Adubação nitrogenada do milho em um sistema de irrigação por aspersão em linha Nitrogen fertilization of corn in a line source sprinkler system

Foi avaliado o efeito do nitrogênio na cultura do milho através da fertirrigação, utilizando um sistema de irrigação por aspersão em linha e uréia como fonte de N. O sistema de aspersão em linha foi constituído por 3 linhas com cinco aspersores cada uma, cujo espaçamento foi de 6 metros entre si e 12 metros entre as linhas. O fertilizante foi aplicado nas linhas externas e a linha central aplicou apenas água. A lâmina de água total aplicada durante o ciclo foi de 650 mm. Essa aplicação foi feita de forma uniforme, e as doses de nitrogênio foram decrescentes na direção perpendicular às linhas externas de aspersores, variando de 353 a 30 kg/ha de N. Os resultados obtidos mostraram que as diferentes dosagens de nitrogênio afetaram os seguintes parâmetros medidos: altura das plantas, altura de inserção das espigas, produtividade, comprimento das espigas, peso de mil grãos e teor de nitrogênio nos grãos. O ponto de máxima produtividade de grãos (7634 kg/ha) foi estimado através de uma função de produção da cultura em relação ao fator doses de nitrogênio. A máxima produtividade estimada pode ser atingida com uma dose de 262,6 kg/ha de N.<br>The nitrogen effect on a corn crop, applied by fertigation through a line source sprinkler system was evaluated, using urea [CO(NH2)2] as nitrogen source. The line source sprinkler system had three pipelines with five sprinklers each. The sprinkler spacing was six meters, and the lateral spacing, twelve meters. Fertigation and irrigaiton were made by the external lines, and the central line was used only for irrigation. The total water depth applied during the crop cicle was 650 mm. This water application was made in an uniform way along the experimental area, and nitrogen levels decreased along the perpendicular direction to the central sprinkler line, ranging from 353 to 30 kg N/ha. Results showed that different nitrogen levels affected the following crop production factors: plant height, corn cob inserction height, corn yield, corn cob length, thousand grain weight, and nitrogen contain of grains. The point of maximum grain yield (7634 kg/ha) was estimated by a crop production function in relation to nitrogen levels. The maximum grain yield was obtained with 262.6 kg N/ha

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