Superação da dormência de sementes de mucuna-preta pela utilização de "calor seco"

The germination of freshly harvested velvet bean (Mucuna aterrima) seeds was evaluated after "dry heat" treatments under 35, 45 and 55°C, during periods of 0, 2, 4, 6, 8, 16, 24, 48, 72 and 96 hours. The temperature of 55°C was satisfactory to overcome the impermeability of the seed coat, and the exposing periods between 16 and 24 hours were the most effective.Avaliou-se a germinação de sementes recém-colhidas de mucuna preta (Mucuna aterrima) após tratamento com "calor seco", em estufa elétrica com ventilação forçada, nas temperaturas de 35, 45 e 55°C, por períodos de exposição correspondentes a 0, 2, 4, 6, 8,16,24, 48, 72 e 96 horas. A temperatura de 55°C foi adequada para a superação da impermeabilidade do tegumento da semente, sendo mais efetivos os períodos de exposição entre 16 e 24 horas

Plantas invasoras de várzea no estado de São Paulo

Due to competition for water, light and nutrients the weeds are serious problems for certain kind of crops. They are responsible for the reduction in production. The survey and the recognition of different weeds and the their biological study permit a more efficient and economical way of control. The botanical material was collected in lowland crops during three different periods of the year. The purpose was to collect as many different species of weeds as possible. The phenology, the mode of reproduction, the frequency and cycle of weed species are important factors for the rational and effective control. Although the greatest amount of weed species collected belong to the Compositae and Gramineae, the most economically important species belong to the following families: Cyperaceae, Lythraceae, Onagraceae, Polygonaceae, Pontederiaceae and Portulacaceae.As plantas invasoras que ocorrem em uma determinada cultura, constituem sério problema, tendo em vista a concorrência em água, luz e nutrientes que promove com a planta cultivada, determinando uma sensível queda da produtividade da lavoura. O levantamento e reconhecimento dessas plantas, além do estudo biológico, permitem um controle mais eficiente e económico. A coleta do material botânico foi realizada através de visitas em áreas de várzeas cultivadas e em três épocas distintas do ano, com a finalidade de se levantar o maior número possível de espécies invasoras. A fenologia, o modo ou modos de reprodução, frequência e ciclo são elementos indispensáveis para um controle racional e efetivo. Apesar do maior número de espécies pertencerem as famílias Compositae e Gramineae, as espécies de maior importância econômica estão abrigadas também nas famílias Cyperaceae, Lythraceae, Onagraceae, Polygonaceae, Pontederiaceae e Portulacaceae.859

Dust Devil Tracks

Dust devils that leave dark- or light-toned tracks are common on Mars and they can also be found on the Earth’s surface. Dust devil tracks (hereinafter DDTs) are ephemeral surface features with mostly sub-annual lifetimes. Regarding their size, DDT widths can range between ∼1 m and ∼1 km, depending on the diameter of dust devil that created the track, and DDT lengths range from a few tens of meters to several kilometers, limited by the duration and horizontal ground speed of dust devils. DDTs can be classified into three main types based on their morphology and albedo in contrast to their surroundings; all are found on both planets: (a) dark continuous DDTs, (b) dark cycloidal DDTs, and (c) bright DDTs. Dark continuous DDTs are the most common type on Mars. They are characterized by their relatively homogenous and continuous low albedo surface tracks. Based on terrestrial and martian in situ studies, these DDTs most likely form when surficial dust layers are removed to expose larger-grained substrate material (coarse sands of ≥500 μm in diameter). The exposure of larger-grained materials changes the photometric properties of the surface; hence leading to lower albedo tracks because grain size is photometrically inversely proportional to the surface reflectance. However, although not observed so far, compositional differences (i.e., color differences) might also lead to albedo contrasts when dust is removed to expose substrate materials with mineralogical differences. For dark continuous DDTs, albedo drop measurements are around 2.5 % in the wavelength range of 550–850 nm on Mars and around 0.5 % in the wavelength range from 300–1100 nm on Earth. The removal of an equivalent layer thickness around 1 μm is sufficient for the formation of visible dark continuous DDTs on Mars and Earth. The next type of DDTs, dark cycloidal DDTs, are characterized by their low albedo pattern of overlapping scallops. Terrestrial in situ studies imply that they are formed when sand-sized material that is eroded from the outer vortex area of a dust devil is redeposited in annular patterns in the central vortex region. This type of DDT can also be found in on Mars in orbital image data, and although in situ studies are lacking, terrestrial analog studies, laboratory work, and numerical modeling suggest they have the same formation mechanism as those on Earth. Finally, bright DDTs are characterized by their continuous track pattern and high albedo compared to their undisturbed surroundings. They are found on both planets, but to date they have only been analyzed in situ on Earth. Here, the destruction of aggregates of dust, silt and sand by dust devils leads to smooth surfaces in contrast to the undisturbed rough surfaces surrounding the track. The resulting change in photometric properties occurs because the smoother surfaces have a higher reflectance compared to the surrounding rough surface, leading to bright DDTs. On Mars, the destruction of surficial dust-aggregates may also lead to bright DDTs. However, higher reflective surfaces may be produced by other formation mechanisms, such as dust compaction by passing dust devils, as this may also cause changes in photometric properties. On Mars, DDTs in general are found at all elevations and on a global scale, except on the permanent polar caps. DDT maximum areal densities occur during spring and summer in both hemispheres produced by an increase in dust devil activity caused by maximum insolation. Regionally, dust devil densities vary spatially likely controlled by changes in dust cover thicknesses and substrate materials. This variability makes it difficult to infer dust devil activity from DDT frequencies. Furthermore, only a fraction of dust devils leave tracks. However, DDTs can be used as proxies for dust devil lifetimes and wind directions and speeds, and they can also be used to predict lander or rover solar panel clearing events. Overall, the high DDT frequency in many areas on Mars leads to drastic albedo changes that affect large-scale weather patterns

History and Applications of Dust Devil Studies

Studies of dust devils, and their impact on society, are reviewed. Dust devils have been noted since antiquity, and have been documented in many countries, as well as on the planet Mars. As time-variable vortex entities, they have become a cultural motif. Three major stimuli of dust devil research are identified, nuclear testing, terrestrial climate studies, and perhaps most significantly, Mars research. Dust devils present an occasional safety hazard to light structures and have caused several deaths