A influência do lobby do etanol na definição da política agrícola e energética dos Estados Unidos (2002-2011)

Pós-graduação em Relações Internacionais (UNESP - UNICAMP - PUC-SP) - FFC

Potenciais aves dispersoras de sementes das espécies vegetais zoocóricas da Mata da Bica, Botucatu - SP

The semidecidual forests, as tropical forests, presents zoochoric dispersal syndrome in the most of their plant species, with approximately one third of frugivorous species responsible for the seeds dispersal are birds. The bills width is a limiting factor, it must be equal or bigger than the seeds width, because the viable seeds dispersal depends on leaving the digestive system after been swallowed hole. Birds and plants inventorys were realized in a semidecidual Forest fragment, in Botucatu – SP, called Mata da Bica. After this, the birds consumers of fuits/seeds were selected (frugivorous, granivorous and onivorous) and also the zoochoric plants, both for building a possibilities matrix, to verify the potential seed dispersers according to the seeds and bills width. Going to the matrix end we can observe a decrease in the interaction possibillities, because the seeds width increases and the bills width decreases. It has been observed that 50,7% seeds could be dispersed by all listed birds, because the seeds were narrower than the narrowest bill. In the other way large seeded species, as Holocalix balansae and Hymemaea courbaril has shown only two possible dispersers: Trogon surrucura and Piaya cayana. There are no possible dispersers to Syagrus oleraceae in the matrix. The need for large birds or other animals that works as large seed disperses demand conservation efforts, since most of these animals need big and conserved areas for their life habits

Evidence for dark matter in the inner Milky Way

The ubiquitous presence of dark matter in the Universe is today a central tenet in modern cosmology and astrophysics(1). Throughout the Universe, the evidence for dark matter is compelling in dwarfs, spiral galaxies, galaxy clusters as well as at cosmological scales. However, it has been historically difficult to pin down the dark matter contribution to the total mass density in the Milky Way, particularly in the innermost regions of the Galaxy and in the solar neighbourhood(2). Here we present an up-to-date compilation of Milky Way rotation curve measurements(3-13), and compare it with state-of-the-art baryonic mass distribution models(14-26). We show that current data strongly disfavour baryons as the sole contribution to the Galactic mass budget, even inside the solar circle. Our findings demonstrate the existence of dark matter in the inner Galaxy without making any assumptions about its distribution. We anticipate that this result will compel new model-independent constraints on the dark matter local density and profile, thus reducing uncertainties on direct and indirect dark matter searches, and will help reveal the structure and evolution of the Galaxy.

The dark matter profile of the Milky Way: a non-parametric reconstruction

We present the results of a new, non-parametric method to reconstruct the Galactic dark matter profile directly from observations. Using the latest kinematic data to track the total gravitational potential and the observed distribution of stars and gas to set the baryonic component, we infer the dark matter contribution to the circular velocity across the Galaxy. The radial derivative of this dynamical contribution is then estimated to extract the dark matter profile. The innovative feature of our approach is that it makes no assumption on the functional form or shape of the profile, thus allowing for a clean determination with no theoretical bias. We illustrate the power of the method by constraining the spherical dark matter profile between 2.5 and 25 kpc away from the Galactic center. The results show that the proposed method, free of widely used assumptions, can already be applied to pinpoint the dark matter distribution in the Milky Way with competitive accuracy, and paves the way for future developments.