Inelastic muon-nucleon interactions will be studied using the nuclear emulsion technique. The momentum of the primary muon beam is 15.8 GeV/C. Muons and other leptons of high energy make excellent probes to study mucleon structure. Muon beams of small contamination, using accelerators, became available in 1965, but the data is limited.In this experiment, we will scan several nuclear emulsion pellicles for muon-nucleon inelastic scatters and study the angular distribution of the scattered muon at 15.8 GeV/C. The results will be compared with previous data and also with the theoretical form factor predictions at this momentum.Ball State UniversityMuncie, IN 47306

ITC/USA 2013 Conference Proceedings / The Forty-Ninth Annual International Telemetering Conference and Technical Exhibition / October 21-24, 2013 / Bally's Hotel & Convention Center, Las Vegas, NV / We address the problem of detection in orbital angular momentum (OAM). The focus of our analysis will be on the power efficient Q-ary Pulse Position Modulation (Q - PPM). Free space optical signals sent through wireless channels are degraded by atmospheric turbulence. In this paper a novel detection approach based on a factor graph representation of OAM Q-PPM signalling is presented to equalize for the crosstalk among orbital angular momentum vortices. It will be shown that our proposed detection algorithm significantly outperforms the separate detection scenario in terms of error rate performance.

In this thesis a kinetic theory for spin-1/2 particles is given a brief overview, focusing on the derivation of an evolution equation for the quasiprobability distribution function used in the theory to describe certain types of quantum plasma. The current theory is expanded upon by exploring conservation laws. A local conservation law for momentum is derived using two different expressions for electromagnetic momentum, given by Abraham and Minkowski respectively. There has been some controversy over which of these expressions should be used; in the case considered here the expression given by Minkowski seems to be more suitable. Based on the conservation law for momentum, a conservation law for angular momentum is also derived.

Magistro darbo autorius: Andrius Samuolis Magistro darbo pavadinimas: Judesio kiekio momento ryšio schemos grafo transformacija Vadovas: doc. dr. A. Deveikis Darbas pristatytas: Vytauto Didžiojo Universitetas, Informatikos fakultetas, Kaunas, 2011 birželis. Puslapių skaičius: 46 Lentelių skaičius: 2 Paveikslų skaičius: 43 Priedų skaičius: 3 Sudaromas supaprastintas judesio kiekio momento grafinis metodas skirtas transformacijos matricų vaizdavimui ir supaprastinimui. Siūlomas metodas apibendrina Vilniaus teorinės fizikos mokyklos sukurto grafinio metodo praktinio taikymo patirtį ir apima tik daţniausiai taikomas jo taisykles. Transformacijos matrica supaprastinama suvedant jos pavidalą į 6j ir 9j koeficientus. Metodo taisyklės yra pakankamai paprastos ir gali būti naudojamos atitinkamų kompiuterinių įrankių kūrimui. / Author of Master Thesis: Andrius Samuolis Full title of Master Thesis: Transformation of the angular momentum coupling graph Supervisor: doc. dr. A. Deveikis Presented at: Vytautas Magnus University, Faculty of Informatics, Kaunas, June 2011. Number of pages: 46 Number of tables: 2 Number of pictures: 43 Number of appendices: 3 Establishes a simplified graphical angular momentum method, which is intended to represent and simplified transformation matrix. Suggest method summarizes graphic method practical experience and includes only the most common form of the rules, which were created by Vilnius school of Theoretical Physics. The transformation matrix is simplified when it’s shape is reduced to 6j and 9j coefficients. Principle rules are simple and can be used in the development of computer tools.

No description available.

Includes bibliographical references (p. 10). / "Physics and Mathematics" -t.p. "TID-4500 (15th Ed.)" -t.p.

En 1972, Skumanich découvre une relation empirique unique entre la période de rotation de surface des étoiles G et leur âge sur la séquence principale. Cette découverte ouvrit alors une nouvelle voie pour la datation stellaire : la gyrochronologie. Dès lors, bon nombre d'auteurs, entre la fin des années 80 et 90, se sont intéressés à l'évolution de la vitesse de rotation de surface des étoiles de faible masse ($M_*$ = 0.4 $M_{odot}$- 1.1 $M_{odot}$). Les premiers modèles phénoménologies sur le sujet été nés.L'évolution de la vitesse de rotation de ces étoiles commence à être raisonnablement bien reproduite par la classe de modèle paramétrique que je présente dans cette thèse. Par manque de descriptions théoriques satisfaisantes, seuls les effets globaux des mécanismes physiques impliqués sont ici décris. Le principal enjeu est d'étudier le cadre et la façon dont le moment cinétique stellaire est impacté par ces processus tout en contraignant leurs principales caractéristiques.Au cours de ma thèse, j'ai modélisé les trajets rotationnels des enveloppes externes et médianes des distributions de période de rotation de 18 amas stellaire entre 1 Myr et 1 Gyr. Ceci m'a permis d'analyser la dépendance temporelle des mécanismes physiques impliqués dans l'évolution du moment cinétique des étoiles de type solaire. Les résultats que j'ai obtenus montrent que l'évolution de la rotation différentielle interne impact fortement la convergence rotationnelle (relation empirique de Skumanich), l'évolution de l'abondance de surface en lithium, et les intensités du champ magnétique généré par effet dynamo. En plus de reproduire ces enveloppes externes, le modèle que j'ai développé fournit des contraintes sur les mécanismes de redistribution interne du moment cinétique et sur les durées de vie des disques circumstellaires, supposés responsables de la régulation rotationnelle observée durant les quelques premiers millions d'années de la pré-séquence principale. L'extension du modèle aux étoiles moins massives (0.5 et 0.8 $M_{odot}$) que j'ai réalisé, a également fournis la dépendance en masse de ces différents processus physiques.Cette étape à notamment ajoutée de fortes contraintes sur les temps caractéristiques associés au transport de moment cinétique entre le coeur et l'enveloppe, sur l'efficacité du freinage magnétique vraisemblablement reliée à un changement de topologie des étoiles de type solaire vers celles de 0.5 $M_{odot}$, et sur l'histoire rotationnelle, interne comme de surface, des étoiles entre 1 Myr à 1 Gyr. / In 1972, Skumanich discovers a unique empirical relationship between the rotation period of the surface of G star and their age on the main sequence. This discovery then opened a new path for stellar dating: the gyrochronology. Therefore, many authors in the late 80's and the begenning 90's, were interested in the evolution of the surface angular velocity of low-mass stars ($M_*$ = 0.4 $M_{odot}$- 1.1 $M_{odot}$). The first phenomenological models on the subject were born.The angular velocity evolution of these stars begins to be reasonably well reproduced by the class of parametrical model that I present in this thesis. Because of the lack of adequate theoretical descriptions, only the overall effects of the physical mechanisms involved are described here. The main issue is to study the framework and how the stellar angular momentum is affected by these processes and to constrain their main characteristics.Over the course of my thesis, I modelled the rotational tracks of external and median envelopes and median of rotation period distributions of 18 stellar clusters between 1 Myr and 1 Gyr. This allowed me to analyse the time dependence of the physical mechanisms involved in the angular momentum evolution of solar-type stars. The results I obtained show that the evolution of the internal differential rotation significantly impact the rotational convergence (empirical Skumanich's relationship), the evolution of the surface lithium abundance, and the intensity of the magnetic field generated by dynamo effect. In addition to the reproduction of these external envelopes, the model I developed provides constraints on the mechanisms of internal redistribution of angular momentum and the lifetimes of circumstellar disks, that are held responsible for the rotational regulation observed during the first few million years of pre-main sequence. The extension of the model to less massive stars (0.5 et 0.8 $M_{odot}$) that I performed also provided the mass dependence of these physical processes. Most specifically, this step added strong constraints on the characteristic time associated to the transport of angular momentum between the core and the envelope, on the efficiency of magnetic braking likely related to a change of topology from solar-type stars to those of 0.5 $M_{odot}$, and on the internal and external rotational history of stars from 1 Myr to 1 Gyr.

abstract: The numerical climate models have provided scientists, policy makers and the general public, crucial information for climate projections since mid-20th century. An international effort to compare and validate the simulations of all major climate models is organized by the Coupled Model Intercomparison Project (CMIP), which has gone through several phases since 1995 with CMIP5 being the state of the art. In parallel, an organized effort to consolidate all observational data in the past century culminates in the creation of several "reanalysis" datasets that are considered the closest representation of the true observation. This study compared the climate variability and trend in the climate model simulations and observations on the timescales ranging from interannual to centennial. The analysis focused on the dynamic climate quantity of zonal-mean zonal wind and global atmospheric angular momentum (AAM), and incorporated multiple datasets from reanalysis and the most recent CMIP3 and CMIP5 archives. For the observation, the validation of AAM by the length-of-day (LOD) and the intercomparison of AAM revealed a good agreement among reanalyses on the interannual and the decadal-to-interdecadal timescales, respectively. But the most significant discrepancies among them are in the long-term mean and long-term trend. For the simulations, the CMIP5 models produced a significantly smaller bias and a narrower ensemble spread of the climatology and trend in the 20th century for AAM compared to CMIP3, while CMIP3 and CMIP5 simulations consistently produced a positive trend for the 20th and 21st century. Both CMIP3 and CMIP5 models produced a wide range of the magnitudes of decadal and interdecadal variability of wind component of AAM (MR) compared to observation. The ensemble means of CMIP3 and CMIP5 are not statistically distinguishable for either the 20th- or 21st-century runs. The in-house atmospheric general circulation model (AGCM) simulations forced by the sea surface temperature (SST) taken from the CMIP5 simulations as lower boundary conditions were carried out. The zonal wind and MR in the CMIP5 simulations are well simulated in the AGCM simulations. This confirmed SST as an important mediator in regulating the global atmospheric changes due to GHG effect. / Dissertation/Thesis / Ph.D. Mechanical Engineering 2013

Objetiva-se discutir e explorar as consequências da conservação do momento angular em situações físicas que apresentem dissipação de energia. Frequentemente, sistemas mecânicos dissipativos são omitidos nas formulações matemáticas da mecânica clássica. No entanto, a conservação da energia mecânica é uma idealização drasticamente incompatível, a longos períodos de tempo, com a maioria das situações reais. Apesar de parecer controversa, esta abordagem é compreensível desde que é incluída na dissipação toda a complexidade dos sistemas mecânicos, os quais não podemos modelar completamente. Espera-se assim que os resultados obtidos sejam parcialmente comprovados em experimentos, sendo que a discrepância é atribuída à parte desconhecida do fenômeno, que muitas vezes é considerada irrelevante para fins práticos. Devido à mencionada complexidade de fenômenos dissipativos, a postura adotada nesta dissertação foi analisar específicos exemplos, de natureza distinta, simplificados, que apresentem as duas propriedades em questão. Concentrou-se especialmente no problema de dissipação de energia em corpos deformáveis na ausência de estímulos externos. / The goal of this work is to study physical systems where angular momentum is a conserved quantity while energy is dissipated. It is a common practice among people working on classical mechanics to neglect energy dissipation. While this hypothesis leads to beautiful mathematical theories, it is strongly violated by the majority of real world systems. The physical complexity of the many ways in which energy is dissipated turns the mathematical modelling of dissipative forces troublesome. There is essentially no general mathematical model for dissipative forces in good agreement with a wide range of experiments. This is in contrast to the very few accepted conservative force models: gravity, elasticity and magneto-electricity. The dissipative force model usually varies among the various physical situations. So, in this work several systems where energy is dissipated while angular momentum is conserved will be considered. The main example will be the motion of a deformable body free from external forces and torques.

Accretion discs efficiently transport angular momentum by a wide variety of as yet imperfectly understood mechanisms, with profound implications for the disc lifetime and planet formation. We discuss two different methods of angular momentum transport: first, generation of acoustic waves by mixing of inertial waves, and second, the generation of a self-sustaining magnetic field via the magnetorotational instability (MRI) which would be a source of dissipative turbulence. Previous local simulations of the MRI have shown that the dynamo changes character on addition of vertical stratification. We investigate numerically 3D hydrodynamic shearing waves with a conserved Hermitian form in an isothermal disc with vertical gravity, and describe the associated symplectic structure. We continue with a numerical investigation into the linear evolution of the MRI and the undular magnetic buoyancy instability in isolated flux regions and characterise the resultant quasi-linear EMFs as a function of height above the midplane. We combine this with an analytic description of the linear modes under an assumption of a poloidal-toroidal scale separation. Finally, we use RAMSES to perform full MHD simulations in a zero net flux shearing box, followed by spatial and a novel temporal averaging to reveal the essential structure of the dynamo. We find that inertial modes may be efficiently converted into acoustic modes for "bending waves", despite a fundamental ambiguity in the inertial mode structure. With our linear MRI and the undular magnetic buoyancy modes we find the localisation of the instability high in the atmosphere becomes determined by magnetic buoyancy rather than field strength for small enough azimuthal wavenumber, and that the critical Alfven speed below which the dynamo can operate increases with increasing distance from the midplane. We calculate analytically quasi-linear EMFs which predict both a vertical propagation of toroidal field and a method for creation of radial field. From our fully nonlinear calculations we find an electromotive force in phase with the toroidal field, which is itself 3π/2 out of phase with the radial (sheared) field at the midplane, and good agreement with our quasi-linear analytics. We have identified an efficient mechanism for generating acoustic waves in a disc. In our investigation of the accretion disc dynamo, we have reproduced analytically the EMFs calculated in our simulations, given arguments based on the phase of relevant quantities, several correlation integrals and the scalings suggested by our analytic work. Our analysis contributes significantly to an explanation for the dynamo in an accretion disc.