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Search Results: 1 - 10 of 51 matches for " Puerari "
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SUBMISS O DA TUTELA PENAL AO INTERESSE FISCAL NOS CRIMES DE SONEGA O TRIBUTáRIA
Adriano Farias Puerari
Revista Eletr?nica do Curso de Direito da UFSM , 2013, DOI: 10.5902/198136947524
Abstract: Atualmente, a larga expans o das novas tecnologias lidera uma evolu o cada vez maior do fen meno da globaliza o, que tem como um de seus muitos desdobramentos o incremento da criminalidade econ mica. O desenvolvimento político e econ mico de um país é reflexo da abrangência do Direito Econ mico que o tutela e, consequentemente, da amplia o do Direito Penal Econ mico, pois o tratamento de quest es que envolvam prote o aos crimes de colarinho branco é condi o de possibilidade à prote o e à defesa de uma ordem jurídica justa. Nesse contexto, o presente artigo tem por objetivo analisar a evolu o da delinquência econ mica, identificando o bem jurídico protegido pelo Direito Penal Econ mico de modo a confrontar a tutela penal frente aos interesses arrecadatórios da Administra o, especialmente para demonstrar a impunidade que gira em torno dos delitos de sonega o fiscal.
FORMATION OF RINGS BY GALACTIC COLLISIONS
I. Puerari,L. Aguilar
Revista mexicana de astronomía y astrofísica , 2009,
Abstract: We study the formation and evolution of rings in disk galaxies by the impact of a spherical companion. This study is carried out by using numerical simulations and fully self-consistent models. We have tested a number of target disk galaxies with di erent radial scalelengths or central radial velocity dispersion, and a number of companions with di erent masses and radial scalelengths. We also have tested a large number of initial conditions to produce collisions with di erent velocities, inclinations and impact parameters. Our main results are: (a) strong interactions (high companion mass and/or slow impact velocity) result in rings with constant expansion velocity; (b) our tested collisions are very e ective to heat the disk, increasing the radial velocity dispersion; (c) the rings created by collisions are certainly density waves; (d) inclined-central collisions create inclined rings, but they are not e ective to displace the nucleus of the target; (e) perpendicular-peripheral collisions are more e ective to displace the nucleus, as well as to create inclined rings, which remain inclined for a long period of time (some 108 years).
A Morphological Method to Determine Co-Rotation Radii in Spiral Galaxies
Ivanio Puerari,Horacio Dottori
Physics , 1996, DOI: 10.1086/310502
Abstract: Shock induced star formation in a stellar density wave scenario produces an azimuthal gradient of ages across the spiral arms which has opposite signs on either side of the corotation resonance (CR). We present a method based on the Fourier analysis of azimuthal profiles, to locate the CR and determine the arm character (trailing or leading) in spiral galaxies. Basically, we compare the behavior of the phase angle of the two-armed spiral in blue and infrared colors which pick out respectively young and older disk stellar population. We illustrate the method using theoretical leading and trailing, spirals. We have also applied the method to the spiral galaxies NGC 7479, for which we confirm the reported leading arms, and NGC 1832. In these galaxies we find two and three CRs respectively.
A perturbative analysis of Quasi-Radial density waves in galactic disks
X. Hernandez,I. Puerari
Physics , 2011,
Abstract: The theoretical understanding of density waves in disk galaxies starts from the classical WKB perturbative analysis of tight-winding perturbations, the key assumption being that the potential due to the density wave is approximately radial. The above has served as a valuable guide in aiding the understanding of both simulated and observed galaxies, in spite of a number of caveats being present. The observed spiral or bar patterns in real galaxies are frequently only marginally consistent with the tight-winding assumption, often in fact, outright inconsistent. Here we derive a complementary formulation to the problem, by treating quasi-radial density waves under simplified assumptions in the linear regime. We assume that the potential due to the density wave is approximately tangential, and derive the corresponding dispersion relation of the problem. We obtain an instability criterion for the onset of quasi-radial density waves, which allows a clear understanding of the increased stability of the higher order modes, which appear at progressively larger radii, as often seen in real galaxies. The theory naturally yields a range of pattern speeds for these arms which appears constrained by the condition $\Omega_{p}<\Omega_{0} \pm \kappa /m$. For the central regions of galaxies where solid body rotation curves might apply, we find weak bars in the oscillatory regime with various pattern speeds, including counter rotating ones, and a prediction for $\Omega_{p}$ to increase towards the centre, as seen in the rapidly rotating bars within bars of some numerical simulations. We complement this study with detailed numerical simulations of galactic disks and careful Fourier analysis of the emergent perturbations, which support the theory presented.
Formation of massive counter-rotating disks: an alternative scenario
I. Puerari,D. Pfenniger
Physics , 1999, DOI: 10.1023/A:1017581325673
Abstract: In this contribution, we investigate the scenario of major mergers between galaxies of comparable mass to the formation of massive counter-rotating disks. Such a scenario can be ruled out in general because they produce rather ellipticals. Yet for a narrow range of initial conditions, major mergers can nevertheless produce anyway rare galaxies such as NGC 4550, and so they are viable alternatives for the formation of these counter-rotating systems. The scenario is successful in producing a remarkably axisymmetric disk possessing strongly counter-rotating populations.
Toward a dust penetrated classification of the evolved stellar Population II disks of galaxies
David L. Block,Ivanio Puerari
Physics , 1998,
Abstract: (abridged): To derive a coherent physical framework for the excitation of spiral structure in galaxies, one must consider the co-existence of two different dynamical components: a gas-dominated Population I disk (OB associations, HII regions, cold interstellar HI gas) and an evolved stellar Population II component. The Hubble classification scheme has as its focus, the morphology of the Population I component only. In the near-infrared, the morphology of evolved stellar disks indicates a simple classification scheme: the dominant Fourier m-mode in the dust penetrated regime, and the associated pitch angle. On the basis of deprojected K$'$ (2.1$\mu m$) images, we propose that the evolved stellar disks may be grouped into three principal dust penetrated archetypes: those with tightly wound stellar arms characterised by pitch angles at K$'$ of $\sim$ 10$^{\circ}$ (the $\alpha$ class), an intermediate group with pitch angles of $\sim$ 25$^{\circ}$ (the $\beta$ class) and thirdly, those with open spirals demarcated by pitch angles at K$'$ of $\sim$ 40$^{\circ}$ (the $\gamma$ bin). Both optically flocculent or grand design galaxies can reside within the {\it same} dust penetrated morphological bin. Any specific dust penetrated archetype may be the resident disk of {\it both} an early or late type galaxy in the optical regime. There is no correlation between our dust penetrated classes and optical Hubble binning; the Hubble tuning fork does not constrain the morphology of the old stellar Population II disks.
Color Correlations in (S+S) Binary Galaxies I. The Holmberg Effect
Hector Hernandez Toledo,Ivanio Puerari
Physics , 2000,
Abstract: Relying on his photometry of galaxies, Holmberg (1958) found, more than 40 years ago, that the color indices of paired galaxies were closely correlated. Our deep broad-band BVRI CCD photometry of 45 (S+S) pairs from the Karachentsev (1972) catalogue (see Hernandez Toledo and Puerari, this volume), and additional (B-V) color information from the literature (50 extra (S+S) pairs), help us to confirm the effect. This "Holmberg Effect" has long been remained unverified and not explained yet.
BVRI Surface Photometry of (S+S) Binary Galaxies
Hector Hernandez Toledo,Ivanio Puerari
Physics , 2000,
Abstract: We report the first results of our multicolour broad-band BVRI photometry for a statistically well defined sample of interacting pairs, drawn from the Catalogue of Isolated Pairs of Galaxies in the Northern Hemisphere Karachentsev (1972). At present, the details of photometric structure of disk-disk (S+S) galaxies are just beginning to be studied because of their intrinsic difficulties. We take advantage of the statistical properties of this well defined sample of interacting galaxies to try to isolate the main structural components of galaxies. Due to their environmental simplicity (compared to groups and clusters), the sample provides an unique opportunity to peform a photometric study of galaxies and their structural components in a non-equilibrium configuration. In this contribution, the first results of a deep multicolour (BVRI) photometric study of a sample of 45 (S+S) isolated pairs of galaxies is presented. Our attention is focused on the morphology and the global photometric properties (integrated magnitudes, colours and mean surface brightness profiles).
O PROCESSO JUDICIAL ELETR NICO E AS TRADI ES (INAUTêNTICAS) PROCESSUAIS
Cristiano Becker Isaia,Adriano Farias Puerari
Revista Direitos Emergentes na Sociedade Global , 2012, DOI: 10.5902/231630546259
Abstract: As novas tecnologias de informa o e comunica o, no contexto do Poder Judiciário, vêm sendo utilizadas com o objetivo de implementar melhorias de gest o e atendimento ao cidad o, notadamente em rela o à efetividade na presta o jurisdicional. Nesse panorama, o presente artigo analisa os princípios constitucionais do processo sob a ótica da nova sistemática processual adotada com a implanta o do processo judicial eletr nico, este instituído pela Lei no 11.419/2006. Para tanto, é realizado um exame dos fundamentos das garantias constitucionais de acesso à justi a e da razoável duran o do processo, bem como das condi es de possibilidade para efetividade da presta o jurisdicional. Em seguida investigam-se as altera es produzidas pelo e-Processo em rela o ao problema da morosidade do Poder Judiciário e o alcance dessas modifica es no que tange à preserva o das garantias constitucionais do processo, mormente se considerado o quadro de exclus o digital do país. Por fim, no contexto da celeridade de tramita o dos processos digitais, reflete-se, sob um viés hermenêutico, acerca da inefetividade da reforma trazida pela lei do processo eletr nico na manuten o dos reclames de instantaneidade de uma sociedade da informa o, o que se deve a fixa o pela ordinariza o, heran a do racionalismo. http://dx.doi.org/10.5902/231630546259
Formation of rings in galactic discs by infalling small companions
E. Athanassoula,I. Puerari,A. Bosma
Physics , 1996, DOI: 10.1093/mnras/286.2.284
Abstract: We use N-body simulations to study the formation of rings in a disc galaxy by the impact of a small spherical companion. Both barred and nonbarred target discs are considered. We discuss the effect of the properties of the target disc (distribution of mass in the disc, velocity dispersion, etc.) as well as of the mass and orbit of the companion on the properties of the rings, such as their amplitude, width, shape, expansion velocity and lifetime. In particular the amplitude, width, lifetime and expansion velocity of the first ring increase considerably with companion mass, and so does the expansion velocity of the particles in it and the total extent of the disc after the interaction. We also discuss the formation and evolution of spokes and show that they can be caused by companions of relatively small mass. In our three examples of oblique impacts on barred target galaxies we note important transient displacements of the bar, as well as changes of its pattern speed and size. An asymmetric pseudoring is formed in each case, and during the first stages of its evolution the bar forms part of it.
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