A graphical tool for an analytical approach of scattering photons by the Compton effect

The photons scattered by the Compton effect can be used to characterize the physical properties of a given sample due to the influence that the electron density exerts on the number of scattered photons. However, scattering measurements involve experimental and physical factors that must be carefully analyzed to predict uncertainty in the detection of Compton photons. This paper presents a method for the optimization of the geometrical parameters of an experimental arrangement for Compton scattering analysis, based on its relations with the energy and incident flux of the X-ray photons. In addition, the tool enables the statistical analysis of the information displayed and includes the coefficient of variation (CV) measurement for a comparative evaluation of the physical parameters of the model established for the simulation. (C) 2012 Elsevier B.V. All rights reserved.

Canonical quantum potential scattering theory

A new formulation of potential scattering in quantum mechanics is developed using a close structural analogy between partial waves and the classical dynamics of many non-interacting fields. Using a canonical formalism we find nonlinear first-order differential equations for the low-energy scattering parameters such as scattering length and effective range. They significantly simplify typical calculations, as we illustrate for atom-atom and neutron-nucleus scattering systems. A generalization to charged particle scattering is also possible.

Doubly charged Higgs from e-gamma scattering in the 3-3-1 Model

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Dispersion relations and the spin polarizabilities of the nucleon

A forward dispersion calculation is implemented for the spin polarizabilities γ1, ⋯, γ4 of the proton and the neutron. These polarizabilities are related to the spin structure of the nucleon at low energies and are structure-constants of the Compton scattering amplitude at script O sign(ω3). In the absence of a direct experimental measurement of these quantities, a dispersion calculation serves the purpose of constraining the model building, and of comparing with recent calculations in heavy baryon chiral perturbation theory. © 1998 Elsevier Science B.V.

Scattering Amplitudes Interpolating Between Instant Form and Front Form of Relativistic Dynamics

Among the three forms of relativistic Hamiltonian dynamics proposed by Dirac in 1949, the front form has the largest number of kinematic generators. This distinction provides useful consequences in the analysis of physical observables in hadron physics. Using the method of interpolation between the instant form and the front form, we introduce the interpolating scattering amplitude that links the corresponding time-ordered amplitudes between the two forms of dynamics and provide the physical meaning of the kinematic transformations as they allow the invariance of each individual time-ordered amplitude for an arbitrary interpolation angle. We discuss the rationale for using front form dynamics, nowadays known as light-front dynamics (LFD), and present a few explicit examples of hadron phenomenology that LFD uniquely can offer from first-principles quantum chromodynamics. In particular, model-independent constraints are provided for the analyses of deuteron form factors and the N Delta transition form factors at large momentum transfer squared Q(2). The swap of helicity amplitudes between the collinear and non-collinear kinematics is also discussed in deeply virtual Compton scattering.

Further investigating the determination of phosphorus in plants by INAA using bremsstrahlung measurement

Phosphorus is an essential element for plants and animals, playing a fundamental role in the production of biochemical energy. Despite its relevance, phosphorus is not commonly determined by instrumental neutron activation analysis (INAA), because (32)P does not emit gamma-rays in its decay. There are alternative methods for the determination of phosphorus by INAA, such as the use of beta counting or the measurement of bremsstrahlung originated from the high energy beta particle from (32)P. Here the determination of phosphorus in plant materials by measuring the bremsstrahlung production was further investigated, to optimize an analytical protocol for minimizing interferences and overcoming the poor specificity. Eight certified reference materials of plant matrices with phosphorus ranging between 171 and 5,180 mg kg(-1) were irradiated at a thermal neutron flux of 9.5 x 10(12) cm(-2) s(-1) and measured with a HPGe detector at decay times varying from 7 to 60 days. Phosphorus solutions added to a certified reference material at three levels were used for calibration. Counts accumulated in the baseline at four different regions of the gamma-ray spectra were tested for the determination of phosphorus, with better results for the 100 keV region. The Compton scattering contribution in the selected range was discounted using an experimental peak-to-Compton factor and the net areas of all peaks in the spectra with energies higher than 218 keV, i.e. Compton edge above 100 keV. Amongst the interferences investigated, the production of (32)P from sulfur, and the contribution of Compton scattering should be considered for producing good results.

Strahlungsbegleitete Pion-Photoproduktion am Proton

Im Jahre 1997 wurden von Tatischeff et al. bei der Reaktion p p -> X p pi+ resonanzartige Zustände im Spektrum der invarianten Masse des fehlenden Nukleons X bei M = 1004, 1044 und 1094 MeV gefunden. In einem zweiten Experiment von Filkov et al. beobachtete man bei der Reaktion p d -> p p X Resonanzstrukturen bei M = 966, 986 und 1003 MeV. Solche exotischen Resonanzen widersprechen etablierten Nukleonenmodellen, die die Delta(1232)-Resonanz als ersten Anregungszustand beschreiben. Zur Deutung der beobachteten Strukturen wurden Quarkcluster-Modelle mit und ohne Farb-Magnet-Wechselwirkungen entwickelt. Lvov et al. zweifelten die experimentellen Ergebnisse an, da keine Strukturen in den Daten zur reellen Comptonstreuung gefunden wurden. Als Gegenargument wurde von Kobushkin vorgeschlagen, dass diese Resonanzen eine total-antisymmetrische Spin-Flavour-Wellenfunktion haben und nur der N-2Gamma-Zerfall erlaubt wäre. In dieser Arbeit wurde die Reaktion g p -> X pi+ -> n g g pi+ zur Suche nach diesen exotischen Resonanzen verwendet. Die Daten wurden parallel zur Messung der Pion-Polarisierbarkeiten am Mainzer Beschleuniger MAMI genommen. Durch Bremsstrahlung der Elektronen an einer Radiatorfolie wurden reelle Photonen erzeugt, deren Energie von der A2-Photonenmarkierungsanlage (Glasgow-Tagger) bestimmt wurde. Als Protontarget wurde ein 10 cm langes Flüssigwasserstoff-Target verwendet. Geladene Reaktionsprodukte wurden unter Vorwärtswinkeln Theta < 20 Grad bezüglich der Strahlachse in einer Vieldraht-Proportionalkammer nachgewiesen, während Photonen im Spektrometer TAPS mit 526 BaF2-Kristallen unter Polarwinkeln Theta > 60 Grad detektiert wurden. Zum Nachweis von Neutronen stand ein Flugzeitdetektor mit insgesamt 111 Einzelmodulen zur Verfügung. Zum Test der Analysesoftware und des experimentellen Aufbaus wurden zusätzlich die Reaktionskanäle g p -> p pi0 und g p -> n pi0 pi+ ausgewertet. Für die Ein-Pion-Produktion wurden differentielle Wirkungsquerschnitte unter Rückwärtswinkeln bestimmt und mit theoretischen Modellen und experimentellen Werten verglichen. Für den Kanal g p -> n pi0 pi+ wurden Spektren invarianter Massen für verschiedene Teilchenkombinationen ermittelt und mit einer Simulation verglichen. Die Daten legen nahe, dass die Reaktion hauptsächlich über eine Anregung der Delta0(1232)-Resonanz verläuft. Bei der Suche nach exotischen Resonanzen wurden keine statistisch signifikanten Strukturen gefunden. Es wurden Obergrenzen für den differentiellen Wirkungsquerschnitt ermittelt.

Chirale effektive Feldtheorie mit Vektormesonen : vom elektromagnetischen Formfaktor zur virtuellen Compton-Streuung

Die vorliegende Arbeit beschäftigt sich mit der Modellierung niederenergetischer elektromagnetischer und hadronischer Prozesse im Rahmen einer manifest lorentzinvarianten, chiralen effektiven Feldtheorie unter expliziter, dynamischer Berücksichtigung resonanter, das heißt vektormesonischer Freiheitsgrade. Diese effektive Theorie kann daher als Approximation der grundlegenden Quantenchromodynamik bei kleinen Energien verstanden werden. Besonderes Augenmerk wird dabei auf das verwendete Zähl- sowie Renormierungschema gelegt, wodurch eine konsistente Beschreibung mesonischer Prozesse bis zu Energien von etwa 1GeV ermöglicht wird. Das verwendete Zählschema beruht dabei im Wesentlichen auf einem Argument für großes N_c (Anzahl der Farbfreiheitsgrade) und lässt eine äquivalente Behandlung von Goldstonebosonen (Pionen) und Resonanzen (Rho- und Omegamesonen) zu. Als Renormierungsschema wird das für (bezüglich der starken Wechselwirkung) instabile Teilchen besonders geeignete complex-mass scheme als Erweiterung des extended on-mass-shell scheme verwendet, welches in Kombination mit dem BPHZ-Renormierungsverfahren (benannt nach Bogoliubov, Parasiuk, Hepp und Zimmermann) ein leistungsfähiges Konzept zur Berechnung von Quantenkorrekturen in dieser chiralen effektiven Feldtheorie darstellt. Sämtliche vorgenommenen Rechnungen schließen Terme der chiralen Ordnung vier sowie einfache Schleifen in Feynman-Diagrammen ein. Betrachtet werden unter anderem der Vektorformfaktor des Pions im zeitartigen Bereich, die reelle Compton-Streuung (beziehungsweise Photonenfusion) im neutralen und geladenen Kanal sowie die virtuelle Compton-Streuung, eingebettet in die Elektron-Positron-Annihilation. Zur Extraktion der Niederenergiekopplungskonstanten der Theorie wird letztendlich eine Reihe experimenteller Datensätze verschiedenartiger Observablen verwendet. Die hier entwickelten Methoden und Prozeduren - und insbesondere deren technische Implementierung - sind sehr allgemeiner Natur und können daher auch an weitere Problemstellungen aus diesem Gebiet der niederenergetischen Quantenchromodynamik angepasst werden.

Incorporação do espalhamento Compton no modelo de TBC modificado

No último século, houve grande avanço no entendimento das interações das radiações com a matéria. Essa compreensão se faz necessária para diversas aplicações, entre elas o uso de raios X no diagnóstico por imagens. Neste caso, imagens são formadas pelo contraste resultante da diferença na atenuação dos raios X pelos diferentes tecidos do corpo. Entretanto, algumas das interações dos raios X com a matéria podem levar à redução da qualidade destas imagens, como é o caso dos fenômenos de espalhamento. Muitas abordagens foram propostas para estimar a distribuição espectral de fótons espalhados por uma barreira, ou seja, como no caso de um feixe de campo largo, ao atingir um plano detector, tais como modelos que utilizam métodos de Monte Carlo e modelos que utilizam aproximações analíticas. Supondo-se um espectro de um feixe primário que não interage com nenhum objeto após sua emissão pelo tubo de raios X, este espectro é, essencialmente representado pelos modelos propostos anteriormente. Contudo, considerando-se um feixe largo de radiação X, interagindo com um objeto, a radiação a ser detectada por um espectrômetro, passa a ser composta pelo feixe primário, atenuado pelo material adicionado, e uma fração de radiação espalhada. A soma destas duas contribuições passa a compor o feixe resultante. Esta soma do feixe primário atenuado, com o feixe de radiação espalhada, é o que se mede em um detector real na condição de feixe largo. O modelo proposto neste trabalho visa calcular o espectro de um tubo de raios X, em situação de feixe largo, o mais fidedigno possível ao que se medem em condições reais. Neste trabalho se propõe a discretização do volume de interação em pequenos elementos de volume, nos quais se calcula o espalhamento Compton, fazendo uso de um espectro de fótons gerado pelo Modelo de TBC, a equação de Klein-Nishina e considerações geométricas. Por fim, o espectro de fótons espalhados em cada elemento de volume é somado ao espalhamento dos demais elementos de volume, resultando no espectro total espalhado. O modelo proposto foi implementado em ambiente computacional MATLAB® e comparado com medições experimentais para sua validação. O modelo proposto foi capaz de produzir espectros espalhados em diferentes condições, apresentando boa conformidade com os valores medidos, tanto em termos quantitativos, nas quais a diferença entre kerma no ar calculado e kerma no ar medido é menor que 10%, quanto qualitativos, com fatores de mérito superiores a 90%.

The influence of magnetic field geometry on magnetars X-ray spectra

Nowadays, the analysis of the X-ray spectra of magnetically powered neutron stars or magnetars is one of the most valuable tools to gain insight into the physical processes occurring in their interiors and magnetospheres. In particular, the magnetospheric plasma leaves a strong imprint on the observed X-ray spectrum by means of Compton up-scattering of the thermal radiation coming from the star surface. Motivated by the increased quality of the observational data, much theoretical work has been devoted to develop Monte Carlo (MC) codes that incorporate the effects of resonant Compton scattering (RCS) in the modeling of radiative transfer of photons through the magnetosphere. The two key ingredients in this simulations are the kinetic plasma properties and the magnetic field (MF) configuration. The MF geometry is expected to be complex, but up to now only mathematically simple solutions (self-similar solutions) have been employed. In this work, we discuss the effects of new, more realistic, MF geometries on synthetic spectra. We use new force-free solutions [14] in a previously developed MC code [9] to assess the influence of MF geometry on the emerging spectra. Our main result is that the shape of the final spectrum is mostly sensitive to uncertain parameters of the magnetospheric plasma, but the MF geometry plays an important role on the angle-dependence of the spectra.

Is SGR 0418+5729 indeed a waning magnetar?

SGR 0418+5729 is a transient soft gamma-ray repeater which underwent a major outburst in 2009 June, during which the emission of short bursts was observed. Its properties appeared quite typical of other sources of the same class until long-term X-ray monitoring failed to detect any period derivative. The present upper limit on P implies that the surface dipole field is Bp lsim 7.5 × 1012 G, well below those measured in other soft gamma-ray repeaters (SGRs) and in the Anomalous X-ray Pulsars (AXPs), a group of similar sources. Both SGRs and AXPs are currently believed to be powered by ultra-magnetized neutron stars (magnetars, Bp ≈ 1014-1015 G). SGR 0418+5729 hardly seems to fit in such a picture. We show that the magneto-rotational properties of SGR 0418+5729 can be reproduced if this is an aged magnetar, ≈1 Myr old, which experienced substantial field decay. The large initial toroidal component of the internal field required to match the observed properties of SGR 0418+5729 ensures that crustal fractures, and hence bursting activity, can still occur at the present time. The thermal spectrum observed during the outburst decay is compatible with the predictions of a resonant Compton scattering model (as in other SGRs/AXPs) if the field is low and the magnetospheric twist is moderate.

A study of the scattering of fast neutrons in large samples

In the present work, the elastic scattering of fast neutrons from iron and concrete samples were studied at incident neutron energies of 14.0 and 14.4 Mev, using a neutron spectrometer based on the associated particle time-of-flight technique. These samples were chosen because of their importance in the design of fusion reactor shielding and construction. Using the S.A.M.E.S. accelerator and the 3 M v Dynamitron accelerator at the Radiation Centre, 14.0 and 14.4 Mev neutrons were produced by the T(d, n)4He reaction at incident deuteron energies of 140 keV and 900 keV mass III ions respectively. The time of origin of the neutron was determined by detecting the associated alpha particles. The samples used were extended flat plates of thicknesses up to 1.73 mean free paths for iron and 2.3 mean free paths for concrete. The associated alpha particles and fast neutrons were detected by means of a plastic scintillator mounted on a fast focused photomultiplier tube. The differential neutron elastic scattering cross-sections were measured for 14 Mev neutrons in various thicknesses of iron and concrete in the angular range from zero to 90°. In addition, the angular distributions of 14.4 Mev neutrons after passing through extended samples of iron were measured at several scattering angles in the same angular range. The measurements obtained for the thin sample of iron were compared with the results of Coon et al. The differential cross-sections for the thin iron sample were also analyzed on the optical model using the computer code RAROMP. For the concrete sample, the angular distribution of the thin sample was compared with the cross-sections calculated from the major constituent elements of concrete, and with the predicted values of the optical model for those elements. No published data could be found to compare with the results of the concrete differential cross-sections. In the case of thick samples of iron and concrete, the number of scattered neutrons were compared with a phenomological calculation based on the continuous slowing down model. The variation of measured cross-sections with sample thickness were found to follow the empirical relation σ = σ0 eαx. By using the universal constant "K", good fits were obtained to the experimental data. In parallel with the work at 14.0 and 14.4 Mev, an associated particle time-of-flight spectrometer was investigated which used the 2H(d,n)3He reaction for 3.02 Mev neutron energy at the incident deuteron energy of 1 Mev.

Emissione di Compton inverso e applicazioni astrofisiche

L’emissione di Compton Inverso (IC) rientra nei processi di radiazione detti di diffusione (o di scattering) e riguarda l’interazione tra elettroni relativistici ad alta energia e fotoni molto meno energetici. Il meccanismo di interazione viene approssimato ad un semplice urto tra le due particelle, in seguito al quale il fotone acquista parte dell’energia cinetica dell’elettrone, venendo diffuso ed osservato a frequenza più alta e con direzione di propagazione diversa rispetto a quanto possedeva prima dell’urto. Il Compton Inverso è il meccanismo contrario della diffusione Compton, dove il fotone perde energia in seguito all’urto con l’elettrone e viene osservato a frequenze inferiori a quelle originarie. L’IC viene osservato in ambito astrofisico soprattutto in combinazione con l’emissione di sicrotrone – nella quale elettroni relativistici presenti in regioni magnetizzate vengono accelerati dal campo magnetico ed emettono radiazione – in un fenomeno detto Synchrotron Self-Compton. Esso avviene solitamente in sorgenti molto compatte nelle quali i fotoni prodotti per sincrotrone hanno maggiore possibilità di interagire nuovamente con gli elettroni che li hanno generati, venendo diffusi ad energie più elevate. L’IC viene inoltre osservato in combinazione alla diffusione Compton in un processo detto Comptonizzazione. Ciò si verifica in plasmi molto caldi e abbastanza rarefatti, nei quali si hanno innumerevoli scambi di energia tra le particelle che li compongono. La tesi comprende una prima parte introduttiva nella quale viene presentato il contesto storico di inizio Novecento nel quale si inserisce, tra gli altri, il fisico Arthur H. Compton. Successivamente, vengono spiegati nel dettaglio i principali meccanismi di diffusione con particolare attenzione all’IC. Infine, sono illustrate le applicazioni astrofisiche del Compton Inverso e alcune delle sorgenti nelle quali l’IC viene osservato in combinazione con altri processi di radiazione.

High p(T) direct photon and pi(0) triggered azimuthal jet correlations and measurement of k(T) for isolated direct photons in p plus p collisions at root s=200 GeV

Correlations of charged hadrons of 1< p(T) < 10 Gev/c with high pT direct photons and pi(0) mesons in the range 5< p(T) < 15 Gev/c are used to study jet fragmentation in the gamma + jet and dijet channels, respectively. The magnitude of the partonic transverse momentum, k(T), is obtained by comparing to a model incorporating a Gaussian kT smearing. The sensitivity of the associated charged hadron spectra to the underlying fragmentation function is tested and the data are compared to calculations using recent global fit results. The shape of the direct photon-associated hadron spectrum as well as its charge asymmetry are found to be consistent with a sample dominated by quark-gluon Compton scattering. No significant evidence of fragmentation photon correlated production is observed within experimental uncertainties.

INTEGRAL and XMM-Newton observations towards the unidentified MeV source GRO J1411-64.

The COMPTEL unidentified source GRO J1411-64 was observed by INTEGRAL, and its central part, also by XMM-Newton. The data analysis shows no hint for new detections at hard X-rays. The upper limits in flux herein presented constrain the energy spectrum of whatever was producing GRO J1411-64, imposing, in the framework of earlier COMPTEL observations, the existence of a peak in power output located somewhere between 300-700 keV for the so-called low state. The Circinus Galaxy is the only source detected within the 4$\sigma$ location error of GRO J1411-64, but can be safely excluded as the possible counterpart: the extrapolation of the energy spectrum is well below the one for GRO J1411-64 at MeV energies. 22 significant sources (likelihood $> 10$) were extracted and analyzed from XMM-Newton data. Only one of these sources, XMMU J141255.6-635932, is spectrally compatible with GRO J1411-64 although the fact the soft X-ray observations do not cover the full extent of the COMPTEL source position uncertainty make an association hard to quantify and thus risky. The unique peak of the power output at high energies (hard X-rays and gamma-rays) resembles that found in the SED seen in blazars or microquasars. However, an analysis using a microquasar model consisting on a magnetized conical jet filled with relativistic electrons which radiate through synchrotron and inverse Compton scattering with star, disk, corona and synchrotron photons shows that it is hard to comply with all observational constrains. This and the non-detection at hard X-rays introduce an a-posteriori question mark upon the physical reality of this source, which is discussed in some detail.