Topologically massive yang-mills field on the null-plane: A hamilton-jacobi approach

Non-abelian gauge theories are super-renormalizable in 2+1 dimensions and suffer from infrared divergences. These divergences can be avoided by adding a Chern-Simons term, i.e., building a Topologically Massive Theory. In this sense, we are interested in the study of the Topologically Massive Yang-Mills theory on the Null-Plane. Since this is a gauge theory, we need to analyze its constraint structure which is done with the Hamilton-Jacobi formalism. We are able to find the complete set of Hamiltonian densities, and build the Generalized Brackets of the theory. With the GB we obtain a set of involutive Hamiltonian densities, generators of the evolution of the system. © 2010 American Institute of Physics.

Chaotic diffusion caused by close encounters with several massive asteroids: II. the regions of (10) Hygiea, (2) Pallas, and (31) Euphrosyne

Context. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families. © 2013 ESO.

Note on linearized new massive gravity in arbitrary dimensions

By means of a triple master action we deduce here a linearized version of the new massive gravity (NMG) in arbitrary dimensions. The theory contains a 4th-order and a 2nd-order term in derivatives. The 4th-order term is invariant under a generalized Weyl symmetry. The action is formulated in terms of a traceless ημνΩμνρ=0 mixed symmetry tensor Ωμνρ=-Ωμρν and corresponds to the massive Fierz-Pauli action with the replacement e μν=∂ρΩμνρ. The linearized 3D and 4D NMG theories are recovered via the invertible maps Ωμνρ=Ïμνρβhβμ and Ωμνρ=ÏμνργδT [γδ]μ respectively. The properties h μν=hνμ and T[[γδ]μ]= 0 follow from the traceless restriction. The equations of motion of the linearized NMG theory can be written as zero curvature conditions ∂νTρμ-∂ρT νμ=0 in arbitrary dimensions. © 2013 American Physical Society.

Correspondence between the self-dual model and the topologically massive electrodynamics: A new view

Following the study of the Topologically Massive Theories under the Hamilton-Jacobi, we now analyze the constraint structure of the Self-Dual model as well as its correspondence with the Topologically Massive Electrodynamics. © 2013 American Institute of Physics.

Efeito do uso do cogumelo Agaricus brasiliensis no estado nutricional, na frequência e intensidade dos efeitos adversos da terapia medicamentosa e na resposta bioquímica hepática em indivíduos com hepatite crônica pelo vírus C: estudo prospectivo, randomizado, duplo cego, placebo controlado

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Scalar source in circular motion interacting with massive klein-gordon field in Minkowski spacetime

We analyze the scalar radiation emitted by a source in uniform circular motion in Minkowski spacetime interacting with a massive Klein-Gordon field. We assume the source rotating around a central object due to a Newtonian force. By considering the canonical quantization of this field, we use perturbation theory to compute the radiation emitted at the tree level. Regarding the initial state of the field as being the Minkowski vacuum, we compute the emission amplitude for the rotating source, assuming it as being minimally coupled to the massive Klein-Gordon field. We then compute the power emitted by the swirling source as a function of its angular velocity, as measured by asymptotic static observers.

Topologically massive Yang-Mills: A Hamilton-Jacobi constraint analysis

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Dimensional reduction of the massless limit of the linearized 'New Massive Gravity'

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Search for massive resonances in dijet systems containing jets tagged as W or Z boson decays in pp collisions at root s=8 TeV

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Search for massive resonances decaying into pairs of boosted bosons in semi-leptonic final states at root s=8 TeV

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

QCD chiral symmetry restoration with a large number of quarks in a model with a confining propagator and dynamically massive gluons

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Free massive particles with total energy E

We analyze free elementary particles with a rest mass m and total energy E

X-Ray studies of the physics of matter around super-massive black-holes in nearby Seyfert galaxies

Seyfert galaxies are the closest active galactic nuclei. As such, we can use them to test the physical properties of the entire class of objects. To investigate their general properties, I took advantage of different methods of data analysis. In particular I used three different samples of objects, that, despite frequent overlaps, have been chosen to best tackle different topics: the heterogeneous BeppoS AX sample was thought to be optimized to test the average hard X-ray (E above 10 keV) properties of nearby Seyfert galaxies; the X-CfA was thought the be optimized to compare the properties of low-luminosity sources to the ones of higher luminosity and, thus, it was also used to test the emission mechanism models; finally, the XMM–Newton sample was extracted from the X-CfA sample so as to ensure a truly unbiased and well defined sample of objects to define the average properties of Seyfert galaxies. Taking advantage of the broad-band coverage of the BeppoS AX MECS and PDS instruments (between ~2-100 keV), I infer the average X-ray spectral propertiesof nearby Seyfert galaxies and in particular the photon index (~1.8), the high-energy cut-off (~290 keV), and the relative amount of cold reflection (~1.0). Moreover the unified scheme for active galactic nuclei was positively tested. The distribution of isotropic indicators used here (photon index, relative amount of reflection, high-energy cut-off and narrow FeK energy centroid) are similar in type I and type II objects while the absorbing column and the iron line equivalent width significantly differ between the two classes of sources with type II objects displaying larger absorbing columns. Taking advantage of the XMM–Newton and X–CfA samples I also deduced from measurements that 30 to 50% of type II Seyfert galaxies are Compton thick. Confirming previous results, the narrow FeK line is consistent, in Seyfert 2 galaxies, with being produced in the same matter responsible for the observed obscuration. These results support the basic picture of the unified model. Moreover, the presence of a X-ray Baldwin effect in type I sources has been measured using for the first time the 20-100 keV luminosity (EW proportional to L(20-100)^(−0.22±0.05)). This finding suggests that the torus covering factor may be a function of source luminosity, thereby suggesting a refinement of the baseline version of the unifed model itself. Using the BeppoSAX sample, it has been also recorded a possible correlation between the photon index and the amount of cold reflection in both type I and II sources. At a first glance this confirms the thermal Comptonization as the most likely origin of the high energy emission for the active galactic nuclei. This relation, in fact, naturally emerges supposing that the accretion disk penetrates, depending to the accretion rate, the central corona at different depths (Merloni et al. 2006): the higher accreting systems hosting disks down to the last stable orbit while the lower accreting systems hosting truncated disks. On the contrary, the study of the well defined X–C f A sample of Seyfert galaxies has proved that the intrinsic X-ray luminosity of nearby Seyfert galaxies can span values between 10^(38−43) erg s^−1, i.e. covering a huge range of accretion rates. The less efficient systems have been supposed to host ADAF systems without accretion disk. However, the study of the X–CfA sample has also proved the existence of correlations between optical emission lines and X-ray luminosity in the entire range of L_(X) covered by the sample. These relations are similar to the ones obtained if high-L objects are considered. Thus the emission mechanism must be similar in luminous and weak systems. A possible scenario to reconcile these somehow opposite indications is assuming that the ADAF and the two phase mechanism co-exist with different relative importance moving from low-to-high accretion systems (as suggested by the Gamma vs. R relation). The present data require that no abrupt transition between the two regimes is present. As mentioned above, the possible presence of an accretion disk has been tested using samples of nearby Seyfert galaxies. Here, to deeply investigate the flow patterns close to super-massive black-holes, three case study objects for which enough counts statistics is available have been analysed using deep X-ray observations taken with XMM–Newton. The obtained results have shown that the accretion flow can significantly differ between the objects when it is analyzed with the appropriate detail. For instance the accretion disk is well established down to the last stable orbit in a Kerr system for IRAS 13197-1627 where strong light bending effect have been measured. The accretion disk seems to be formed spiraling in the inner ~10-30 gravitational radii in NGC 3783 where time dependent and recursive modulation have been measured both in the continuum emission and in the broad emission line component. Finally, the accretion disk seems to be only weakly detectable in rk 509, with its weak broad emission line component. Finally, blueshifted resonant absorption lines have been detected in all three objects. This seems to demonstrate that, around super-massive black-holes, there is matter which is not confined in the accretion disk and moves along the line of sight with velocities as large as v~0.01-0.4c (whre c is the speed of light). Wether this matter forms winds or blobs is still matter of debate together with the assessment of the real statistical significance of the measured absorption lines. Nonetheless, if confirmed, these phenomena are of outstanding interest because they offer new potential probes for the dynamics of the innermost regions of accretion flows, to tackle the formation of ejecta/jets and to place constraints on the rate of kinetic energy injected by AGNs into the ISM and IGM. Future high energy missions (such as the planned Simbol-X and IXO) will likely allow an exciting step forward in our understanding of the flow dynamics around black holes and the formation of the highest velocity outflows.

Caratterizzazione sismica di tre siti della rete accelerometrica nazionale (ran) mediante elaborazione di terremoti e rumore ambientale.

Il lavoro di questa tesi ha previsto l'acquisizione e l'elaborazione di dati geofisici al fine di determinare la risposta sismica di tre siti della Rete Accelerometrica Nazionale (RAN), collocandosi all'interno del progetto sismologico S2-2014 Constraining Observations into Seismic Hazard gestito dal Dipartimento di Protezione Civile Nazionale e dall’Istituto Nazionale di Geofisica e di Vulcanologia. Tale necessità nasce dal fatto che il più delle volte le informazioni per la corretta caratterizzazione geofisica dei siti ospitanti le stazioni accelerometriche risultano essere insufficienti, rendendo così i dati acquisiti non idonei per l'utilizzo in sede di calcolo delle leggi di attenuazione dalle quali successivamente vengono derivate le mappe di pericolosità sismica a livello nazionale e locale. L'obbiettivo di questo lavoro di tesi è stato quello di determinare l'eventuale presenza di effetti di sito o effetti di interazione suolo-struttura, per tre stazioni ubicate in Friuli-Venezia Giulia (codici stazioni MAI, TLM1 e BRC), capaci di amplificare il moto del terreno nella parte di suolo compresa fra il bedrock sismico (inteso come strato che non amplifica) e il piano campagna. Le principali tecniche utilizzate sono le seguenti: HVSR ossia rapporto spettrale della componente orizzontale su quella verticale da misure di rumore ambientale acquisite e EHV ovvero rapporto spettrale della componente orizzontale su verticale da registrazione di terremoti scaricate dal database accelerometrico italiano ITACA. I risultati delle due tecniche sono stati poi confrontati al fine di verificare un'eventuale congruenza, portando alle seguenti conclusioni. La caratterizzazione della stazione TLM1 ha portato alla importante conclusione che il sito non è idoneo per l’acquisizione di dati accelerometrici da utilizzare per il calcolo di leggi predittive o di attenuazione. La stazione accelerometrica è ospitata all’interno di un box in lamiera su una collina nel comune di Verzegnis (UD). Il problema principale che riguarda questo sito è la vicinanza della diga Ambiesta e del relativo invaso. La stazione di BRC è collocata all’interno di una cabina di trasformazione dell’ENEL sul lato destro del torrente Cellina, al suo ingresso nel lago di Barcis (PN). Le condizioni topografiche della zona, molto impervie, non consentono la corretta acquisizione dei dati. Un ulteriore fattore di disturbo è dato dall’interazione suolo-struttura, causata dalla cabina ENEL in cui è alloggiata la strumentazione. La caratterizzazione della stazione MAI collocata all'interno di una cabina ENEL nel centro del comune di Majano (UD) ha portato alla conclusione che questa è l'unica delle tre stazioni considerate capace di acquisire dati utilizzabili per il processo di validazione per le stime di pericolosità sismica. Questo perché le condizioni topografiche dell’area, pianura con stratificazione 1D, hanno permesso di sfruttare a pieno le potenzialità delle metodologie utilizzate, consentendo anche la ricostruzione di profili di velocità delle onde di taglio S con i quali è stata assegnata la categoria C del suolo previsto dall'approccio semplificato presente nelle NTC08.