Synthesis, characterization, optical absorption, luminescence and defect centres in Er3+ and Yb3+ co-doped MgAl2O4 phosphors

The Er3+-Yb3+ co-doped MgAl2O4 phosphor powders have been prepared by the combustion method. The phosphor powders are well characterized by X-ray diffraction (XRD) and energy dispersive (EDX) techniques. The absorption spectrum of Er3+/Er3+-Yb3+ doped/co-doped phosphor powder has been recorded in the UV-Vis-NIR region of the electro-magnetic spectrum. The evidence for indirect pumping under 980 nm excitation of Er3+ from Yb3+ was observed in the MgAl2O4 matrix material. Electron spin resonance (ESR) studies were carried out to identify the defect centres responsible for the thermally stimulated luminescence (TSL) process in MgAl2O4:Er3+ phosphor. Three defect centres were identified in irradiated phosphor by ESR measurements which were carried out at room temperature and these were assigned to an O- ion and F+ centres. O- ion (hole centre) appears to correlate with the low temperature TSL peak at 210 A degrees C and one of the F+ centres (electron centre) is related to the high temperature peak at 460 A degrees C.

The relationship between gamma Cassiopeiae's X-ray emission and its circumstellar environment

gamma Cas is the prototypical classical Be star and is recently best known for its variable hard X-ray emission. To elucidate the reasons for this emission, we mounted a multiwavelength campaign in 2010 centered around four XMM-Newton observations. The observational techniques included long baseline optical interferometry (LBOI) from two instruments at CHARA, photometry carried out by an automated photometric telescope and H alpha observations. Because gamma Cas is also known to be in a binary, we measured radial velocities from the H alpha line and redetermined its period as 203.55 +/- 0.20 days and its eccentricity as near zero. The LBOI observations suggest that the star's decretion disk was axisymmetric in 2010, has an system inclination angle near 45 degrees, and a larger radius than previously reported. In addition, the Be star began an "outburst" at the beginning of our campaign, made visible by a brightening and reddening of the disk during our campaign and beyond. Our analyses of the new high resolution spectra disclosed many attributes also found from spectra obtained in 2001 (Chandra) and 2004 (XMM-Newton). As well as a dominant hot (approximate to 14 keV) thermal component, the familiar attributes included: (i) a fluorescent feature of Fe K even stronger than observed at previous times; (ii) strong lines of N VII and Ne XI lines indicative of overabundances; and (iii) a subsolar Fe abundance from K-shell lines but a solar abundance from L-shell ions. We also found that two absorption columns are required to fit the continuum. While the first one maintained its historical average of 1 x 10(21) cm(-2), the second was very large and doubled to 7.4 x 10(23) cm(-2) during our X-ray observations. Although we found no clear relation between this column density and orbital phase, it correlates well with the disk brightening and reddening both in the 2010 and earlier observations. Thus, the inference from this study is that much (perhaps all?) of the X-ray emission from this source originates behind matter ejected by gamma Cas into our line of sight.

Beyond the diffraction limit of optical/IR interferometers I. Angular diameter and rotation parameters of Achernar from differential phases

Context. Spectrally resolved long-baseline optical/IR interferometry of rotating stars opens perspectives to investigate their fundamental parameters and the physical mechanisms that govern their interior, photosphere, and circumstellar envelope structures. Aims. Based on the signatures of stellar rotation on observed interferometric wavelength-differential phases, we aim to measure angular diameters, rotation velocities, and orientation of stellar rotation axes. Methods. We used the AMBER focal instrument at ESO-VLTI in its high-spectral resolution mode to record interferometric data on the fast rotator Achernar. Differential phases centered on the hydrogen Br gamma line (K band) were obtained during four almost consecutive nights with a continuous Earth-rotation synthesis during similar to 5h/night, corresponding to similar to 60 degrees position angle coverage per baseline. These observations were interpreted with our numerical code dedicated to long-baseline interferometry of rotating stars. Results. By fitting our model to Achernar's differential phases from AMBER, we could measure its equatorial radius R-eq = 11.6 +/- 0.3 R-circle dot, equatorial rotation velocity V-eq = 298 +/- 9 km s(-1), rotation axis inclination angle i = 101.5 +/- 5.2 degrees, and rotation axis position angle (from North to East) PA(rot) = 34.9 +/- 1.6 degrees. From these parameters and the stellar distance, the equatorial angular diameter circle divide(eq) of Achernar is found to be 2.45 +/- 0.09 mas, which is compatible with previous values derived from the commonly used visibility amplitude. In particular, circle divide(eq) and PA(rot) measured in this work with VLTI/AMBER are compatible with the values previously obtained with VLTI/VINCI. Conclusions. The present paper, based on real data, demonstrates the super-resolution potential of differential interferometry for measuring sizes, rotation velocities, and orientation of rotating stars in cases where visibility amplitudes are unavailable and/or when the star is partially or poorly resolved. In particular, we showed that differential phases allow the measurement of sizes up to similar to 4 times smaller than the diffraction-limited angular resolution of the interferometer.

Quantification of Short and Medium Range Order in Mixed Network Former Glasses of the System GeO2-NaPO3: A Combined NMR and X-ray Photoelectron Spectroscopy Study

Glasses in the system xGeO(2)-(1-x)NaPO3 (0 <= x <= 0.50) were prepared by conventional melting quenching and characterized by thermal analysis, Raman spectroscopy, X-ray photoelectron spectroscopy (XPS), and P-31 nuclear magnetic resonance (MAS NMR) techniques. The deconvolution of the latter spectra was aided by homonuclear J-resolved and refocused INADEQUATE techniques. The combined analyses of P-31 MAS NMR and O-1s XPS lineshapes, taking charge and mass balance considerations into account, yield the detailed quantitative speciations of the phosphorus, germanium, and oxygen atoms and their respective connectivities. An internally consistent description is possible without invoking the formation of higher-coordinated germanium species in these glasses, in agreement with experimental evidence in the literature. The structure can be regarded, to a first approximation, as a network consisting of P-(2) and P-(3) tetrahedra linked via four-coordinate germanium. As implied by the appearance of P-(3) units, there is a moderate extent of network modifier sharing between phosphate and germanate network formers, as expressed by the formal melt reaction P-(2) + Ge-(4) -> P-(3) + Ge-(3). The equilibrium constant of this reaction is estimated as K = 0.52 +/- 0.11, indicating a preferential attraction of network modifier by the phosphorus component. These conclusions are qualitatively supported by Raman spectroscopy as well as P-31{Na-23} and P-31{Na-23} rotational echo double resonance (REDOR) NMR results. The combined interpretation of O-1s XPS and P-31 MAS NMR spectra shows further that there are clear deviations from a random connectivity scenario: heteroatomic P-O-Ge linkages are favored over homoatomic P-O-P and Ge-O-Ge linkages.

Enhancement of optical absorption by modulation of the oxygen flow of TiO2 films deposited by reactive sputtering

Oxygen-deficient TiO2 films with enhanced visible and near-infrared optical absorption have been deposited by reactive sputtering using a planar diode radio frequency magnetron configuration. It is observed that the increase in the absorption coefficient is more effective when the O-2 gas supply is periodically interrupted rather than by a decrease of the partial O-2 gas pressure in the deposition plasma. The optical absorption coefficient at 1.5 eV increases from about 1 x 10(2) cm(-1) to more than 4 x 10(3) cm(-1) as a result of the gas flow discontinuity. A red-shift of similar to 0.24 eV in the optical absorption edge is also observed. High resolution transmission electron microscopy with composition analysis shows that the films present a dense columnar morphology, with estimated mean column width of 40nm. Moreover, the interruptions of the O-2 gas flow do not produce detectable variations in the film composition along its growing direction. X-ray diffraction and micro-Raman experiments indicate the presence of the TiO2 anatase, rutile, and brookite phases. The anatase phase is dominant, with a slight increment of the rutile and brookite phases in films deposited under discontinued O-2 gas flow. The increase of optical absorption in the visible and near-infrared regions has been attributed to a high density of defects in the TiO2 films, which is consistent with density functional theory calculations that place oxygen-related vacancy states in the upper third of the optical bandgap. The electronic structure calculation results, along with the adopted deposition method and experimental data, have been used to propose a mechanism to explain the formation of the observed oxygen-related defects in TiO2 thin films. The observed increase in sub-bandgap absorption and the modeling of the corresponding changes in the electronic structure are potentially useful concerning the optimization of efficiency of the photocatalytic activity and the magnetic doping of TiO2 films. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4724334]

SnO2 nanocrystals synthesized by microwave-assisted hydrothermal method: towards a relationship between structural and optical properties

The exploration of novel synthetic methodologies that control both size and shape of functional nanostructure opens new avenues for the functional application of nanomaterials. Here, we report a new and versatile approach to synthesize SnO2 nanocrystals (rutile-type structure) using microwave-assisted hydrothermal method. Broad peaks in the X-ray diffraction spectra indicate the nanosized nature of the samples which were indexed as a pure cassiterite tetragonal phase. Chemically and physically adsorbed water was estimated by TGA data and FT-Raman spectra to account for a new broad peak around 560 cm(-1) which is related to defective surface modes. In addition, the spherical-like morphology and low dispersed distribution size around 3-5 nm were investigated by HR-TEM and FE-SEM microscopies. Room temperature PL emission presents two broad bands at 438 and 764 nm, indicating the existence of different recombination centers. When the size of the nanospheres decreases, the relative intensity of 513 nm emission increases and the 393 nm one decreases. UV-Visible spectra show substantial changes in the optical absorbance of crystalline SnO2 nanoparticles while the existence of a small tail points out the presence of localized levels inside the forbidden band gap and supplies the necessary condition for the PL emission.

Annealing effects on nanostructured gold-polymethylmethacrylate composites: Small-angle x-ray scattering analysis

Composites formed of a polymer-embedded layer of sub-10 nm gold nanoclusters were fabricated by very low energy (49 eV) gold ion implantation into polymethylmethacrylate. We used small angle x-ray scattering to investigate the structural properties of these metal-polymer composite layers that were fabricated at three different ion doses, both in their original form (as-implanted) and after annealing for 6 h well above the polymer glass transition temperature (150 degrees C). We show that annealing provides a simple means for modification of the structure of the composite by coarsening mechanisms, and thereby changes its properties. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4720464]

Influence of nanoparticle size on the nonlinear optical properties of magnetite ferrofluids

The nonlinear index of refraction (n(2)) and the two-photon absorption coefficient (beta) of water-based ferrofluids made of magnetite nanocrystals of different sizes and with different coatings have been measured through the Z-scan technique, with ultrashort (femtoseconds) laser pulses. Their third-order susceptibility is calculated from the values of n(2) and beta. The influence of different particles' coatings and sizes on these nonlinear optical properties are investigated. The values of n(2) and beta depend more significantly on the nanoparticles' size than on the particular coating. We observe a decrease of beta as the nanoparticles' diameters decrease, although the optical gap is found to be the same for all samples. The results are interpreted considering modifications in the electronic orbital shape due to the particles' nanosize effect.

Experimental Investigation of Three-Dimensional Single and Double optical Lattices

A complete laser cooling setup was built, with focus on threedimensional near-resonant optical lattices for cesium. These consist of regularly ordered micropotentials, created by the interference of four laser beams. One key feature of optical lattices is an inherent ”Sisyphus cooling” process. It efficiently extracts kinetic energy from the atoms, leading to equilibrium temperatures of a few µK. The corresponding kinetic energy is lower than the depth of the potential wells, so that atoms can be trapped. We performed detailed studies of the cooling processes in optical lattices by using the time-of-flight and absorption-imaging techniques. We investigated the dependence of the equilibrium temperature on the optical lattice parameters, such as detuning, optical potential and lattice geometry. The presence of neighbouring transitions in the cesium hyperfine level structure was used to break symmetries in order to identify, which role “red” and “blue” transitions play in the cooling. We also examined the limits for the cooling process in optical lattices, and the possible difference in steady-state velocity distributions for different directions. Moreover, in collaboration with ´Ecole Normale Sup´erieure in Paris, numerical simulations were performed in order to get more insight in the cooling dynamics of optical lattices. Optical lattices can keep atoms almost perfectly isolated from the environment and have therefore been suggested as a platform for a host of possible experiments aimed at coherent quantum manipulations, such as spin-squeezing and the implementation of quantum logic-gates. We developed a novel way to trap two different cesium ground states in two distinct, interpenetrating optical lattices, and to change the distance between sites of one lattice relative to sites of the other lattice. This is a first step towards the implementation of quantum simulation schemes in optical lattices.

A spectroscopic and photometric study of MSP companions in Galactic Globular Clusters

This Thesis is devoted to the study of the optical companions of Millisecond Pulsars in Galactic Globular Clusters (GCs) as a part of a large project started at the Department of Astronomy of the Bologna University, in collaboration with other institutions (Astronomical Observatory of Cagliari and Bologna, University of Virginia), specifically dedicated to the study of the environmental effects on passive stellar evolution in galactic GCs. Globular Clusters are very efficient “Kilns” for generating exotic object, such as Millisecond Pulsars (MSP), low mass X-ray binaries(LMXB) or Blue Straggler Stars (BSS). In particular MSPs are formed in binary systems containing a Neutron Star which is spun up through mass accretion from the evolving companion (e.g. Bhattacharia & van den Heuvel 1991). The final stage of this recycling process is either the core of a peeled star (generally an Helium white dwarf) or a very light almos exhausted star, orbiting a very fast rotating Neutron Star (a MSP). Despite the large difference in total mass between the disk of the Galaxy and the Galactic GC system (up a factor 103), the percentage of fast rotating pulsar in binary systems found in the latter is very higher. MSPs in GCs show spin periods in the range 1.3 ÷ 30ms, slowdown rates ˙P 1019 s/s and a lower magnetic field, respect to ”normal” radio pulsars, B 108 gauss . The high probability of disruption of a binary systems after a supernova explosion, explain why we expect only a low percentage of recycled millisecond pulsars respect to the whole pulsar population. In fact only the 10% of the known 1800 radio pulsars are radio MSPs. Is not surprising, that MSP are overabundant in GCs respect to Galactic field, since in the Galactic Disk, MSPs can only form through the evolution of primordial binaries, and only if the binary survives to the supernova explosion which lead to the neutron star formation. On the other hand, the extremely high stellar density in the core of GCs, relative to most of the rest of the Galaxy, favors the formation of several different binary systems, suitable for the recycling of NSs (Davies at al. 1998). In this thesis we will present the properties two millisecond pulsars companions discovered in two globular clusters, the Helium white dwarf orbiting the MSP PSR 1911-5958A in NGC 6752 and the second case of a tidally deformed star orbiting an eclipsing millisecond pulsar, PSR J1701-3006B in NGC6266

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.

Synthese von flüssigkristallinen Polysiloxanen und Charakterisierung der smektischen Phasen

Gegenstand dieser Arbeit ist die Untersuchung der smektischen Phasen von Polysiloxanen mit flüssigkristallinen Seitengruppen (LC-Polysiloxane). Der erste Teil der vorliegenden Arbeit befasste sich mit der Herstellung verschiedener flüssigkristalliner ferroelektrischer Polysiloxane. Die Polymere wurden in Bezug auf das verwendete Polymerrückgrat (Homo- und Copolysiloxan) sowie durch den zusätzlichen Einbau von vernetzbaren Seitengruppen variiert. Im zweiten Teil der Arbeit wurden die Eigenschaften der smektischen Phasen der hergestellten Substanzen näher untersucht. Ein erster Untersuchungsgegenstand war das Dehnungsverhalten von freistehenden flüssigkristallinen Elastomerfilmen (LCE). Bei der Verwendung eines Polymers, in dem nur ein Teil des Polysiloxanrückgrats mit Seitengruppen substituiert ist, wird die uniaxiale Dehnung des Films parallel zu den smektischen Schichten durch eine gleichmäßige Kontraktion in der Filmebene und parallel zur Schichtnormalen ausgeglichen, was auf einen außergewöhnlich niedrigen smektischen Schichtkompressionsmodul zurückzuführen ist. Im Gegensatz dazu ist dieser Modul bei den Homopolymersystemen so groß, dass praktisch senkrecht zu den smektischen Schichten keine Kontraktion stattfindet. Ein zweiter Untersuchungsgegenstand der Netzwerkbildung bestand in der Bestimmung der dynamisch-mechanischen Eigenschaften der LC-Polysiloxane mittels eines Oszillationsrheometers. Hier erfolgten die Messungen von Speicher- und Verlustmodul in Abhängigkeit vom Polymerrückgrat und von der Vernetzung. Die unvernetzten Systeme zeigten in den smektischen Phasen (oberhalb Tg) noch – im wesentlichen – Festkörpereigenschaften (physikalische Vernetzung) mit einem dominierenden Speichermodul beim LC-Homopolysiloxan. Beim LC-Copolysiloxan haben beide Module eine gleiche Größenordnung. Am Phasenübergang in die isotrope Phase wurden beide Module absolut kleiner, der Verlustmodul aber relativ größer. In der isotropen Phase verhalten sich die LC-Polymere damit überwiegend wie viskose Schmelzen. Außerdem korrelierten die mittels DSC bestimmten Phasenübergangstemperaturen mit einer Änderung der dynamisch-mechanischen Eigenschaften. Nach der Vernetzung dominierte der Speichermodul sowohl beim LC-Homo- als auch beim LC-Copolysiloxan bis in die isotrope Phase, und es war aufgrund der Bildung einer festen Netzwerkstruktur keine Abhängigkeit der Module von Phasenübergängen mehr erkennbar. Als dritter Untersuchungsgegenstand wurde der Phasenübergang zwischen den beiden smektischen Phasen (SmC* nach SmA*) der flüssigkristallinen Polysiloxane näher behandelt. Als wichtigstes Ergebnis ist festzuhalten, dass die verdünnten LC-Polysiloxane an diesem Übergang fast keine Schichtdickenänderung aufweisen. Dazu wurde jeweils die röntgenographisch ermittelte Schichtdicke mit der aus den optischen Tiltwinkeln theoretisch berechneten Schichtdicke verglichen. Dadurch konnte gezeigt werden, dass sich die Phasenübergänge nach dem de Vries-Modell verhalten. Damit konnte zum ersten Mal an Polymersystemen ein de Vries-Verhalten nachgewiesen werden. Im Gegensatz dazu zeigte das Homopolysiloxan mit dem Dreiringmesogen beim Übergang von SmC* nach SmA* einen ausgeprägten Sprung in der Schichtdicke. Wie auch durch DSC-Messungen nachweisbar, lag ein Phasenübergang 1. Ordnung vor. Bei den LC-Copolysiloxanen liegt dagegen ein Phasenübergang 2. Ordnung vor. Schließlich wurde die Schichtdicke unter dem Einfluss der Vernetzung untersucht. Beim LC-Copolysiloxan mit dem Dreiringmesogen und einem Anteil an vernetzbaren Gruppen von 15 % wurde eine Stabilisierung der smektischen Phasen erreicht. Zum einen war die Änderung der Schichtdicke am SmC*-SmA*-Phasenübergang geringer im Vergleich zum unvernetzten System und zum anderen war noch 50 °C über der ursprünglichen Klärtemperatur eine smektische Schichtstruktur röntgenographisch nachzuweisen. Insgesamt ist es mit den verschiedenen Untersuchungsmethoden gelungen, einen systematischen Unterschied zwischen smektischen Homo- und Copolysiloxanen aufzuzeigen, der seinen Ursprung – aller Wahrscheinlichkeit nach – in der Mikrophasenseparation von Mesogenen und Polysiloxanketten findet.

Electronic energy transfer processes in pi-conjugated polymers

Currently pi-conjugated polymers are considered as technologically interesting materials to be used as functional building elements for the development of the new generation of optoelectronic devices. More specifically during the last few years, poly-p-phenylene materials have attracted considerable attention for their blue photoluminescence properties. This Thesis deals with the optical properties of the most representative blue light poly-p-phenylene emitters such as poly(fluorene), oligo(fluorene), poly(indenofluorene) and ladder-type penta(phenylene) derivatives. In the present work, laser induced photoluminescence spectroscopy is used as a major tool for the study of the interdependence between the dynamics of the probed photoluminescence, the molecular structures of the prepared polymeric films and the presence of chemical defects. Complementary results obtained by two-dimensional wide-angle X-ray diffraction are reported. These findings show that the different optical properties observed are influenced by the intermolecular solid-state interactions that in turn are controlled by the pendant groups of the polymer backbone. A significant feedback is delivered regarding the positive impact of a new synthetic route for the preparation of a poly(indenofluorene) derivative on the spectral purity of the compound. The energy transfer mechanisms that operate in the studied systems are addressed by doping experiments. After the evaluation of the structure/property interdependence, a new optical excitation pathway is presented. An efficient photon low-energy up-conversion that sensitises the blue emission of poly(fluorene) is demonstrated. The observed phenomenon takes place in poly(fluorene) derivatives hosts doped with metallated octaethyl porphyrins, after quasi-CW photoexcitation of intensities in the order of kW/cm2. The up-conversion process is parameterised in terms of temperature, wavelength excitation and central metal cation in the porphyrin ring. Additionally the observation of the up-conversion is extended in a broad range of poly-p-phenylene blue light emitting hosts. The dependence of the detected up-conversion intensity on the excitation intensity and doping concentration is reported. Furthermore the dynamics of the up-conversion intensity are monitored as a function of the doping concentration. These experimental results strongly suggest the existence of triplet-triplet annihilation events into the porphyrin molecules that are subsequently followed by energy transfer to the host. After confirming the occurrence of the up-conversion in solutions, cyclic voltammetry is used in order to show that the up-conversion efficiency is partially determined from the energetic alignment between the HOMO levels of the host and the dopant.

Grazing incidence pumped Zr x-ray laser for spectroscopy on Li-like ions

X-ray laser fluorescence spectroscopy of the 2s-2p transition in Li-like ions is promising to become a widely applicable tool to provide information on the nuclear charge radii of stable and radioactive isotopes. For performing such experiments at the Experimental Storage Ring ESR, and the future NESR within the FAIR Project, a grazing incidence pumped (GRIP) x-ray laser (XRL) was set up at GSI Darmstadt using PHELIX (Petawatt High Energy Laser for heavy Ions eXperiments). The experiments demonstrated that lasing using the GRIP geometry could be achieved with relatively low pump energy, a prerequisite for higher repetition rate. In the first chapter the need of a plasma XRL is motivated and a short history of the plasma XRL is presented. The distinctive characteristic of the GRIP method is the controlled deposition of the pump laser energy into the desired plasma density region. While up to now the analysis performed were mostly concerned with the plasma density at the turning point of the main pump pulse, in this thesis it is demonstrated that also the energy deposition is significantly modified for the GRIP method, being sensitive in different ways to a large number of parameters. In the second chapter, the theoretical description of the plasma evolution, active medium and XRL emission properties are reviewed. In addition an innovative analysis of the laser absorption in plasma which includes an inverse Bremsstrahlung (IB) correction factor is presented. The third chapter gives an overview of the experimental set-up and diagnostics, providing an analytical formula for the average and instantaneous traveling wave speed generated with a tilted, on-axis spherical mirror, the only focusing system used up to now in GRIP XRL. The fourth chapter describes the experimental optimization and results. The emphasis is on the effect of the incidence angle of the main pump pulse on the absorption in plasma and on output and gain in different lasing lines. This is compared to the theoretical results for two different incidence angles. Significant corrections for the temperature evolution during the main pump pulse due to the incidence angle are demonstrated in comparison to a simple analytical model which does not take into account the pumping geometry. A much better agreement is reached by the model developed in this thesis. An interesting result is also the appearance of a central dip in the spatially resolved keV emission which was observed in the XRL experiments for the first time and correlates well with previous near field imaging and plasma density profile measurements. In the conclusion also an outlook to the generation of shorter wavelength XRL’s is given.

Synthese und Charakterisierung von Oxidchalkogeniden und Bronzen für die Nanostrukturierung

Ausgehend von der Entdeckung der reversiblen Strukturierung mittels Rastersondenmethoden im Phasensystem Na2O/V2O5/P2O5 wurden im Rahmen dieser Arbeit zwei Ansatzpunkte verfolgt. Einerseits sollten mittels der Schmelzflußelektrolyse einige bereits existierende niederdimensionale Molybdänbronzen mit bekannten elektronischen Übergängen in ausreichend großen Kristallen gezüchtet werden, um sie auf ihre Strukturierungseigenschaften hin zu untersuchen. Gleichzeitig sollte durch Variation versucht werden, neue, bisher unbekannte Bronzen oder reduzierte Oxide zu synthetisieren und charakterisieren. Der zweite Schwerpunkt dieser Arbeit lag in der Synthese und Charakterisierung von Oxidchalkogeniden, bestehend aus einem Seltenerdmetall und einem 3d-Metall von Titan bis hin zu den mittleren Übergangsmetallen. Diese Verbindungen können durch die Kombination der jeweiligen Eigenschaften der oxidischen und chalkogeniden Teilstrukturen völlig neue elektronische und/oder magnetische Eigenschaften aufweisen. Mögliche auftretende Phasenübergänge sind wiederum für Strukturierungsversuche interessant. Die zu den Oxidchalkogeniden durchgeführten Untersuchungen ergaben im Phasensystem Ln/Ti/S/O (Ln = Lanthanoide) insgesamt sechs Verbindungen. Zwei von ihnen, La8Ti9S24O4 und Nd20Ti11S44O6, besitzen als gemeinsames Strukturelement tetranukleare [Ti4(u4-S)2(u2-O)4]-Cluster, bestehend aus vier miteinander über gemeinsame Flächen kondensierte TiS4O2-Oktaeder. Die Titanpositionen innerhalb der Cluster sind mit Ti+3-Ionen besetzt. Beide Verbindungen weisen in einem Temperaturbereich zwischen 150 K und 250 K eine deutlich ausgeprägte Hysterese der magnetischen Suszeptibilität auf, die sich im Falle von La8Ti9S24O4 auf einen Jahn-Teller-Übergang zurückführen läßt. Daneben konnte erstmals eine Serie oxidisch/sulfidisch gemischter Ruddlesden-Popper-Verbindungen mit Ln2Ti2S2O5 (Ln = Pr, Nd, Sm) synthetisiert und charakterisiert werden. Titan liegt als vierwertiges Ion in aus TiSO5-Oktaedern gebildeten Perowskit-Doppelschichten vor. Die neunfach koordinierten Positionen sind mit den Seltenerdmetallionen gefüllt, die zwölffach koordinierten Lagen sind unbesetzt. Bei dem sechsten erhaltene Titanoxidsulfid, La4TiS6.5O1.5, handelt es sich um einen Halbleiter mit einer Bandlücke von etwa 2 eV. Weiterhin gelang es, die Serie Ln2M3S2O8 (Ln = La, Ce, Pr, Nd, Sm; M = Nb, Ta) zu synthetisieren und in ihren physikalischen Eigenschaften zu charakterisieren. Es handelt sich ausnahmslos um Halbleiter mit Bandlücken zwischen E=0.125 eV für La2Nb3S2O8 und E=0.222 eV für Pr2Ta3S2O8. Die Struktur der Oxidsulfide Ce2Ta3S2O8, Pr2Ta3S2O8, Nd2Nb3S2O8 sowie Sm2Ta3S2O8 weist im Gegensatz zu den anderen Verbindungen eine Fehlordnung eines der beiden kristallographisch unabhängigen Nb- bzw. Ta-Atome auf. Daraus resultiert eine Symmetrieerniedrigung von Pnma zu Pbam. Der Einsatz von Europium führte zu einer neuen Modifikation des bronzoiden Oxids EuTa2O6, in der das Europium als Eu+2 vorliegt, wie 151Eu-Mößbauer-Untersuchungen bestätigten. Vor der Durchführung der Kristallzüchtungen mittels der Schmelzflußelektrolysen mußten die benutzen Öfen und Elektrolysezellen geplant und angefertigt werden. Es konnten dann verschiedene blaue, rote und violette Moybdänbronzen (sowie La2Mo2O7) in Kristallen bis zu 25 mm Länge dargestellt werden. Ferner gelang die erste exakte Einkristalluntersuchung der roten Bronze Rb0.33MoO3. Sie verfügt über die höchste d-Elektronen-Lokalisierungsrate aller bekannten roten Bronzen. Die erhaltenen Bronzen wurden teilweise von der Arbeitsgruppe Fuchs, Physikalisches Institut der Westfälischen Wilhelms-Universität Münster, auf ihre Nanostrukturierbarkeit hin untersucht. Dabei ergaben sich zwei verschiedene Strukturierungsmechanismen. Sind es im Fall der blauen Alkalimetall-Molybdänbronzen ausschließlich Lochstrukturen, die entstehen, handelt es sich bei La2Mo2O7 um Hügelstrukturen. Mittels der Schmelzflußelektrolyse konnte auch das gemischtvalente Alkalimetall-Eisenmolybdat NaFe2(MoO4)3 synthetisiert werden. Daneben gelang die Synthese dreier weiterer Alkalimetall-Eisenmolybdate: Cs2Fe2(MoO4)3, NaFe4(MoO4)5 und CsFe5(MoO4)7. Bis auf Cs2Fe2(MoO4)3, welches in der bekannten Langbeinit-Struktur kristallisiert, handelt es sich bei den übrigen Alkalimetall-Eisenmolybdaten um völlig neuartige Käfigverbindungen, bzw. bei CsFe5(MoO4)7 um eine Tunnelverbindung. Die Kristallstrukturen beinhalten kondensierte FeO6-Oktaeder. Im Fall von NaFe2(MoO4)3 lassen sich [Fe2O10]-Einheiten, für NaFe4(MoO4)5 [Fe2O10]- sowie [Fe3O14]-Einheiten, und für CsFe5(MoO4)7 [Fe4O18]-Baueinheiten beobachten. Die Positionen der Fe+2- und Fe+3-Atome in NaFe4(MoO4)5 wurden mit Hilfe einer 57Fe-Mößbauer-Untersuchung bestimmt.