Eletrodinâmica quântica generalizada a la teoria de perturbação causal

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Effects of a mixed vector-scalar kink-like potential for spinless particles in two-dimensional space time

The intrinsically relativistic problem of spinless particles subject to a general mixing of vector and scalar kink- like potentials (similar to tanh gamma x) is investigated. The problem is mapped into the exactly solvable Sturm - Liouville problem with the Rosen - Morse potential and exact bounded solutions for particles and antiparticles are found. The behavior of the spectrum is discussed in some detail. An apparent paradox concerning the uncertainty principle is solved by recurring to the concept of effective Compton wavelength.

MHD numerical simulations of colliding winds in massive binary systems - I. Thermal versus non-thermal radio emission

In the past few decades detailed observations of radio and X-ray emission from massive binary systems revealed a whole new physics present in such systems. Both thermal and non-thermal components of this emission indicate that most of the radiation at these bands originates in shocks. O and B-type stars and WolfRayet (WR) stars present supersonic and massive winds that, when colliding, emit largely due to the freefree radiation. The non-thermal radio and X-ray emissions are due to synchrotron and inverse Compton processes, respectively. In this case, magnetic fields are expected to play an important role in the emission distribution. In the past few years the modelling of the freefree and synchrotron emissions from massive binary systems have been based on purely hydrodynamical simulations, and ad hoc assumptions regarding the distribution of magnetic energy and the field geometry. In this work we provide the first full magnetohydrodynamic numerical simulations of windwind collision in massive binary systems. We study the freefree emission characterizing its dependence on the stellar and orbital parameters. We also study self-consistently the evolution of the magnetic field at the shock region, obtaining also the synchrotron energy distribution integrated along different lines of sight. We show that the magnetic field in the shocks is larger than that obtained when the proportionality between B and the plasma density is assumed. Also, we show that the role of the synchrotron emission relative to the total radio emission has been underestimated.

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.

Structure of the N=50 As, Ge, Ga nuclei

The level structures of the N = 50 As-83, Ge-82, and Ga-81 isotones have been investigated by means of multi-nucleon transfer reactions. A first experiment was performed with the CLARA PRISMA setup to identify these nuclei. A second experiment was carried out with the GASP array in order to deduce the gamma-ray coincidence information. The results obtained on the high-spin states of such nuclei are used to test the stability of the N = 50 shell closure in the region of Ni-78 (Z = 28). The comparison of the experimental level schemes with the shell-model calculations yields an N = 50 energy gap value of 4.7(3) MeV at Z = 28. This value, in a good agreement with the prediction of the finite-range liquid-drop model as well as with the recent large-scale shell model calculations, does not support a weakening of the N = 50 shell gap down to Z = 28. (c) 2012 Elsevier B.V. All rights reserved.

Prospect on intergalactic magnetic field measurements with gamma-ray instruments

Observing high-energy gamma-rays from Active Galactic Nuclei (AGN) offers a unique potential to probe extremely tiny values of the intergalactic magnetic field (IGMF), a long standing question of astrophysics, astropa rticle physics and cosmology. Very high energy (VHE) photons from blazars propagating along the line of sight interact with the extragalactic background light (EBL) and produce e + e − pairs. Through inverse-Compton interaction, mainly on the cosmic microwave background (CMB), these pairs generate secondary GeV-TeV compo- nents accompanying the primary VHE signal. Such secondary components would be detected in the gamma-ray range as delayed “pair echos” for very weak IGMF ( B< 10 − 16 G ), while they should result in a spatially extended ga mma-ray emission around the source for higher IGMF values ( B> 10 − 16 G ). Coordinated observations with space (i.e. Fermi) and ground- based gamma-ray instruments, such as the pre sent Cherenkov experiments H.E.S.S., MAGIC and VERITAS, the future Cherenkov Telescope Array (CTA) Observatory, and the wide-field detectors such as HAWC and LHAASO, should allow to analyze and finally detect such echos, extended emission or pair halos, and to further characterize the IGMF.

Statistical properties of Radio Halos and the re-acceleration model

Galaxy clusters occupy a special position in the cosmic hierarchy as they are the largest bound structures in the Universe. There is now general agreement on a hierarchical picture for the formation of cosmic structures, in which galaxy clusters are supposed to form by accretion of matter and merging between smaller units. During merger events, shocks are driven by the gravity of the dark matter in the diffuse barionic component, which is heated up to the observed temperature. Radio and hard-X ray observations have discovered non-thermal components mixed with the thermal Intra Cluster Medium (ICM) and this is of great importance as it calls for a “revision” of the physics of the ICM. The bulk of present information comes from the radio observations which discovered an increasing number of Mpcsized emissions from the ICM, Radio Halos (at the cluster center) and Radio Relics (at the cluster periphery). These sources are due to synchrotron emission from ultra relativistic electrons diffusing through µG turbulent magnetic fields. Radio Halos are the most spectacular evidence of non-thermal components in the ICM and understanding the origin and evolution of these sources represents one of the most challenging goal of the theory of the ICM. Cluster mergers are the most energetic events in the Universe and a fraction of the energy dissipated during these mergers could be channelled into the amplification of the magnetic fields and into the acceleration of high energy particles via shocks and turbulence driven by these mergers. Present observations of Radio Halos (and possibly of hard X-rays) can be best interpreted in terms of the reacceleration scenario in which MHD turbulence injected during these cluster mergers re-accelerates high energy particles in the ICM. The physics involved in this scenario is very complex and model details are difficult to test, however this model clearly predicts some simple properties of Radio Halos (and resulting IC emission in the hard X-ray band) which are almost independent of the details of the adopted physics. In particular in the re-acceleration scenario MHD turbulence is injected and dissipated during cluster mergers and thus Radio Halos (and also the resulting hard X-ray IC emission) should be transient phenomena (with a typical lifetime <» 1 Gyr) associated with dynamically disturbed clusters. The physics of the re-acceleration scenario should produce an unavoidable cut-off in the spectrum of the re-accelerated electrons, which is due to the balance between turbulent acceleration and radiative losses. The energy at which this cut-off occurs, and thus the maximum frequency at which synchrotron radiation is produced, depends essentially on the efficiency of the acceleration mechanism so that observations at high frequencies are expected to catch only the most efficient phenomena while, in principle, low frequency radio surveys may found these phenomena much common in the Universe. These basic properties should leave an important imprint in the statistical properties of Radio Halos (and of non-thermal phenomena in general) which, however, have not been addressed yet by present modellings. The main focus of this PhD thesis is to calculate, for the first time, the expected statistics of Radio Halos in the context of the re-acceleration scenario. In particular, we shall address the following main questions: • Is it possible to model “self-consistently” the evolution of these sources together with that of the parent clusters? • How the occurrence of Radio Halos is expected to change with cluster mass and to evolve with redshift? How the efficiency to catch Radio Halos in galaxy clusters changes with the observing radio frequency? • How many Radio Halos are expected to form in the Universe? At which redshift is expected the bulk of these sources? • Is it possible to reproduce in the re-acceleration scenario the observed occurrence and number of Radio Halos in the Universe and the observed correlations between thermal and non-thermal properties of galaxy clusters? • Is it possible to constrain the magnetic field intensity and profile in galaxy clusters and the energetic of turbulence in the ICM from the comparison between model expectations and observations? Several astrophysical ingredients are necessary to model the evolution and statistical properties of Radio Halos in the context of re-acceleration model and to address the points given above. For these reason we deserve some space in this PhD thesis to review the important aspects of the physics of the ICM which are of interest to catch our goals. In Chapt. 1 we discuss the physics of galaxy clusters, and in particular, the clusters formation process; in Chapt. 2 we review the main observational properties of non-thermal components in the ICM; and in Chapt. 3 we focus on the physics of magnetic field and of particle acceleration in galaxy clusters. As a relevant application, the theory of Alfv´enic particle acceleration is applied in Chapt. 4 where we report the most important results from calculations we have done in the framework of the re-acceleration scenario. In this Chapter we show that a fraction of the energy of fluid turbulence driven in the ICM by the cluster mergers can be channelled into the injection of Alfv´en waves at small scales and that these waves can efficiently re-accelerate particles and trigger Radio Halos and hard X-ray emission. The main part of this PhD work, the calculation of the statistical properties of Radio Halos and non-thermal phenomena as expected in the context of the re-acceleration model and their comparison with observations, is presented in Chapts.5, 6, 7 and 8. In Chapt.5 we present a first approach to semi-analytical calculations of statistical properties of giant Radio Halos. The main goal of this Chapter is to model cluster formation, the injection of turbulence in the ICM and the resulting particle acceleration process. We adopt the semi–analytic extended Press & Schechter (PS) theory to follow the formation of a large synthetic population of galaxy clusters and assume that during a merger a fraction of the PdV work done by the infalling subclusters in passing through the most massive one is injected in the form of magnetosonic waves. Then the processes of stochastic acceleration of the relativistic electrons by these waves and the properties of the ensuing synchrotron (Radio Halos) and inverse Compton (IC, hard X-ray) emission of merging clusters are computed under the assumption of a constant rms average magnetic field strength in emitting volume. The main finding of these calculations is that giant Radio Halos are naturally expected only in the more massive clusters, and that the expected fraction of clusters with Radio Halos is consistent with the observed one. In Chapt. 6 we extend the previous calculations by including a scaling of the magnetic field strength with cluster mass. The inclusion of this scaling allows us to derive the expected correlations between the synchrotron radio power of Radio Halos and the X-ray properties (T, LX) and mass of the hosting clusters. For the first time, we show that these correlations, calculated in the context of the re-acceleration model, are consistent with the observed ones for typical µG strengths of the average B intensity in massive clusters. The calculations presented in this Chapter allow us to derive the evolution of the probability to form Radio Halos as a function of the cluster mass and redshift. The most relevant finding presented in this Chapter is that the luminosity functions of giant Radio Halos at 1.4 GHz are expected to peak around a radio power » 1024 W/Hz and to flatten (or cut-off) at lower radio powers because of the decrease of the electron re-acceleration efficiency in smaller galaxy clusters. In Chapt. 6 we also derive the expected number counts of Radio Halos and compare them with available observations: we claim that » 100 Radio Halos in the Universe can be observed at 1.4 GHz with deep surveys, while more than 1000 Radio Halos are expected to be discovered in the next future by LOFAR at 150 MHz. This is the first (and so far unique) model expectation for the number counts of Radio Halos at lower frequency and allows to design future radio surveys. Based on the results of Chapt. 6, in Chapt.7 we present a work in progress on a “revision” of the occurrence of Radio Halos. We combine past results from the NVSS radio survey (z » 0.05 − 0.2) with our ongoing GMRT Radio Halos Pointed Observations of 50 X-ray luminous galaxy clusters (at z » 0.2−0.4) and discuss the possibility to test our model expectations with the number counts of Radio Halos at z » 0.05 − 0.4. The most relevant limitation in the calculations presented in Chapt. 5 and 6 is the assumption of an “averaged” size of Radio Halos independently of their radio luminosity and of the mass of the parent clusters. This assumption cannot be released in the context of the PS formalism used to describe the formation process of clusters, while a more detailed analysis of the physics of cluster mergers and of the injection process of turbulence in the ICM would require an approach based on numerical (possible MHD) simulations of a very large volume of the Universe which is however well beyond the aim of this PhD thesis. On the other hand, in Chapt.8 we report our discovery of novel correlations between the size (RH) of Radio Halos and their radio power and between RH and the cluster mass within the Radio Halo region, MH. In particular this last “geometrical” MH − RH correlation allows us to “observationally” overcome the limitation of the “average” size of Radio Halos. Thus in this Chapter, by making use of this “geometrical” correlation and of a simplified form of the re-acceleration model based on the results of Chapt. 5 and 6 we are able to discuss expected correlations between the synchrotron power and the thermal cluster quantities relative to the radio emitting region. This is a new powerful tool of investigation and we show that all the observed correlations (PR − RH, PR − MH, PR − T, PR − LX, . . . ) now become well understood in the context of the re-acceleration model. In addition, we find that observationally the size of Radio Halos scales non-linearly with the virial radius of the parent cluster, and this immediately means that the fraction of the cluster volume which is radio emitting increases with cluster mass and thus that the non-thermal component in clusters is not self-similar.

Metrologia dei campi di radiazioni di bassa energia

The conversion coefficients from air kerma to ICRU operational dose equivalent quantities for ENEA’s realization of the X-radiation qualities L10-L35 of the ISO “Low Air Kerma rate” series (L), N10-N40 of the ISO “Narrow spectrum” series (N) and H10-H60 of the ISO “High Air-kerma rate” (H) series and two beams at 5 kV and 7.5 kV were determined by utilising X-ray spectrum measurements. The pulse-height spectra were measured using a planar high-purity germanium spectrometer (HPGe) and unfolded to fluence spectra using a stripping procedure then validate with using Monte Carlo generated data of the spectrometer response. HPGe portable detector has a diameter of 8.5 mm and a thickness of 5 mm. The entrance window of the crystal is collimated by a 0.5 mm thick Aluminum ring to an open diameter of 6.5 mm. The crystal is mounted at a distance of 5 mm from the Berillium window (thickness 25.4 micron). The Monte Carlo method (MCNP-4C) was used to calculate the efficiency, escape and Compton curves of a planar high-purity germanium detector (HPGe) in the 5-60 keV energy. These curves were used for the determination of photon spectra produced by the X-ray machine SEIFERT ISOVOLT 160 kV in order to allow a precise characterization of photon beams in the low energy range, according to the ISO 4037. The detector was modelled with the MCNP computer code and validated with experimental data. To verify the measuring and the stripping procedure, the first and the second half-value layers and the air kerma rate were calculated from the counts spectra and compared with the values measured using an a free-air ionization chamber. For each radiation quality, the spectrum was characterized by the parameters given in ISO 4037-1. The conversion coefficients from the air kerma to the ICRU operational quantities Hp(10), Hp(0.07), H’(0.07) and H*(10) were calculated using monoenergetic conversion coefficients. The results are discussed with respect to ISO 4037-4, and compared with published results for low-energy X-ray spectra. The main motivation for this work was the lack of a treatment of the low photon energy region (from a few keV up to about 60 keV).

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.

Präparation eines reinen metastabilen 7 Li +-Ionenstrahls für die Präzisionsspektroskopie im Speicherring

An dem Schwerionenspeicherring TSR (MPI für Kernphysik, Heidelberg) wurde ein 7 Li +-Ionenstrahl geringer Dichte durch RF-Bunchen und Laserkühlung präpariert.Die Phasenraumverteilung in dem Strahl wurde durch Laser- spektroskopie an Ionen im metastabilen Zustand untersucht. Ein umlaufsynchrones, zeitaufgelöstes Meßverfahren für das Fluoreszenzlicht ermöglichte die Bestimmung der räumlichen Struktur mit dieser rein optischen Methode.Durch einen speziellen Präparationsschritt wurden die Ionen im Grundzustand aus dem Speicherring entfernt. Der sonst dominierende Heizeffekt der strahlinternen Streuung war dadurch vernachlässigbar und es konnte eine Temperatur von 160 mK erreicht werden.Der präparierte Ionenstrahl bietet besondere Eigenschaften im Hinblick auf Präzisionsexperimente, bei denen mit möglichst ungestörten Ionen gearbeitet werden soll. Es wird gezeigt, daß die Phasenraumverteilung der Ionen nicht mehr durch Ion-Ion-Wechselwirkungen bestimmt ist und daß der verbleibende Heizmechanismus durch die Streuung am Restgas erklärt werden kann.1993 wurde durch Laserspektroskopie an 7 Li + im TSR die spezielle Relativitätstheorie im Hinblick auf die relativistische Zeitdilatation experimentell getestet. In diesem Zusammenhang wird das zu erwartende Ergebnis eines Experimentes diskutiert, das, basierend auf den in dieser Arbeit vorgestellten Verfahren, einen erneuten Test der relativistischen Zeitdilatation mit verbesserter Genauigkeit durchführen könnte.

Strukturbildung in dünnen Filmen aus Mischungen statistischer Copolymere

Dünne Polymerfilme besitzen einen weiten Anwendungsbereich in vielen High-Tech Applikationen. All diese Anwendungen erfordern ein bestimmtes Anwendungsprofil des dünnen Films. Diese Anforderungen umschließen sowohl die physikalischen Eigenschaften des Films als auch seine Struktur. Um sie zu realisieren, werden oftmals Mischungsfilme aus verschiedenen Polymeren verwendet. Diese neigen jedoch in vielen Fällen zur bereits während der Präparation zu Phasenseparation.Vor diesem Hintergrund wurde untersucht welchen Einfluss die Verträglichkeit der gemischten Polymere auf die Strukturbildung des dünnen Films ausüben. Als Modellsystem hierfür dienten Mischungen statistischer Poly-styrol-stat-para brom-styrol Copolymere.Die Oberflächenstrukturen, die sich währen der Präparation der Mischungsfilme einstellten, wurden mit Rasterkraftmikroskopie untersucht. wobei die Topologie einer statistischen Analyse unterzogen wurde. Zum einen wurde hierzu die spektrale Leistungsdichte der Oberflächenkontour zum anderen die zugehörigen Minkowski-Funktionale berechnet.Neben Oberflächenstrukturen bilden sich während der Präparation auch Entmischungsstrukturen im inneren des Filmes. Zur Charakterisierung dieser Strukturen wurden die Filme durch Streuung unter streifendem Einfall untersucht. Durch eine modellfreie Interpretation der Streuexperimente gelang der Nachweis der inneren StrukturenFür nur schwach unverträglich Filme konnte auf Basis der Streuexperimente eine Replikation der Oberflächenstruktur des Substrates auf die Filmoberflächen nachgewiesen werden. Diese Replikation wurde für verschieden raue Substrate und bezueglich der Kinetik ihrer Abnahme beim Quellen der Filme untersucht.

Untersuchung der Ordnung und Diffusion von Polymerdispersionen bei ihrer Verfilmung

Im Rahmen dieser Arbeit wurde die, für industrielle Applikationen sehr wichtige, Trocknung und Verfilmung von Latexdispersionen untersucht. Unter der Verfilmung wird in diesem Zusammenhang allgemein der Übergang einer Polymerdispersion in einen transparenten, mechanisch stabilen Polymerfilm während ihrer Trocknung verstanden. Für die Untersuchungen wurden schwerpunktmäßig Streumethoden verwendet. Die Untersuchungen haben gezeigt, daß die Streuung eine besonders geeignete Methode zur Untersuchung der Verfilmung ist, die in Abhängigkeit des beobachteten Streuvektorbereichs, der verwendeten Strahlung, der Probenpräparation und des resultierenden Kontrasts eine Vielzahl unterschiedlicher Informationen über die Verfilmung in ihren verschiedenen Phasen liefert. Von besonderem Interesse war es, den prinzipiellen Verlauf der Verfilmung bei den heterogen trocknenden Reinacrylatlatices zu untersuchen. Dazu wurde mit Hilfe der Röntgenultrakleinwinkelstreuung gezielt der Zustand der Partikel in den einzelnen Phasen der heterogen trocknenden Proben beobachtet. Mit Hilfe der Neutronenkleinwinkelstreuung konnte das Verhalten des Emulgators während der Verfilmung und dessen Verteilung im resultierenden Film genauer untersucht werden. Die Röntgenkleinwinkelstreuung erlaubte eine eingehende Untersuchung der Kristallisation des Emulgators im trockenen Film. Geeignete Kontrastierung durch gezielte Deuterierung ermöglichte die Untersuchung des Comonomereinflusses auf die Interdiffusion von Latexpartikeln mit Neutronenkleinwinkelstreuung. Aus den Meßergebnissen wurde ein Modell zur heterogenen Trocknung von Latexdispersionen entwickelt, das den Ablauf der Verfilmung in einem konsistenten Bild zusammenfaßt.

Dynamik unterkühlter molekularer Flüssigkeiten in Modenkopplungsapproximation - die Rolle der Orientierungsfreiheitsgrade für den Bosonenpeak

Die von Schilling et al. 1997 aufgestellten molekularenModenkopplungsgleichungen sind für zwei Systeme, dipolareharte Kugeln undharte Rotationsellipsoide, numerisch gelöst worden.In den Kompressibilitätsspektrenund den entsprechenden Korrelationsspektren der beidenSysteme fiel im Vergleich mit den Spektren einfacherFlüssigkeiten einzusätzlicher Peak (bp) auf.Die Position des zusätzlichen Peaks ist etwa eine Dekade unterhalb der Position derHochfrequenzpeaks, also im mesoskopischen Frequenzbereich.In molekularen Flüssigkeiten sind Phasenübergänge derOrientierung derglqq Molekülegrqq möglich.Bei dipolaren harten Kugeln kann ferroelektrische Ordnung,bei hartenEllipsoiden nematische Ordnung auftreten. Als Vorläuferphänomen der Orientierungsordnung bilden sich in den molekularenFlüssigkeiten orientierungsgeordnete Domänen. Die Kurzzeitdynamik dieser Domänen findetauf mesoskopischer Zeitskala statt. In der unterkühlten Flüssigkeit ist die Dynamik aller Modenan die Dynamikdieser Orientierungsmoden gekoppelt. Unsere Untersuchungen zeigen starke Hinweise darauf, dassdiese Kopplung denbp erzeugt.Demnach ist die Streuung nichtlokalisierter longitudinalerakustischer Modenan lokalisierten Orientierungsmoden die Ursache für den bp.hat nahezu keine q-Abhängigkeit und zeigt einenIsotopeneffekt. Weiterhin verglichen wir die Eigenschaften des bp mit denEigenschaften des Bosonenpeaks (BP).Der BP befindet sich in Spektren realer Systeme ebenfallseine Dekadeunterhalb der Hochfrequenzpeaks.Dieser Vergleich und der Vergleich mit den Ergebnissen einerMD-Simulation desHE-Systems ließ uns vermuten, dass es sich bei dem bp und bei dem BP in Spektrenmolekularer Systeme um dasselbe Phänomen handelt.In einem schematischen Modenkopplungsmodell konnte dasVerhalten des bpzusätzlich untersucht werden.

Aufbau eines Moeller-Polarimeters für die Drei-Spektrometer-Anlage und Messung der Helizitätsasymmetrie in der Reaktion p(vec{e},e' p)pi 0 im Bereich der Delta-Resonanz

An der Drei-Spektrometer-Anlage am Beschleuniger MAMI wurde ein Elektronpolarimeter aufgebaut, das die longitudinale Spinpolarisation für Strahlenergien von 500-880 MeV bestimmt. Messprinzip ist die Møller-Streuung. Weiterhin wird ein Experiment zur Bestimmung der Strahlhelizitäts-Asymmetrie in resonanter Elektroproduktion neutraler Pionen am Proton vorgestellt. Diese Observable bietet Zugang zu nichtresonanten Untergrundamplituden in der Nukleon-Delta-Anregung, die im Hinblick auf die Extraktion der Quadrupolamplituden in diesem Übergang wichtig sind.

Messung der Polarisierbarkeiten des Pions am MAMI

Die elektromagnetischen Polarisierbarkeiten sindfundamentale Strukturkonstanten des Pions, wie die Masse unddie Ladung, und ihre genaue Messung erlaubt, theoretischeModelle zu ueberpruefen, da sie grosse Diskrepanzen in ihrenVorhersagen zeigen. Ein Pilot-Experiment zur Messung dieser Konstanten mit Hilfeder strahlungsbegleiteten Pion-Photoproduktion in der Photon-Nukleon Streuung photon + proton --> photon + pion+ + neutron wurde durchgefuehrt. Es wurde gezeigt, dass diese Reaktioneffizient von Untergrundprozessen getrennt werden kann, undein Auswerteverfahren fuer das endgueltige Experiment wurdevorbereitet. Das Experiment wurde am MAMI-Beschleuniger mitmarkierten Photonen im Energiebereich zwischen 525 und 792MeV durchgefuehrt. In diesem Intervall ist dieEmpfindlichkeit auf die Polarisierbarkeiten am groesstenDie gestreuten Pionen wurden mit Hilfe einer Vieldrahtkammernachgewiesen, waehrend die Photonen- und Neutronenimpulse imTAPS Photon-Spektrometer bzw. in einem Flugzeit-Detektorgemessen wurden. Mit 985 Ereignissen in etwa 200 Strahlstunden wurden dieZiele dieses Pilot-Experiments erfuellt. Ausserdem wurdegezeigt, dass das endgueltige Experiment den im TechnicalProposal vorgesehenen statistischen Fehler erreichen wird.Vorlaeufige differentielle Wirkungsquerschnitte wurden miteinem Model von L. Fil'kov verglichen.