TY - JOUR A1 - Thapa, Samudrajit A1 - Wyłomańska, Agnieszka A1 - Sikora, Grzegorz A1 - Wagner, Caroline E. A1 - Krapf, Diego A1 - Kantz, Holger A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Leveraging large-deviation statistics to decipher the stochastic properties of measured trajectories JF - New Journal of Physics N2 - Extensive time-series encoding the position of particles such as viruses, vesicles, or individualproteins are routinely garnered insingle-particle tracking experiments or supercomputing studies.They contain vital clues on how viruses spread or drugs may be delivered in biological cells.Similar time-series are being recorded of stock values in financial markets and of climate data.Such time-series are most typically evaluated in terms of time-averaged mean-squareddisplacements (TAMSDs), which remain random variables for finite measurement times. Theirstatistical properties are different for differentphysical stochastic processes, thus allowing us toextract valuable information on the stochastic process itself. To exploit the full potential of thestatistical information encoded in measured time-series we here propose an easy-to-implementand computationally inexpensive new methodology, based on deviations of the TAMSD from itsensemble average counterpart. Specifically, we use the upper bound of these deviations forBrownian motion (BM) to check the applicability of this approach to simulated and real data sets.By comparing the probability of deviations fordifferent data sets, we demonstrate how thetheoretical bound for BM reveals additional information about observed stochastic processes. Weapply the large-deviation method to data sets of tracer beads tracked in aqueous solution, tracerbeads measured in mucin hydrogels, and of geographic surface temperature anomalies. Ouranalysis shows how the large-deviation properties can be efficiently used as a simple yet effectiveroutine test to reject the BM hypothesis and unveil relevant information on statistical propertiessuch as ergodicity breaking and short-time correlations. KW - diffusion KW - anomalous diffusion KW - large-deviation statistic KW - time-averaged mean squared displacement KW - Chebyshev inequality Y1 - 2020 U6 - https://doi.org/10.1088/1367-2630/abd50e SN - 1367-2630 VL - 23 PB - Dt. Physikalische Ges. ; IOP CY - Bad Honnef ; London ER - TY - THES A1 - Keles, Engin T1 - Atmospheric properties and dynamics of gaseous exoplanets inferred from high-resolution alkali line transmission spectroscopy N2 - The characterization of exoplanets applying high-resolution transmission spectroscopy ini- tiated a new era making it possible to trace atmospheric signature at high altitudes in exoplanet atmospheres and to determine atmospheric properties which enrich our under- standing of the formation and evolution of the solar system. In contrast to what is observed in our solar system, where gaseous planets orbit at wide orbits, Jupiter type exoplanets were detected in foreign stellar systems surrounding their host stars within few days, in close orbits, the so called hot- and ultra-hot Jupiters. The most well studied ones are HD209458b and HD189733b, which are the first exoplanets where absorption is detected in their atmospheres, namely from the alkali line sodium. For hot Jupiters, the resonant alkali lines are the atmospheric species with one of the strongest absorption signatures, due to their large absorption cross-section. However, al- though the alkali lines sodium and potassium were detected in low-resolution observations for various giant exoplanets, potassium was absent in different high-resolution investiga- tions in contrast to sodium. The reason for this is quite puzzling, since both alkalis have very similar physical and chemical properties (e.g. condensation and ionization proper- ties). Obtaining high-resolution transit observations of HD189733b and HD209458b, we were able to detect potassium on HD189733b (Manuscript 1), which was the first high-resolution detection of potassium on an exoplanet. The absence of potassium on HD209458b could be reasoned by depletion processes, such as condensation or photo-ionization or high-altitude clouds. In a further study (Manuscript II), we resolved the potassium line and compared this to a previously detected sodium absorption on this planet. The comparison showed, that the potassium lines are either tracing different altitudes and temperatures compared to the sodium lines, or are depleted so that the planetary Na/K- ratio is way larger than the stellar one. A comparison of the alkali lines with synthetic line profiles showed that the sodium lines were much broader than the potassium lines, probably being induced by winds. To investigate this, the effect of zonal streaming winds on the sodium lines on Jupiter-type planets is investigated in a further study (Manuscript III), showing that such winds can significantly broaden the Na- lines and that high-resolution observations can trace such winds with different properties. Furthermore, investigating the Na-line observations for different exoplanets, I showed that the Na-line broadening follows a trend with cooler planets showing stronger line broadening and so hinting on stronger winds, matching well into theoretical predictions. Each presented manuscript depends on the re- sults published within the previous manuscript, yielding a unitary study of the exoplanet HD189733b. The investigation of the potassium absorption required to account for different effects: The telluric lines removal and the effect of center-to-limb variation (see Manuscript I), the residual Rossiter-Mc-Laughlin effect (see Manuscript II) and the broadening of spectral lines on a translucent atmospheric ring by zonal jet streams (see Manuscript III). This thesis shows that high-resolution transmission spectroscopy is a powerful tool to probe sharp alkali line absorption on giant exoplanet atmospheres and to investigate on the properties and dynamics of hot Jupiter type atmospheres. KW - planets and satellites: atmospheres KW - planets and satellites: composition KW - planets and satellites: gaseous planets KW - exoplanets Y1 - 2021 ER - TY - JOUR A1 - Teichmann, Erik T1 - Using phase dynamics to study partial synchrony BT - three examples JF - European physical journal special topics N2 - Partial synchronous states appear between full synchrony and asynchrony and exhibit many interesting properties. Most frequently, these states are studied within the framework of phase approximation. The latter is used ubiquitously to analyze coupled oscillatory systems. Typically, the phase dynamics description is obtained in the weak coupling limit, i.e., in the first-order in the coupling strength. The extension beyond the first-order represents an unsolved problem and is an active area of research. In this paper, three partially synchronous states are investigated and presented in order of increasing complexity. First, the usage of the phase response curve for the description of macroscopic oscillators is analyzed. To achieve this, the response of the mean-field oscillations in a model of all-to-all coupled limit-cycle oscillators to pulse stimulation is measured. The next part treats a two-group Kuramoto model, where the interaction of one attractive and one repulsive group results in an interesting solitary state, situated between full synchrony and self-consistent partial synchrony. In the last part, the phase dynamics of a relatively simple system of three Stuart-Landau oscillators are extended beyond the weak coupling limit. The resulting model contains triplet terms in the high-order phase approximation, though the structural connections are only pairwise. Finally, the scaling of the new terms with the coupling is analyzed. Y1 - 2021 U6 - https://doi.org/10.1140/epjs/s11734-021-00156-3 SN - 1951-6355 SN - 1951-6401 VL - 230 IS - 14-15 SP - 2833 EP - 2842 PB - Springer CY - Heidelberg ER - TY - JOUR A1 - Rubio, Jesús A1 - Anders, Janet A1 - Correa, Luis A. T1 - Global quantum thermometry JF - Physical review letters / publ. by the American Physical Society N2 - A paradigm shift in quantum thermometry is proposed. To date, thermometry has relied on local estimation, which is useful to reduce statistical fluctuations once the temperature is very well known. In order to estimate temperatures in cases where few measurement data or no substantial prior knowledge are available, we build instead a method for global quantum thermometry. Based on scaling arguments, a mean logarithmic error is shown here to be the correct figure of merit for thermometry. Its full minimization provides an operational and optimal rule to postprocess measurements into a temperature reading, and it establishes a global precision limit. We apply these results to the simulated outcomes of measurements on a spin gas, finding that the local approach can lead to biased temperature estimates in cases where the global estimator converges to the true temperature. The global framework thus enables a reliable approach to data analysis in thermometry experiments. Y1 - 2021 U6 - https://doi.org/10.1103/PhysRevLett.127.190402 SN - 0031-9007 SN - 1079-7114 VL - 127 IS - 19 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Keles, Engin T1 - Spectral signature of atmospheric winds in high-resolution transit observations JF - Monthly Notices of the Royal Astronomical Society N2 - The study of exoplanet atmospheres showed large diversity compared to the planets in our Solar system. Especially Jupiter-type exoplanets orbiting their host star in close orbits, the so-called hot and ultra-hot Jupiters, have been studied in detail due to their enhanced atmospheric signature. Due to their tidally locked status, the temperature difference between the day- and nightside triggers atmospheric winds that can lead to various fingerprints in the observations. Spatially resolved absorption lines during transit such as sodium (Na) could be a good tracer for such winds. Different works resolved the Na absorption lines on different exoplanets which show different line widths. Assuming that this could be attributed to such zonal jet streams, this work models the effect of such winds on synthetic absorption lines. For this, transiting Jupiter-type planets with rotational velocities similar to hot and ultra-hot Jupiter are considered. The investigation shows that high wind velocities could reproduce the broadening of Na-line profiles inferred in different high-resolution transit observations. There is a tendency that the broadening values decrease for planets with lower equilibrium temperature. This could be explained by atmospheric drag induced by the ionization of alkali lines that slow down the zonal jet streams, favouring their existence on hot Jupiter rather than ultra-hot Jupiter. Y1 - 2021 U6 - https://doi.org/10.1093/mnras/stab099 VL - 502 IS - 1 SP - 1456 EP - 1468 PB - Oxford Univ. Press CY - Oxford ER - TY - THES A1 - Diercke, Andrea T1 - Physical environment of large-scale high-latitude and polar crown filaments T1 - Die Physik von polaren Filamenten N2 - Filaments are omnipresent features in the solar chromosphere, one of the atmospheric layers of the Sun, which is located above the photosphere, the visible surface of the Sun. They are clouds of plasma reaching from the photosphere to the chromosphere, and even to the outer-most atmospheric layer, the corona. They are stabalized by the magnetic field. If the magnetic field is disturbed, filaments can erupt as coronal mass ejections (CME), releasing plasma into space, which can also hit the Earth. A special type of filaments are polar crown filaments, which form at the interface of the unipolar field of the poles and flux of opposite magnetic polarity, which was transported towards the poles. This flux transport is related to the global dynamo of the Sun and can therefore be analyzed indirectly with polar crown filaments. The main objective of this thesis is to better understand the physical properties and environment of high-latitude and polar crown filaments, which can be approached from two perspectives: (1) analyzing the large-scale properties of high-latitude and polar crown filaments with full-disk Hα observations from the Chromospheric Telescope (ChroTel) and (2) determining the relation of polar crown and high-latitude filaments from the chromosphere to the lower-lying photosphere with high-spatial resolution observations of the Vacuum Tower Telescope (VTT), which reveal the smallest details. The Chromospheric Telescope (ChroTel) is a small 10-cm robotic telescope at Observatorio del Teide on Tenerife (Spain), which observes the entire Sun in Hα, Ca IIK, and He I 10830 Å. We present a new calibration method that includes limb-darkening correction, removal of non-uniform filter transmission, and determination of He I Doppler velocities. Chromospheric full-disk filtergrams are often obtained with Lyot filters, which may display non-uniform transmission causing large-scale intensity variations across the solar disk. Removal of a 2D symmetric limb-darkening function from full-disk images results in a flat background. However, transmission artifacts remain and are even more distinct in these contrast-enhanced images. Zernike polynomials are uniquely appropriate to fit these large-scale intensity variations of the background. The Zernike coefficients show a distinct temporal evolution for ChroTel data, which is likely related to the telescope’s alt-azimuth mount that introduces image rotation. In addition, applying this calibration to sets of seven filtergrams that cover the He I triplet facilitates determining chromospheric Doppler velocities. To validate the method, we use three datasets with varying levels of solar activity. The Doppler velocities are benchmarked with respect to co-temporal high-resolution spectroscopic data of the GREGOR Infrared Spectrograph (GRIS). Furthermore, this technique can be applied to ChroTel Hα and Ca IIK data. The calibration method for ChroTel filtergrams can be easily adapted to other full-disk data exhibiting unwanted large-scale variations. The spectral region of the He I triplet is a primary choice for high-resolution near-infrared spectropolarimetry. Here, the improved calibration of ChroTel data will provide valuable context data. Polar crown filaments form above the polarity inversion line between the old magnetic flux of the previous cycle and the new magnetic flux of the current cycle. Studying their appearance and their properties can lead to a better understanding of the solar cycle. We use full-disk data of the ChroTel at Observatorio del Teide, Tenerife, Spain, which were taken in three different chromospheric absorption lines (Hα 6563 Å, Ca IIK 3933 Å, and He I 10830 Å), and we create synoptic maps. In addition, the spectroscopic He I data allow us to compute Doppler velocities and to create synoptic Doppler maps. ChroTel data cover the rising and decaying phase of Solar Cycle 24 on about 1000 days between 2012 and 2018. Based on these data, we automatically extract polar crown filaments with image-processing tools and study their properties. We compare contrast maps of polar crown filaments with those of quiet-Sun filaments. Furthermore, we present a super-synoptic map summarizing the entire ChroTel database. In summary, we provide statistical properties, i.e. number and location of filaments, area, and tilt angle for both the maximum and declining phase of Solar Cycle 24. This demonstrates that ChroTel provides a promising dataset to study the solar cycle. The cyclic behavior of polar crown filaments can be monitored by regular full-disk Hα observations. ChroTel provides such regular observations of the Sun in three chromospheric wavelengths. To analyze the cyclic behavior and the statistical properties of polar crown filaments, we have to extract the filaments from the images. Manual extraction is tedious, and extraction with morphological image processing tools produces a large number of false positive detections and the manual extraction of these takes too much time. Automatic object detection and extraction in a reliable manner allows us to process more data in a shorter time. We will present an overview of the ChroTel database and a proof of concept of a machine learning application, which allows us a unified extraction of, for example, filaments from ChroTel data. The chromospheric Hα spectral line dominates the spectrum of the Sun and other stars. In the stellar regime, this spectral line is already used as a powerful tracer of magnetic activity. For the Sun, other tracers are typically used to monitor solar activity. Nonetheless, the Sun is observed constantly in Hα with globally distributed ground-based full-disk imagers. The aim of this study is to introduce Hα as a tracer of solar activity and compare it to other established indicators. We discuss the newly created imaging Hα excess in the perspective of possible application for modelling of stellar atmospheres. In particular, we try to determine how constant is the mean intensity of the Hα excess and number density of low-activity regions between solar maximum and minimum. Furthermore, we investigate whether the active region coverage fraction or the changing emission strength in the active regions dominates time variability in solar Hα observations. We use ChroTel observations of full-disk Hα filtergrams and morphological image processing techniques to extract the positive and negative imaging Hα excess, for bright features (plage regions) and dark absorption features (filaments and sunspots), respectively. We describe the evolution of the Hα excess during Solar Cycle 24 and compare it to other well established tracers: the relative sunspot number, the F10.7 cm radio flux, and the Mg II index. Moreover, we discuss possible applications of the Hα excess for stellar activity diagnostics and the contamination of exoplanet transmission spectra. The positive and negative Hα excess follow the behavior of the solar activity over the course of the cycle. Thereby, positive Hα excess is closely correlated to the chromospheric Mg II index. On the other hand, the negative Hα excess, created from dark features like filaments and sunspots, is introduced as a tracer of solar activity for the first time. We investigated the mean intensity distribution for active regions for solar minimum and maximum and found that the shape of both distributions is very similar but with different amplitudes. This might be related with the relatively stable coronal temperature component during the solar cycle. Furthermore, we found that the coverage fraction of Hα excess and the Hα excess of bright features are strongly correlated, which will influence modelling of stellar and exoplanet atmospheres. High-resolution observations of polar crown and high-latitude filaments are scarce. We present a unique sample of such filaments observed in high-resolution Hα narrow-band filtergrams and broad-band images, which were obtained with a new fast camera system at the VTT. ChroTel provided full-disk context observations in Hα, Ca IIK, and He I 10830 Å. The Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) provided line-of-sight magnetograms and ultraviolet (UV) 1700 Å filtergrams, respectively. We study filigree in the vicinity of polar crown and high-latitude filaments and relate their locations to magnetic concentrations at the filaments’ footpoints. Bright points are a well studied phenomenon in the photosphere at low latitudes, but they were not yet studied in the quiet network close to the poles. We examine size, area, and eccentricity of bright points and find that their morphology is very similar to their counterparts at lower latitudes, but their sizes and areas are larger. Bright points at the footpoints of polar crown filaments are preferentially located at stronger magnetic flux concentrations, which are related to bright regions at the border of supergranules as observed in UV filtergrams. Examining the evolution of bright points on three consecutive days reveals that their amount increases while the filament decays, which indicates they impact the equilibrium of the cool plasma contained in filaments. N2 - Filamente sind omnipräsente Strukturen in der Chromosphäre der Sonne. Diese Schicht befindet sich über der Photosphäre, welche die sichtbare Oberfläche der Sonne darstellt. Filamente sind Plasmagebilde, welche in der Photosphäre verankert sind und von der Chromosphäre in die Korona reichen, der äußersten Atmosphärenschicht der Sonne. Diese Strukturen werden durch das Magnetfeld der Sonne stabilisiert. Durch Störungen des Magnetfelds, destabilisiert sich das Filament und das dort enthaltene Plasma kann als Sonneneruption, ein sogenannter koronaler Massenauswurf, ins Weltall geschleudert werden, welcher auch die Erde treffen könnte. Das Verständnis von Filamenten, deren Stabilität und Verbindung zum Magnetfeld sind ungemein wichtig, um Sonneneruptionen besser verstehen und vorhersagen zu können. Ein spezieller Typ von Filamenten, sind polare Filamente, (engl. polar crown filaments). Diese bilden sich an der Grenzfläche des unipolaren Magnetfelds an den Polen und dem Magnetfeld von gemischten Polaritäten in den Aktivitätsgürteln der Sonne. In letzteren werden Reste von bipolaren und zerfallenen Sonnenfleckengruppen zum Pol transportiert. Dieser Transport wird durch den Sonnendynamo initialisiert, so dass die Untersuchung polarer Filamente indirekt Rückschlüsse auf den Sonnendynamo zulässt. Die vorliegende Arbeit untersucht die polaren Filamente aus zwei Perspektiven. Zum einen aus der globalen Perspektive, bei der wir synoptische Beobachtungen der gesamten Sonnenscheibe nutzen, um das zyklische Verhalten der Filamente zu untersuchen. Zum anderen aus einer detailorientierten Perspektive, wobei wir hochaufgelöste Beobachtungen der Filamente auswerten, um mehr über die Verbindung von kühlem chromosphärischem Plasma zum Magnetfeld zu erfahren. Für die Untersuchung des zyklischen Verhaltens von polaren Filamenten nutzen wir Daten des Chromospheric Telescope (ChroTel), welches alle drei Minuten Aufnahmen der Chromosphäre in drei verschiedenen Wellenlängen macht. Die Wasserstofflinie der Balmerserie Hα ist dabei die beste Möglichkeit Filamente in der Chromosphäre abzubilden. Eine während dieser Arbeit entwickelte Methode, zum Korrigieren von Intensitätsungleichmäßigkeiten in Sonnenbildern, legt den Grundstein für alle weiteren Studien mit diesen Daten. Die Filamente können somit aus den Bildern heraus extrahiert werden und damit kann der aktuelle Sonnenzyklus zwischen Maximum und Minimum untersucht werden. Wir konnten die Wanderung der polaren Filamente für den Sonnenzyklus 24 in den Daten lokalisieren und die polwärtsgerichtete Geschwindigkeit bestimmen, welche wir mit vorherigen Ergebnissen verglichen haben. Da die morphologischen Bildbearbeitungsmethode, welche wir zur Extraktion der Filamente benutzt haben, auch andere Strukturen, wie Sonnenflecken nicht ausschließen konnte, haben wir neue Methoden entwickelt, die auf Maschinellem Lernen mit tiefen neuronalen Netzwerken beruhen. Die vorläufigen Ergebnisse sind sehr vielversprechend und auch auf Hα Bildern von anderen Teleskopen leicht übertragbar. Für die Untersuchung der polaren Filamente mit hochaufgelösten Bildern verwenden wir Beobachtungen vom Vakuumturmteleskop (VTT) auf Teneriffa, Spanien. Die Bilder wurden mit Hα Schmal- und Breitbandfiltern aufgenommen und zeigen sowohl die Chromosphäre als auch die Photosphäre. Wir untersuchen dabei die kleinsten auflösbaren Aufhellungen, (engl. bright points), welche in Verbindung mit dem Magnetfeld stehen. Diese kleinskaligen Aufhellungen finden wir vor allem an den Fußpunktregionen der Filamente, die mit starken Konzentrationen vom Magnetfeld korrelieren. Solche hellen Punkte in der Nähe von polaren Filamenten wurden bisher nie mit hochaufgelösten Beobachtungen untersucht. Die statistische Auswertung dieser Strukturen zeigt, dass sie sich kaum von ihren äquatornahen Gegenstücken unterscheiden, mit Ausnahme einer tendenziell größeren Fläche. KW - Solar Physics KW - Sonnenphysik KW - Filaments KW - Filamente KW - Chromosphere KW - Chromosphäre Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-511301 ER - TY - THES A1 - Lepro, Valentino T1 - Experimental and theoretical study on amoeboid cell-cargo active motion BT - a physical analysis of cell-mediated particle transport N2 - As society paves its way towards device miniaturization and precision medicine, micro-scale actuation and guided transport become increasingly prominent research fields, with high potential impact in both technological and clinical contexts. In order to accomplish directed motion of micron-sized objects, as biosensors and drug-releasing microparticles, towards specific target sites, a promising strategy is the use of living cells as smart biochemically-powered carriers, building the so-called bio-hybrid systems. Inspired by leukocytes, native cells of living organisms efficiently migrating to critical targets as tumor tissue, an emerging concept is to exploit the amoeboid crawling motility of such cells as mean of transport for drug delivery applications. In the research work described in this thesis, I synergistically applied experimental, computational and theoretical modeling approaches to investigate the behaviour and transport mechanism of a novel kind of bio-hybrid system for active transport at the micro-scale, referred to as cellular truck. This system consists of an amoeboid crawling cell, the carrier, attached to a microparticle, the cargo, which may ideally be drug-loaded for specific therapeutic treatments. For the purposes of experimental investigation, I employed the amoeba Dictyostelium discoideum as crawling cellular carrier, being a renowned model organism for leukocyte migration and, in general, for eukaryotic cell motility. The performed experiments revealed a complex recurrent cell-cargo relative motion, together with an intermittent motility of the cellular truck as a whole. The evidence suggests the presence of cargoes on amoeboid cells to act as mechanical stimulus leading cell polarization, thus promoting cell motility and giving rise to the observed intermittent dynamics of the truck. Particularly, bursts in cytoskeletal polarity along the cell-cargo axis have been found to occur in time with a rate dependent on cargo geometrical features, as particle diameter. Overall, the collected experimental evidence pointed out a pivotal role of cell-cargo interactions in the emergent cellular truck motion dynamics. Especially, they can determine the transport capabilities of amoeboid cells, as the cargo size significantly impacts the cytoskeletal activity and repolarization dynamics along the cell-cargo axis, the latter responsible for truck displacement and reorientation. Furthermore, I developed a modeling framework, built upon the experimental evidence on cellular truck behaviour, that connects the relative dynamics and interactions arising at the truck scale with the actual particle transport dynamics. In fact, numerical simulations of the proposed model successfully reproduced the phenomenology of the cell-cargo system, while enabling the prediction of the transport properties of cellular trucks over larger spatial and temporal scales. The theoretical analysis provided a deeper understanding of the role of cell-cargo interaction on mass transport, unveiling in particular how the long-time transport efficiency is governed by the interplay between the persistence time of cell polarity and time scales of the relative dynamics stemming from cell-cargo interaction. Interestingly, the model predicts the existence of an optimal cargo size, enhancing the diffusivity of cellular trucks; this is in line with previous independent experimental data, which appeared rather counterintuitive and had no explanation prior to this study. In conclusion, my research work shed light on the importance of cargo-carrier interactions in the context of crawling cell-mediated particle transport, and provides a prototypical, multifaceted framework for the analysis and modelling of such complex bio-hybrid systems and their perspective optimization. N2 - Im Zuge der fortschreitenden gesellschaftlichen Entwicklung hin zur Miniaturisierung und Präzisionsmedizin, gewinnen Fragen zu Antrieb und zielgerichtetem Transport auf der Mikrometerskala zunehmend an Bedeutung, nicht zuletzt wegen ihres kaum zu unterschätzendem Potentials für Medizin und Technik. Eine vielversprechende Strategie, um den zielgerichteten Transport von Objekten auf der Mikrometerskala, wie zum Beispiel Biosensoren oder mit Medikamenten beladene Mikropartikel, zu bewerkstelligen, ist die Verwendung von lebenden Zellen als intelligenten, biochemisch angetriebenen Transportern. Zellen und Mikroobjekte bilden dabei gemeinsam sogenannte Bio-Hybridsysteme. Inspiriert von Leukozyten - nativen Zellen lebender Organismen, welche sich effizient zu kritischen Zielen, wie Tumorgewebe, bewegen - besteht ein neues Konzept darin, die amöboide Fortbewegung solcher Zellen für den Medikamententransport zu nutzen. Im Rahmen dieser Doktorarbeit kamen experimentelle, numerische und theoretische Modellierungsansätze zum Einsatz, um die Eigenschaften und Transportmechanismen eines neuen Bio-Hybridsystems für den aktiven Transport von Objekten auf der Mikrometerskala zu untersuchen. Dieses Bio-Hybridsystem wird im Folgenden als Zelltransporter bezeichnet. Ein Zelltransporter besteht aus einer sich amöboid fortbewegenden Zelle, dem Transporter, und einem Mikropartikel, der Fracht, welche idealerweise mit Medikamenten für therapeutische Zwecke beladen sein kann. Für die experimentellen Untersuchungen wurde die Amöbe Dictyostelium discoideum als Transporter verwendet. Sie ist ein bekannter Modellorganismus für die Leukozytenmigration und für die Motilität eukaryotischer Zellen im Allgemeinem. Die durchgeführten Experimente zeigten eine komplexe, periodische Zell-Fracht-Relativbewegung, zusammen mit einer intermittierenden Motilität des gesamten Zelltransporters. Die experimentellen Beobachtungen weisen darauf hin, dass die Anwesenheit der Fracht als mechanischer Stimulus auf die amöboide Zelle wirkt und zur Zellpolarisation führt, was wiederum die Zellmotilität fördert und die intermittierende Dynamik des Zelltransportes begründet. So wurde festgestellt, dass das Auftreten der Polarisation des Zytoskeletts entlang der Zell-Fracht-Achse von den geometrischen Merkmalen der Fracht, wie zum Beispiel des Partikeldurchmessers, abhängt. Insgesamt wiesen die gesammelten experimentellen Daten auf eine zentrale Rolle der Zell-Fracht-Wechselwirkungen in der Bewegungsdynamik von Zelltransportern hin. Insbesondere kann die Zell-Fracht-Wechselwirkung die Transportfähigkeiten von amöboiden Zellen erheblich beeinflussen, da die Größe der Fracht die Aktivität des Zytoskeletts und die Repolarisationsdynamik entlang der Zell-Fracht-Achse modelliert, wobei letzteres für die Verlagerung und Neuorientierung des Zelltransportes verantwortlich ist. Darüber hinaus wurde eine Modellierung entwickelt, welche auf den experimentellen Erkenntnissen zum Verhalten der Zelltransporter aufbaut und die relative Dynamik auf Zelltranporterebene, mit der tatsächlichen Partikeltransportdynamik verbindet. Tatsächlich reproduzierten numerische Simulationen des vorgeschlagenen Modells erfolgreich die Phänomenologie des Zell-Fracht-Systems und ermöglichten gleichzeitig die Vorhersage der Transporteigenschaften von Zelltransportern über größere räumliche und zeitliche Skalen. Des Weiteren liefert die theoretische Analyse ein tieferes Verständnis der Rolle der Zell-Fracht-Wechselwirkung beim Massentransport und zeigte insbesondere, wie die Langzeittransporteffizienz durch das Zusammenspiel von Persistenzzeit der Zellpolarität und den Zeitskalen der relativen Dynamik, welche sich aus der Zell-Fracht-Interaktion ergeben, bestimmt wird. Interessanterweise sagt das Modell die Existenz einer optimalen Frachtgröße voraus, wodurch die Diffusivität von Zelltransportern maximiert wird. Dies steht im Einklang mit früheren, unabhängigen experimentellen Daten, für die es vor dieser Studie keine Erklärung gab. Zusammenfassend lässt sich sagen, dass die vorliegende Forschungsarbeit Licht auf die Bedeutung von Transporter-Fracht-Wechselwirkungen, beim Partikeltransports mittels amöboider Zellen, wirft und eine breite Grundlage für die Analyse und Modellierung komplexer Bio-Hybridsysteme und deren perspektivische Optimierung schafft. KW - biophysics KW - bio-hybrid system KW - particle transport KW - active transport KW - amoeboid motion KW - Biophysik KW - Bio-Hybridsystem KW - Partikeltransport KW - aktiven Transport KW - amöboide Bewegung Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-490890 ER - TY - GEN A1 - Thapa, Samudrajit A1 - Wyłomańska, Agnieszka A1 - Sikora, Grzegorz A1 - Wagner, Caroline E. A1 - Krapf, Diego A1 - Kantz, Holger A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Leveraging large-deviation statistics to decipher the stochastic properties of measured trajectories T2 - Postprints der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe N2 - Extensive time-series encoding the position of particles such as viruses, vesicles, or individualproteins are routinely garnered insingle-particle tracking experiments or supercomputing studies.They contain vital clues on how viruses spread or drugs may be delivered in biological cells.Similar time-series are being recorded of stock values in financial markets and of climate data.Such time-series are most typically evaluated in terms of time-averaged mean-squareddisplacements (TAMSDs), which remain random variables for finite measurement times. Theirstatistical properties are different for differentphysical stochastic processes, thus allowing us toextract valuable information on the stochastic process itself. To exploit the full potential of thestatistical information encoded in measured time-series we here propose an easy-to-implementand computationally inexpensive new methodology, based on deviations of the TAMSD from itsensemble average counterpart. Specifically, we use the upper bound of these deviations forBrownian motion (BM) to check the applicability of this approach to simulated and real data sets.By comparing the probability of deviations fordifferent data sets, we demonstrate how thetheoretical bound for BM reveals additional information about observed stochastic processes. Weapply the large-deviation method to data sets of tracer beads tracked in aqueous solution, tracerbeads measured in mucin hydrogels, and of geographic surface temperature anomalies. Ouranalysis shows how the large-deviation properties can be efficiently used as a simple yet effectiveroutine test to reject the BM hypothesis and unveil relevant information on statistical propertiessuch as ergodicity breaking and short-time correlations. T3 - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 1118 KW - diffusion KW - anomalous diffusion KW - large-deviation statistic KW - time-averaged mean squared displacement KW - Chebyshev inequality Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-493494 SN - 1866-8372 IS - 1118 ER - TY - JOUR A1 - Kluge, Lucas A1 - Schewe, Jacob T1 - Evaluation and extension of the radiation model for internal migration JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - Human migration is often studied using gravity models. These models, however, have known limitations, including analytic inconsistencies and a dependence on empirical data to calibrate multiple parameters for the region of interest. Overcoming these limitations, the radiation model has been proposed as an alternative, universal approach to predicting different forms of human mobility, but has not been adopted for studying migration. Here we show, using data on within-country migration from the USA and Mexico, that the radiation model systematically underpredicts long-range moves, while the traditional gravity model performs well for large distances. The universal opportunity model, an extension of the radiation model, shows an improved fit of long-range moves compared to the original radiation model, but at the cost of introducing two additional parameters. We propose a more parsimonious extension of the radiation model that introduces a single parameter. We demonstrate that it fits the data over the full distance spectrum and also-unlike the universal opportunity model-preserves the analytical property of the original radiation model of being equivalent to a gravity model in the limit of a uniform population distribution. Y1 - 2021 U6 - https://doi.org/10.1103/PhysRevE.104.054311 SN - 2470-0045 SN - 2470-0053 SN - 2470-0061 VL - 104 IS - 5 PB - American Physical Society CY - College Park ER - TY - THES A1 - Brugger, Julia T1 - Modeling changes in climate during past mass extinctions T1 - Modellierung von Klimaveränderungen während vergangener Massenaussterben N2 - The evolution of life on Earth has been driven by disturbances of different types and magnitudes over the 4.6 million years of Earth’s history (Raup, 1994, Alroy, 2008). One example for such disturbances are mass extinctions which are characterized by an exceptional increase in the extinction rate affecting a great number of taxa in a short interval of geologic time (Sepkoski, 1986). During the 541 million years of the Phanerozoic, life on Earth suffered five exceptionally severe mass extinctions named the “Big Five Extinctions”. Many mass extinctions are linked to changes in climate (Feulner, 2009). Hence, the study of past mass extinctions is not only intriguing, but can also provide insights into the complex nature of the Earth system. This thesis aims at deepening our understanding of the triggers of mass extinctions and how they affected life. To accomplish this, I investigate changes in climate during two of the Big Five extinctions using a coupled climate model. During the Devonian (419.2–358.9 million years ago) the first vascular plants and vertebrates evolved on land while extinction events occurred in the ocean (Algeo et al., 1995). The causes of these formative changes, their interactions and their links to changes in climate are still poorly understood. Therefore, we explore the sensitivity of the Devonian climate to various boundary conditions using an intermediate-complexity climate model (Brugger et al., 2019). In contrast to Le Hir et al. (2011), we find only a minor biogeophysical effect of changes in vegetation cover due to unrealistically high soil albedo values used in the earlier study. In addition, our results cannot support the strong influence of orbital parameters on the Devonian climate, as simulated with a climate model with a strongly simplified ocean model (De Vleeschouwer et al., 2013, 2014, 2017). We can only reproduce the changes in Devonian climate suggested by proxy data by decreasing atmospheric CO2. Still, finding agreement between the evolution of sea surface temperatures reconstructed from proxy data (Joachimski et al., 2009) and our simulations remains challenging and suggests a lower δ18O ratio of Devonian seawater. Furthermore, our study of the sensitivity of the Devonian climate reveals a prevailing mode of climate variability on a timescale of decades to centuries. The quasi-periodic ocean temperature fluctuations are linked to a physical mechanism of changing sea-ice cover, ocean convection and overturning in high northern latitudes. In the second study of this thesis (Dahl et al., under review) a new reconstruction of atmospheric CO2 for the Devonian, which is based on CO2-sensitive carbon isotope fractionation in the earliest vascular plant fossils, suggests a much earlier drop of atmo- spheric CO2 concentration than previously reconstructed, followed by nearly constant CO2 concentrations during the Middle and Late Devonian. Our simulations for the Early Devonian with identical boundary conditions as in our Devonian sensitivity study (Brugger et al., 2019), but with a low atmospheric CO2 concentration of 500 ppm, show no direct conflict with available proxy and paleobotanical data and confirm that under the simulated climatic conditions carbon isotope fractionation represents a robust proxy for atmospheric CO2. To explain the earlier CO2 drop we suggest that early forms of vascular land plants have already strongly influenced weathering. This new perspective on the Devonian questions previous ideas about the climatic conditions and earlier explanations for the Devonian mass extinctions. The second mass extinction investigated in this thesis is the end-Cretaceous mass extinction (66 million years ago) which differs from the Devonian mass extinctions in terms of the processes involved and the timescale on which the extinctions occurred. In the two studies presented here (Brugger et al., 2017, 2021), we model the climatic effects of the Chicxulub impact, one of the proposed causes of the end-Cretaceous extinction, for the first millennium after the impact. The light-dimming effect of stratospheric sulfate aerosols causes severe cooling, with a decrease of global annual mean surface air temperature of at least 26◦C and a recovery to pre-impact temperatures after more than 30 years. The sudden surface cooling of the ocean induces deep convection which brings nutrients from the deep ocean via upwelling to the surface ocean. Using an ocean biogeochemistry model we explore the combined effect of ocean mixing and iron-rich dust originating from the impactor on the marine biosphere. As soon as light levels have recovered, we find a short, but prominent peak in marine net primary productivity. This newly discovered mechanism could result in toxic effects for marine near-surface ecosystems. Comparison of our model results to proxy data (Vellekoop et al., 2014, 2016, Hull et al., 2020) suggests that carbon release from the terrestrial biosphere is required in addition to the carbon dioxide which can be attributed to the target material. Surface ocean acidification caused by the addition of carbon dioxide and sulfur is only moderate. Taken together, the results indicate a significant contribution of the Chicxulub impact to the end-Cretaceous mass extinction by triggering multiple stressors for the Earth system. Although the sixth extinction we face today is characterized by human intervention in nature, this thesis shows that we can gain many insights into future extinctions from studying past mass extinctions, such as the importance of the rate of change (Rothman, 2017), the interplay of multiple stressors (Gunderson et al., 2016), and changes in the carbon cycle (Rothman, 2017, Tierney et al., 2020). N2 - In den 4,6 Milliarden Jahren Erdgeschichte wurde die Entwicklung des Lebens durch Störungen unterschiedlichster Art geprägt (Raup, 1994, Alroy, 2008). Ein Beispiel für solche Störungen sind Massenaussterben. Diese sind durch einen außergewöhnlichen Anstieg der Aussterberate einer großen Anzahl von Taxa in einem kurzen geologischen Zeitintervall gekennzeichnet (Sepkoski, 1986). Während der 541 Millionen Jahre des Phanerozoikums traten fünf außergewöhnlich schwere Massenaussterben auf. Viele Massenaussterben stehen mit Klimaveränderungen im Zusammenhang (Feulner, 2009). Die Untersuchung vergangener Massenaussterben ist daher nicht nur faszinierend, sondern gibt auch Einblicke in die komplexen Prozesse des Erdsystems. Diese Dissertation möchte unser Verständnis für die Auslöser von Massenaussterben sowie deren Auswirkungen auf das Leben erweitern. Dazu untersuche ich die Klimaveränderungen während zwei der fünf großen Aussterbeereignisse mit Hilfe eines gekoppelten Klimamodells. Während des Devons (vor 419,2-358,9 Millionen Jahren) entwickelten sich die ersten Gefäßpflanzen und Wirbeltiere an Land, während im Ozean Massenaussterben statt- fanden (Algeo et al., 1995). Die Ursachen dieser tiefgreifenden Veränderungen, ihre Wechselwirkungen und ihre Zusammenhänge mit Klimaveränderungen sind noch wenig verstanden. Daher untersuchen wir die Sensitivität des Klimas des Devons bezüglich verschiedener Randbedingungen mit einem Klimamodell mittlerer Komplexität (Brugger et al., 2019). Im Gegensatz zu Le Hir et al. (2011), die unrealistisch hohe Albedo Werte für den Boden verwenden, finden wir nur einen geringen biogeophysikalischen Einfluss von Änderungen der Vegetationsbedeckung. Außerdem können unsere Simulationen den starken Einfluss von Orbitalparametern, der mit einem Klimamodell mit stark vereinfachtem Ozeanmodell (De Vleeschouwer et al., 2013, 2014, 2017) simuliert wurde, nicht reproduzieren. Die in Proxydaten gefundenen klimatischen Veränderungen im Devon können wir nur durch eine Verringerung des atmosphärischen CO2 simulieren. Dennoch bleibt es eine Herausforderung, eine Übereinstimmung zwischen der aus Proxydaten (Joachimski et al., 2009) rekonstruierten Entwicklung der Meeresoberflächentemperatu- ren und unseren Simulationen zu finden. Dies deutet auf ein niedrigeres δ18O-Verhältnis des Meerwassers im Devon hin. Außerdem finden wir im Rahmen unserer Sensitivitäts- studien eine Klimavariabilität auf einer Zeitskala von Jahrzehnten bis Jahrhunderten. Die quasi-periodischen Schwankungen der Ozeantemperatur werden durch einen physikalischen Mechanismus aus sich verändernder Meereisbedeckung, Konvektion und Umwälzbewegung in den hohen nördlichen Breiten des Ozeans angetrieben. In der zweiten Studie dieser Dissertation (Dahl et al., under review) präsentieren wir eine neue Rekonstruktion des atmosphärischen CO2 für das Devon, die auf CO2-sensitiver Kohlenstoffisotopenfraktionierung in den frühesten Gefäßpflanzenfossilien basiert. Diese zeigt einen viel früheren Abfall der atmosphärischen CO2-Konzentration als bisherige Rekonstruktionen, gefolgt von nahezu konstanten CO2-Konzentrationen während des Mittel- und Spätdevon. Unsere Simulationen für das frühe Devon mit identischen Rand- bedingungen wie in unserer Sensitivitätsstudie (Brugger et al., 2019), jedoch mit einer niedrigen atmosphärischen CO2-Konzentration von 500ppm, zeigen keinen direkten Konflikt mit verfügbaren Proxy- und paläobotanischen Daten. Zusätzlich bestätigen die Simulationen, dass unter den simulierten klimatischen Bedingungen die Kohlenstoff- Isotopenfraktionierung einen robusten Proxy für atmosphärisches CO2 darstellt. Um den früheren CO2-Abfall zu erklären, schlagen wir vor, dass frühe Formen von vaskulären Landpflanzen die Verwitterung bereits stark beeinflusst haben. Diese neue Sichtweise auf das Devon stellt bisherige Vorstellungen über die klimatischen Bedingungen und frühere Erklärungen für die devonischen Massenaussterben in Frage. Das zweite in dieser Arbeit untersuchte Massenaussterben ist das Massenaussterben der späten Kreidezeit (vor 66 Millionen Jahren), das sich von denen im Devon in Bezug auf die beteiligten Prozesse und die Zeitskala der Aussterben unterscheidet. Eine der diskutierten Ursachen dieses Massenaussterbens ist der Chicxulub-Meteoriten-Einschlag. In den beiden hier vorgestellten Studien (Brugger et al., 2017, 2021) modellieren wir die klimatischen Auswirkungen des Chicxulub Einschlags für das erste Jahrtausend nach dem Einschlag. Die durch die stratosphärischen Sulfataerosole verringerte Son- neneinstrahlung verursacht eine starke Abkühlung: die global und jährlich gemittelte Oberflächenlufttemperatur nimmt um mindestens 26◦C ab und erholt sich erst nach mehr als 30 Jahren. Die plötzliche Abkühlung der Ozeanoberfläche löst bis in große Tiefen reichende Konvektion aus, die zum Nährstofftransport aus dem tiefen Ozean an die Ozea- noberfläche führt. Mit Hilfe eines biogeochemischen Modells des Ozeans untersuchen wir die kombinierte Wirkung dieser Durchmischung des Ozeans und eisenreichen Staubs aus dem Meteoriten auf die marine Biosphäre. Sobald wieder genügend Sonneneinstrahlung auf die Erdoberfläche trifft, erreicht die marine Nettoprimärproduktion ein kurzes, aber markantes Maximum. Dieser neu entdeckte Mechanismus könnte toxische Folgen für oberflächennahe Ökosysteme des Ozeans haben. Der Vergleich unserer Modellergebnisse mit Proxydaten (Vellekoop et al., 2014, 2016, Hull et al., 2020) deutet darauf hin, dass zusätzlich zum CO2 aus dem Gestein des Einschlagortes Kohlenstoff aus der terrest- rischen Biosphäre freigesetzt wird. Die Versauerung des Oberflächenozeans durch die Zugabe von CO2 und Schwefel ist nur moderat. Insgesamt deuten die Ergebnisse darauf hin, dass der Chicxulub Einschlag einen wesentlichen Beitrag zum Massenaussterben der späten Kreidezeit leistete, indem er das Erdsystem multiplen Stressoren aussetzte. Auch wenn das heutige sechste Aussterben durch menschliche Eingriffe in die Natur geprägt ist, zeigt diese Dissertation, dass wir aus dem Studium vergangener Massenaussterben viele Erkenntnisse über zukünftige Massenaussterben gewinnen können, wie z. B. die Bedeutung der Änderungsrate (Rothman, 2017), ein besseres Verständnis des Zusammenspiels multipler Stressoren (Gunderson et al., 2016) und die Rolle von Veränderungen im Kohlenstoffkreislauf (Rothman, 2017, Tierney et al., 2020). KW - earth system modeling KW - mass extinctions KW - paleoclimatology KW - climate change KW - Erdsystem Modellierung KW - Klimawandel KW - Massenaussterben KW - Paleoklimatologie Y1 - 2022 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-532468 ER - TY - GEN A1 - Regenstein, Wolfgang T1 - Strahlenschutzphysik in Stichpunkten N2 - Das Manuskript dient der Vorbereitung der Prüfung der Fachkunde zum Strahlenschutz für Lehrer. Es enthält wichtige Grundlagen der Kernphysik, insbesondere die Eigenschaften der Alpha-, Beta-, Gamma-, Neutronen- und Röntgenstrahlen. Es folgt eine kurze Beschreibung des Einflusses der Strahlung auf belebte Materie. Wichtige Paragrafen der Strahlenschutzverordnung werden beschrieben. Eine Aufgabensammlung dient zur Illustration und Übung. N2 - The paper serves for preparation to the examination to the „Fachkunde zum Stahlenschutz für Lehrer“. It contains important basics of the nuclear physics, especially the quantities of alpha-, beta-, gamma- und neutron radiation. It follows a description of the influence the radiation on lively matter. Important articles oft the „Strahlenschutzverordnung“ are described. A collection of exercises serves to illustration and practice. KW - Strahlenschutz KW - Strahlenarten KW - Dosimetrie KW - Strahlenbiologie KW - Strahlenbelastung KW - Radiation protection KW - kind of radiation KW - dosis measurement KW - radiobiology KW - radiation load Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-513405 ER - TY - THES A1 - Antonelli, Andrea T1 - Accurate waveform models for gravitational-wave astrophysics: synergetic approaches from analytical relativity N2 - Gravitational-wave (GW) astrophysics is a field in full blossom. Since the landmark detection of GWs from a binary black hole on September 14th 2015, fifty-two compact-object binaries have been reported by the LIGO-Virgo collaboration. Such events carry astrophysical and cosmological information ranging from an understanding of how black holes and neutron stars are formed, what neutron stars are composed of, how the Universe expands, and allow testing general relativity in the highly-dynamical strong-field regime. It is the goal of GW astrophysics to extract such information as accurately as possible. Yet, this is only possible if the tools and technology used to detect and analyze GWs are advanced enough. A key aspect of GW searches are waveform models, which encapsulate our best predictions for the gravitational radiation under a certain set of parameters, and that need to be cross-correlated with data to extract GW signals. Waveforms must be very accurate to avoid missing important physics in the data, which might be the key to answer the fundamental questions of GW astrophysics. The continuous improvements of the current LIGO-Virgo detectors, the development of next-generation ground-based detectors such as the Einstein Telescope or the Cosmic Explorer, as well as the development of the Laser Interferometer Space Antenna (LISA), demand accurate waveform models. While available models are enough to capture the low spins, comparable-mass binaries routinely detected in LIGO-Virgo searches, those for sources from both current and next-generation ground-based and spaceborne detectors must be accurate enough to detect binaries with large spins and asymmetry in the masses. Moreover, the thousands of sources that we expect to detect with future detectors demand accurate waveforms to mitigate biases in the estimation of signals’ parameters due to the presence of a foreground of many sources that overlap in the frequency band. This is recognized as one of the biggest challenges for the analysis of future-detectors’ data, since biases might hinder the extraction of important astrophysical and cosmological information from future detectors’ data. In the first part of this thesis, we discuss how to improve waveform models for binaries with high spins and asymmetry in the masses. In the second, we present the first generic metrics that have been proposed to predict biases in the presence of a foreground of many overlapping signals in GW data. For the first task, we will focus on several classes of analytical techniques. Current models for LIGO and Virgo studies are based on the post-Newtonian (PN, weak-field, small velocities) approximation that is most natural for the bound orbits that are routinely detected in GW searches. However, two other approximations have risen in prominence, the post-Minkowskian (PM, weak- field only) approximation natural for unbound (scattering) orbits and the small-mass-ratio (SMR) approximation typical of binaries in which the mass of one body is much bigger than the other. These are most appropriate to binaries with high asymmetry in the masses that challenge current waveform models. Moreover, they allow one to “cover” regions of the parameter space of coalescing binaries, thereby improving the interpolation (and faithfulness) of waveform models. The analytical approximations to the relativistic two-body problem can synergically be included within the effective-one-body (EOB) formalism, in which the two-body information from each approximation can be recast into an effective problem of a mass orbiting a deformed Schwarzschild (or Kerr) black hole. The hope is that the resultant models can cover both the low-spin comparable-mass binaries that are routinely detected, and the ones that challenge current models. The first part of this thesis is dedicated to a study about how to best incorporate information from the PN, PM, SMR and EOB approaches in a synergistic way. We also discuss how accurate the resulting waveforms are, as compared against numerical-relativity (NR) simulations. We begin by comparing PM models, whether alone or recast in the EOB framework, against PN models and NR simulations. We will show that PM information has the potential to improve currently-employed models for LIGO and Virgo, especially if recast within the EOB formalism. This is very important, as the PM approximation comes with a host of new computational techniques from particle physics to exploit. Then, we show how a combination of PM and SMR approximations can be employed to access previously-unknown PN orders, deriving the third subleading PN dynamics for spin-orbit and (aligned) spin1-spin2 couplings. Such new results can then be included in the EOB models currently used in GW searches and parameter estimation studies, thereby improving them when the binaries have high spins. Finally, we build an EOB model for quasi-circular nonspinning binaries based on the SMR approximation (rather than the PN one as usually done). We show how this is done in detail without incurring in the divergences that had affected previous attempts, and compare the resultant model against NR simulations. We find that the SMR approximation is an excellent approximation for all (quasi-circular nonspinning) binaries, including both the equal-mass binaries that are routinely detected in GW searches and the ones with highly asymmetric masses. In particular, the SMR-based models compare much better than the PN models, suggesting that SMR-informed EOB models might be the key to model binaries in the future. In the second task of this thesis, we work within the linear-signal ap- proximation and describe generic metrics to predict inference biases on the parameters of a GW source of interest in the presence of confusion noise from unfitted foregrounds and from residuals of other signals that have been incorrectly fitted out. We illustrate the formalism with simple (yet realistic) LISA sources, and demonstrate its validity against Monte-Carlo simulations. The metrics we describe pave the way for more realistic studies to quantify the biases with future ground-based and spaceborne detectors. N2 - Wenn zwei kompakte Objekte wie Schwarze Löcher oder Neutronensterne kollidieren, wird der Raum und die Zeit um sie herum stark gekrümmt. Der effekt sind Störungen der Raumzeit, sogenannte Gravitationswellen, die sich im gesamten Universum ausbreiten. Mit den leistungsstarken und präzisen Netzwerken von Detektoren und der Arbeit vieler Wissenschaftler rund um den Globus kann man Gravitationswellen auf der Erde messen. Gravitationswellen tragen Informationen über das System, das sie erzeugt hat. Insbesondere kann man erfahren, wie sich die kompakten Objekte gebildet haben und woraus sie bestehen. Daraus lässt sich ableiten, wie sich das Universum ausdehnt, und man kann die Allgemeine Relativitätstheorie in Regionen mit starker Gravitation testen. Um diese Informationen zu extrahieren, werden genaue Modelle benötigt. Modelle können entweder numerisch durch Lösen der berühmten Einstein-Gleichungen oder analytisch durch Annäherung an deren Lösungen gewonnen werden. In meiner Arbeit haben wir den zweiten Ansatz verfolgt, um sehr genaue Vorhersagen für die Signale zu erhalten, die bei kommenden Beobachtungen durch Gravitationswellendetektoren verwendet werden können. KW - gravitational waves KW - Gravitationswellen KW - general relativity KW - allgemeine Relativitätstheorie KW - data analysis KW - Datenanalyse Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-576671 ER - TY - JOUR A1 - Wiesner, Karoline A1 - Ladyman, James T1 - Complex systems are always correlated but rarely information processing JF - Journal of physics. Complexity N2 - 'Complex systems are information processors' is a statement that is frequently made. Here we argue for the distinction between information processing-in the sense of encoding and transmitting a symbolic representation-and the formation of correlations (pattern formation/self-organisation). The study of both uses tools from information theory, but the purpose is very different in each case: explaining the mechanisms and understanding the purpose or function in the first case, versus data analysis and correlation extraction in the latter. We give examples of both and discuss some open questions. The distinction helps focus research efforts on the relevant questions in each case. KW - correlations KW - information theory KW - complex systems KW - information KW - processing KW - self-organisation Y1 - 2021 U6 - https://doi.org/10.1088/2632-072X/ac371c SN - 2632-072X VL - 2 IS - 4 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Diercke, Andrea A1 - Kuckein, Christoph A1 - Verma, Meetu A1 - Denker, Carsten T1 - Filigree in the surroundings of polar crown and high-latitude filaments JF - Solar physics : a journal for solar and solar-stellar research and the study of solar terrestrial physics N2 - High-resolution observations of polar crown and high-latitude filaments are scarce. We present a unique sample of such filaments observed in high-resolution H alpha narrow-band filtergrams and broad-band images, which were obtained with a new fast camera system at the Vacuum Tower Telescope (VTT), Tenerife, Spain. The Chromospheric Telescope (ChroTel) provided full-disk context observations in H alpha, CaiiK, and Hei 10830 angstrom. The Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) provided line-of-sight magnetograms and ultraviolet (UV) 1700 angstrom filtergrams, respectively. We study filigree in the vicinity of polar crown and high-latitude filaments and relate their locations to magnetic concentrations at the filaments' footpoints. Bright points are a well studied phenomenon in the photosphere at low latitudes, but they were not yet studied in the quiet network close to the poles. We examine size, area, and eccentricity of bright points and find that their morphology is very similar to their counterparts at lower latitudes, but their sizes and areas are larger. Bright points at the footpoints of polar crown filaments are preferentially located at stronger magnetic flux concentrations, which are related to bright regions at the border of supergranules as observed in UV filtergrams. Examining the evolution of bright points on three consecutive days reveals that their amount increases while the filament decays, which indicates they impact the equilibrium of the cool plasma contained in filaments. KW - Chromosphere KW - Quiet KW - Granulation KW - Magnetic fields KW - Photosphere KW - Prominences KW - Quiescent Y1 - 2021 U6 - https://doi.org/10.1007/s11207-021-01776-7 SN - 0038-0938 SN - 1573-093X VL - 296 IS - 2 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Keles, Engin A1 - Mallom, Matthias A1 - von Essen, Carolina A1 - Caroll, Thorsten A. A1 - Alexoudi, Xanthippi A1 - Pino, Lorenzo A1 - Ilyin, Ilya A1 - Poppenhäger, Katja A1 - Kitzmann, Daniel A1 - Nascimbeni, Valerino A1 - Turner, Jake D. A1 - Strassmeier, Klaus G. T1 - The potassium absorption on HD189733b and HD209458b JF - Monthly Notices of the Royal Astronomical Society: Letters N2 - In this work, we investigate the potassium excess absorption around 7699 Å of the exoplanets HD189733b and HD209458b. For this purpose, we used high-spectral resolution transit observations acquired with the 2 × 8.4 m Large Binocular Telescope (LBT) and the Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI). For a bandwidth of 0.8 Å, we present a detection >7σ with an absorption level of 0.18 per cent for HD189733b. Applying the same analysis to HD209458b, we can set 3σ upper limit of 0.09 per cent, even though we do not detect a K-excess absorption. The investigation suggests that the K feature is less present in the atmosphere of HD209458b than in the one of HD189733b. This comparison confirms previous claims that the atmospheres of these two planets must have fundamentally different properties. Y1 - 2021 U6 - https://doi.org/10.1093/mnrasl/slz123 VL - 489 IS - 1 SP - L37 EP - L41 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Guggenberger, Tobias A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Fractional Brownian motion in superharmonic potentials and non-Boltzmann stationary distributions JF - Journal of physics : A, Mathematical and theoretical N2 - We study the stochastic motion of particles driven by long-range correlated fractional Gaussian noise (FGN) in a superharmonic external potential of the form U(x) proportional to x(2n) (n is an element of N). When the noise is considered to be external, the resulting overdamped motion is described by the non-Markovian Langevin equation for fractional Brownian motion. For this case we show the existence of long time, stationary probability density functions (PDFs) the shape of which strongly deviates from the naively expected Boltzmann PDF in the confining potential U(x). We analyse in detail the temporal approach to stationarity as well as the shape of the non-Boltzmann stationary PDF. A typical characteristic is that subdiffusive, antipersistent (with negative autocorrelation) motion tends to effect an accumulation of probability close to the origin as compared to the corresponding Boltzmann distribution while the opposite trend occurs for superdiffusive (persistent) motion. For this latter case this leads to distinct bimodal shapes of the PDF. This property is compared to a similar phenomenon observed for Markovian Levy flights in superharmonic potentials. We also demonstrate that the motion encoded in the fractional Langevin equation driven by FGN always relaxes to the Boltzmann distribution, as in this case the fluctuation-dissipation theorem is fulfilled. KW - anomalous diffusion KW - Boltzmann distribution KW - non-Gaussian distribution Y1 - 2021 U6 - https://doi.org/10.1088/1751-8121/ac019b SN - 1751-8113 SN - 1751-8121 VL - 54 IS - 29 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Kumar, Mohit A1 - Rosenblum, Michael T1 - Two mechanisms of remote synchronization in a chain of Stuart-Landau oscillators JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - Remote synchronization implies that oscillators interacting not directly but via an additional unit (hub) adjust their frequencies and exhibit frequency locking while the hub remains asynchronous. In this paper, we analyze the mechanisms of remote synchrony in a small network of three coupled Stuart-Landau oscillators using recent results on higher-order phase reduction. We analytically demonstrate the role of two factors promoting remote synchrony. These factors are the nonisochronicity of oscillators and the coupling terms appearing in the secondorder phase approximation. We show a good correspondence between our theory and numerical results for small and moderate coupling strengths. Y1 - 2021 U6 - https://doi.org/10.1103/PhysRevE.104.054202 SN - 2470-0045 SN - 2470-0053 VL - 104 IS - 5 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Hannemann, Mandy A1 - Wegner, Gino A1 - Henkel, Carsten T1 - No-slip boundary conditions for electron hydrodynamics and the thermal Casimir pressure JF - Universe : open access journal N2 - We derive modified reflection coefficients for electromagnetic waves in the THz and far infrared range. The idea is based on hydrodynamic boundary conditions for metallic conduction electrons. The temperature-dependent part of the Casimir pressure between metal plates is evaluated. The results should shed light on the "thermal anomaly," where measurements deviate from the standard fluctuation electrodynamics for conducting metals. KW - dispersion force KW - metal optics KW - Drude model KW - hydrodynamic model KW - spatial KW - dispersion KW - viscosity KW - non-contact heat transfer Y1 - 2021 U6 - https://doi.org/10.3390/universe7040108 SN - 2218-1997 VL - 7 IS - 4 PB - MDPI CY - Basel ER - TY - JOUR A1 - Mutothya, Nicholas Mwilu A1 - Xu, Yong A1 - Li, Yongge A1 - Metzler, Ralf T1 - Characterising stochastic motion in heterogeneous media driven by coloured non-Gaussian noise JF - Journal of physics : A, Mathematical and theoretical N2 - We study the stochastic motion of a test particle in a heterogeneous medium in terms of a position dependent diffusion coefficient mimicking measured deterministic diffusivity gradients in biological cells or the inherent heterogeneity of geophysical systems. Compared to previous studies we here investigate the effect of the interplay of anomalous diffusion effected by position dependent diffusion coefficients and coloured non-Gaussian noise. The latter is chosen to be distributed according to Tsallis' q-distribution, representing a popular example for a non-extensive statistic. We obtain the ensemble and time averaged mean squared displacements for this generalised process and establish its non-ergodic properties as well as analyse the non-Gaussian nature of the associated displacement distribution. We consider both non-stratified and stratified environments. KW - diffusion KW - anomalous diffusion KW - non-extensive statistics KW - coloured KW - noise KW - heterogeneous diffusion process Y1 - 2021 U6 - https://doi.org/10.1088/1751-8121/abfba6 SN - 1751-8113 SN - 1751-8121 VL - 54 IS - 29 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Henkel, Carsten T1 - Heat transfer and entanglement BT - non-equilibrium correlation spectra of two quantum oscillators JF - Annalen der Physik N2 - The non-equilibrium state of two oscillators with a mutual interaction and coupled to separate heat baths is discussed. Bosonic baths are considered, and an exact spectral representation for the elements of the covariance matrix is provided analytically. A wide class of spectral densities for the relevant bath modes is allowed for. The validity of the fluctuation-dissipation relation is established for global equilibrium (both baths at the same temperature) in the stationary state. Spectral measures of entanglement are suggested by comparing to the equilibrium spectrum of zero-point fluctuations. No rotating-wave approximation is applied, and anomalous heat transport from cold to hot bath, as reported in earlier work, is demonstrated not to occur. KW - entanglement KW - heat transfer KW - non-equilibrium steady state KW - master KW - equation KW - quantum thermodynamics Y1 - 2021 U6 - https://doi.org/10.1002/andp.202100089 SN - 0003-3804 SN - 1521-3889 VL - 533 IS - 10 PB - Wiley-VCH CY - Weinheim ER -