the older ones. The genetic gain in grain yield was 44.9 kg ha-1 per year, reflecting important efforts of the breeding programs carried out in Southern Brazil. Grain yield changes, during the period of study, were better associated with biomass production (r = 0.78, p<0.01) than with harvest index (r = 0.65, p<0.01).<br>O objetivo deste trabalho foi avaliar a contribuição do melhoramento genético na produtividade de grãos e identificar as características fisiológicas, associadas ao incremento do rendimento, e os processos de crescimento que as produzem. Foram estudadas sete cultivares de trigo, extensivamente cultivadas na região Sul do Brasil entre 1940 e 1992. As cultivares foram comparadas quanto ao rendimento de grãos, produção biológica, índice de colheita, partição de biomassa e componentes do rendimento. O número de grãos por metro quadrado foi o componente mais afetado pelo melhoramento genético, no período de 52 anos abrangidos pelo estudo, e esteve mais correlacionado ao rendimento de grãos (r = 0,94, p<0,01) do que o peso de grãos (r = -0,39ns). O maior número de grãos por metro quadrado, observado nas cultivares modernas, foi mais correlacionado com seu número de grãos por espiga, em relação às cultivares antigas, o que caracteriza a importância do período de pré-antese na produção de grãos. O ganho genético na produção de grãos foi de 44,9 kg ha-1 por ano e reflete o importante esforço dos programas de melhoramento genético desenvolvidos no Sul do Brasil. As variações em rendimento de grãos, ocorridas no período de estudo, estiveram mais associadas à produção de biomassa (r = 0,78, p<0,01) do que ao índice de colheita (r = 0,65, p<0,01)

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