Non-stochastic behavior of atomic surface diffusion on Cu(111) at all temperatures

Atomic diffusion is usually understood as a succession of random, independent displacements of an adatom over the surface's potential energy landscape. Nevertheless, an analysis of Molecular Dynamics simulations of self-diffusion on Cu(111) demonstrates the existence of different types of correlations in the atomic jumps at all temperatures. Thus, the atomic displacements cannot be correctly described in terms of a random walk model. This fact has a profound impact on the determination and interpretation of diffusion coefficients.Comment: 5 figure

On Galois-Division Multiple Access Systems: Figures of Merit and Performance Evaluation

A new approach to multiple access based on finite field transforms is investigated. These schemes, termed Galois-Division Multiple Access (GDMA), offer compact bandwidth requirements. A new digital transform, the Finite Field Hartley Transform (FFHT) requires to deal with fields of characteristic p, p \neq 2. A binary-to-p-ary (p \neq 2) mapping based on the opportunistic secondary channel is introduced. This allows the use of GDMA in conjunction with available digital systems. The performance of GDMA is also evaluated.Comment: 6 pages, 4 figures. In: XIX Simposio Brasileiro de Telecomunicacoes, 2001, Fortaleza, CE, Brazi

Biodiversidade e Sistemas de Produção Orgânica: Recomendações no Caso da Cana-de-Açúcar.

Este trabalho apresenta os principais resultados dessa pesquisa e discute as relações existentes entre os sistemas de produção tropicais e a biodiversidade faunística no caso dessa propriedade rural, dedicada à produção orgânica de cana-de-açúcar. Finalmente, propõe-se algumas estratégias produtivas visando a estabilidade, a conectividade e a conservação da biodiversidade nessa propriedade rural, passíveis de serem adotadas em outras situações agrícolas.bitstream/item/120546/1/2253.pd

Sistemas de Produção Orgânica de Cana-de-açúcar: monitoramento qualificado de biodiversidade.

O monitoramento sistemático e em bases científicas de indicadores ambientais e faunísticos deve continuar nas áreas da Usina São Francisco e no seu entorno. Ele vem permitindo detectar precocemente os problemas e tomar decisões com base em observação e dados objetivos, os mais rigorosos possíveis, evitando os riscos de experimentações aleatórias ou sem fundamento em agroecologia tropical. Visando ampliar a estabilidade temporal do uso das terras e os benefícios decorrentes, várias sugestões são apresentadas a partir dos resultados obtidos sobre a biodiversidade faunística. Uma das principais recomendações técnicas é no sentido de ampliar o tempo de exploração de cada talhão para oito anos (seis cortes), nos canaviais da Usina São Francisco. Isso parece possível graças às interações que vêm sendo obtidas entre variedades e condições de produção em cultivo orgânico. Isso reduzirá ainda mais a freqüência de subsolagem, aração, gradagem e os movimentos de terra que contribuem para diminuir o teor de matéria orgânica nos solos por mineralização e a estabilidade dos agregados, piorando a estruturação dos solos, aumentando o risco de erosão e a perda de biodiversidade. Isso ampliará a estabilidade ambiental, com ganhos ecológicos para os solos, para os agroecossistemas e ecossistemas, para a preservação ambiental e para a conservação da biodiversidade animal e vegetal.bitstream/item/120536/1/2246.pd

Extracting CKM γ\gamma phase from B±→K±π+π−B^{\pm} \to K^{\pm} \pi^+ \pi^- and B0B^0, Bˉ0→Ksπ+π−\bar B^0 \to K_s \pi^+ \pi^-

We discuss some aspects of the search for CP asymmetry in the three body B decays, revealed through the interference among neighbor resonances in the Dalitz plot. We propose a competitive method to extract the CKM $\gamma$ angle combining Dalitz plot amplitude analysis of $B^{\pm} \to K^{\pm} \pi^+ \pi^-$ and untagged $B^0$, $\bar B^0 \to K_s \pi^+ \pi^-$. The method also obtains the ratio and phase difference between the {\it tree} and {\it penguin} contributions from $B^0$ and $\bar B^0 \to K^{*\pm} \pi^{\mp}$ decays and the CP asymmetry between $B^0$ and $\bar{B^0}$. From Monte Carlo studies of 100K events for the neutral mesons, we show the possibility of measuring $\gamma$.Comment: Revised enlarged version to appear at Phys Rev

Collapse of Primordial Clouds

We present here studies of collapse of purely baryonic Population III objects with masses ranging from $10M_\odot$ to $10^6M_\odot$. A spherical Lagrangian hydrodynamic code has been written to study the formation and evolution of the primordial clouds, from the beginning of the recombination era ($z_{rec} \sim 1500$) until the redshift when the collapse occurs. All the relevant processes are included in the calculations, as well as, the expansion of the Universe. As initial condition we take different values for the Hubble constant and for the baryonic density parameter (considering however a purely baryonic Universe), as well as different density perturbation spectra, in order to see their influence on the behavior of the Population III objects evolution. We find, for example, that the first mass that collapses is $8.5\times10^4M_\odot$ for $h=1$, $\Omega=0.1$ and $\delta_i={\delta\rho / \rho}=(M / M_o)^{-1/3}(1+z_{rec})^{-1}$ with the mass scale $M_o=10^{15}M_\odot$. For $M_o=4\times10^{17}M_\odot$ we obtain $4.4\times10^{4}M_\odot$ for the first mass that collapses. The cooling-heating and photon drag processes have a key role in the collapse of the clouds and in their thermal history. Our results show, for example, that when we disregard the Compton cooling-heating, the collapse of the objects with masses $>8.5\times10^4M_\odot$ occurs earlier. On the other hand, disregarding the photon drag process, the collapse occurs at a higher redshift.Comment: 10 pages, MN plain TeX macros v1.6 file, 9 PS figures. Also available at http://www.iagusp.usp.br/~oswaldo (click "OPTIONS" and then "ARTICLES"). MNRAS in pres

Collapse of Primordial Clouds II. The Role of Dark Matter

In this article we extend the study performed in our previous article on the collapse of primordial objects. We here analyze the behavior of the physical parameters for clouds ranging from $10^7M_\odot$ to $10^{15}M_\odot$. We studied the dynamical evolution of these clouds in two ways: purely baryonic clouds and clouds with non-baryonic dark matter included. We start the calculations at the beginning of the recombination era, following the evolution of the structure until the collapse (that we defined as the time when the density contrast of the baryonic matter is greater than $10^4$). We analyze the behavior of the several physical parameters of the clouds (as, e.g., the density contrast and the velocities of the baryonic matter and the dark matter) as a function of time and radial position in the cloud. In this study all physical processes that are relevant to the dynamical evolution of the primordial clouds, as for example photon-drag (due to the cosmic background radiation), hydrogen molecular production, besides the expansion of the Universe, are included in the calculations. In particular we find that the clouds, with dark matter, collapse at higher redshift when we compare the results with the purely baryonic models. As a general result we find that the distribution of the non-baryonic dark matter is more concentrated than the baryonic one. It is important to stress that we do not take into account the putative virialization of the non-baryonic dark matter, we just follow the time and spatial evolution of the cloud solving its hydrodynamical equations. We studied also the role of the cooling-heating processes in the purely baryonic clouds.Comment: 8 pages, MN plain TeX macros v1.6 file, 13 PS figures. Also available at http://www.iagusp.usp.br/~oswaldo (click "OPTIONS" and then "ARTICLES"). MNRAS in pres