@phdthesis{Wiedmer2004, author = {Wiedmer, Petra}, title = {Geschlechtsspezifische K{\"o}rpergewichtsregulation bei M{\"a}usen :Untersuchungen zur Set-point-Theorie der K{\"o}rpermasse}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-0001733}, school = {Universit{\"a}t Potsdam}, year = {2004}, abstract = {Entsprechend der sogenannten Set-point-Theorie besitzt jeder Mensch eine individuell festgelegte K{\"o}rpermasse, die {\"u}ber große Zeitr{\"a}ume konstant gehalten und gegen Abweichungen verteidigt wird. Es wird angenommen, dass der K{\"o}rper auf noch unbekannte Weise {\"A}nderungen in der K{\"o}rpermasse per se wahrnimmt und daraufhin Mechanismen aktiviert, die zur Regenerierung der urspr{\"u}nglichen Masse f{\"u}hren. In dieser Arbeit wurde die Hypothese getestet, dass eine k{\"u}nstliche Erh{\"o}hung der K{\"o}rpermasse zu einer kompensatorischen Reduktion in der K{\"o}rpermasse f{\"u}hrt, um das Ausgangsgewicht wieder zu regenerieren. Die K{\"o}rpermasse von m{\"a}nnlichen und weiblichen M{\"a}usen wurde akut durch die Implantation von Gewichten mit einer Masse von 10\% der aktuellen K{\"o}rpermasse in die Bauchh{\"o}hle erh{\"o}ht. Bei G{\"u}ltigkeit der Set-point-Theorie sollte die K{\"o}rpermassereduktion der Masse des zus{\"a}tzlichen Gewichtsimplantats entsprechen. Die M{\"a}use reagierten auf die k{\"u}nstlich erh{\"o}hte K{\"o}rpermasse geschlechtsspezifisch. M{\"a}nnchen zeigten eine partielle Reduktion in der K{\"o}rpermasse. Weibchen zeigten langfristig jedoch keine {\"A}nderungen in der K{\"o}rpermasse. Die Reduktion der K{\"o}rpermasse erfolgte bei den M{\"a}nnchen durch eine Abnahme in der Fettmasse. Die fettfreie Masse war in beiden Geschlechtern nicht ver{\"a}ndert. {\"A}nderungen in der K{\"o}rpermasse wurden vor allem durch {\"A}nderungen in der Energieaufnahme hervorgerufen. Ein Einfluss des Energieumsatzes auf {\"A}nderungen in der K{\"o}rpermasse konnte nicht nachgewiesen werden. Die Regulation der K{\"o}rpermasse entsprechend eines massespezifischen Set-points konnte partiell f{\"u}r die M{\"a}nnchen gezeigt werden. Bei den M{\"a}nnchen k{\"o}nnte daher die Wahrnehmung der K{\"o}rpermasse in die Regulation der K{\"o}rpermasse teilweise integriert sein. Weibchen verminderten ihre K{\"o}rpermasse dagegen trotz der k{\"u}nstlichen K{\"o}rpermasseerh{\"o}hung nicht. Das f{\"u}hrte zur Bewahrung der Energiereserven und spricht eher f{\"u}r die Regulation der K{\"o}rpermasse entsprechend des notwendigen Energiebedarfs im Vergleich zu {\"A}nderungen in der K{\"o}rpermasse per se. Diese Ergebnisse zeigen, dass die Regulation der K{\"o}rpermasse geschlechtsspezifischen Mechanismen unterliegt. Dementsprechend sind auch geschlechtsspezifische Ans{\"a}tze zur Therapie von {\"U}bergewicht und Adipositas notwendig.}, language = {de} } @phdthesis{Werth2010, author = {Werth, Susanna}, title = {Calibration of the global hydrological model WGHM with water mass variations from GRACE gravity data}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-41738}, school = {Universit{\"a}t Potsdam}, year = {2010}, abstract = {Since the start-up of the GRACE (Gravity Recovery And Climate Experiment) mission in 2002 time dependent global maps of the Earth's gravity field are available to study geophysical and climatologically-driven mass redistributions on the Earth's surface. In particular, GRACE observations of total water storage changes (TWSV) provide a comprehensive data set for analysing the water cycle on large scales. Therefore they are invaluable for validation and calibration of large-scale hydrological models as the WaterGAP Global Hydrology Model (WGHM) which simulates the continental water cycle including its most important components, such as soil, snow, canopy, surface- and groundwater. Hitherto, WGHM exhibits significant differences to GRACE, especially for the seasonal amplitude of TWSV. The need for a validation of hydrological models is further highlighted by large differences between several global models, e.g. WGHM, the Global Land Data Assimilation System (GLDAS) and the Land Dynamics model (LaD). For this purpose, GRACE links geodetic and hydrological research aspects. This link demands the development of adequate data integration methods on both sides, forming the main objectives of this work. They include the derivation of accurate GRACE-based water storage changes, the development of strategies to integrate GRACE data into a global hydrological model as well as a calibration method, followed by the re-calibration of WGHM in order to analyse process and model responses. To achieve these aims, GRACE filter tools for the derivation of regionally averaged TWSV were evaluated for specific river basins. Here, a decorrelation filter using GRACE orbits for its design is most efficient among the tested methods. Consistency in data and equal spatial resolution between observed and simulated TWSV were realised by the inclusion of all most important hydrological processes and an equal filtering of both data sets. Appropriate calibration parameters were derived by a WGHM sensitivity analysis against TWSV. Finally, a multi-objective calibration framework was developed to constrain model predictions by both river discharge and GRACE TWSV, realised with a respective evolutionary method, the ε-Non-dominated-Sorting-Genetic-Algorithm-II (ε-NSGAII). Model calibration was done for the 28 largest river basins worldwide and for most of them improved simulation results were achieved with regard to both objectives. From the multi-objective approach more reliable and consistent simulations of TWSV within the continental water cycle were gained and possible model structure errors or mis-modelled processes for specific river basins detected. For tropical regions as such, the seasonal amplitude of water mass variations has increased. The findings lead to an improved understanding of hydrological processes and their representation in the global model. Finally, the robustness of the results is analysed with respect to GRACE and runoff measurement errors. As a main conclusion obtained from the results, not only soil water and snow storage but also groundwater and surface water storage have to be included in the comparison of the modelled and GRACE-derived total water budged data. Regarding model calibration, the regional varying distribution of parameter sensitivity suggests to tune only parameter of important processes within each region. Furthermore, observations of single storage components beside runoff are necessary to improve signal amplitudes and timing of simulated TWSV as well as to evaluate them with higher accuracy. The results of this work highlight the valuable nature of GRACE data when merged into large-scale hydrological modelling and depict methods to improve large-scale hydrological models.}, language = {en} } @misc{RaetzelWilkensMenzel2016, author = {R{\"a}tzel, Dennis and Wilkens, Martin and Menzel, Ralf}, title = {Gravitational properties of light}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-90553}, year = {2016}, abstract = {The gravitational field of a laser pulse of finite lifetime, is investigated in the framework of linearized gravity. Although the effects are very small, they may be of fundamental physical interest. It is shown that the gravitational field of a linearly polarized light pulse is modulated as the norm of the corresponding electric field strength, while no modulations arise for circular polarization. In general, the gravitational field is independent of the polarization direction. It is shown that all physical effects are confined to spherical shells expanding with the speed of light, and that these shells are imprints of the spacetime events representing emission and absorption of the pulse. Nearby test particles at rest are attracted towards the pulse trajectory by the gravitational field due to the emission of the pulse, and they are repelled from the pulse trajectory by the gravitational field due to its absorption. Examples are given for the size of the attractive effect. It is recovered that massless test particles do not experience any physical effect if they are co-propagating with the pulse, and that the acceleration of massless test particles counter-propagating with respect to the pulse is four times stronger than for massive particles at rest. The similarities between the gravitational effect of a laser pulse and Newtonian gravity in two dimensions are pointed out. The spacetime curvature close to the pulse is compared to that induced by gravitational waves from astronomical sources.}, language = {en} } @article{RaetzelWilkensMenzel2016, author = {R{\"a}tzel, Dennis and Wilkens, Martin and Menzel, Ralf}, title = {Gravitational properties of light}, series = {New journal of physics : the open-access journal for physics}, volume = {18}, journal = {New journal of physics : the open-access journal for physics}, publisher = {IOP Science}, address = {London}, issn = {1367-2630}, doi = {10.1088/1367-2630/18/2/023009}, pages = {1 -- 16}, year = {2016}, abstract = {The gravitational field of a laser pulse of finite lifetime, is investigated in the framework of linearized gravity. Although the effects are very small, they may be of fundamental physical interest. It is shown that the gravitational field of a linearly polarized light pulse is modulated as the norm of the corresponding electric field strength, while no modulations arise for circular polarization. In general, the gravitational field is independent of the polarization direction. It is shown that all physical effects are confined to spherical shells expanding with the speed of light, and that these shells are imprints of the spacetime events representing emission and absorption of the pulse. Nearby test particles at rest are attracted towards the pulse trajectory by the gravitational field due to the emission of the pulse, and they are repelled from the pulse trajectory by the gravitational field due to its absorption. Examples are given for the size of the attractive effect. It is recovered that massless test particles do not experience any physical effect if they are co-propagating with the pulse, and that the acceleration of massless test particles counter-propagating with respect to the pulse is four times stronger than for massive particles at rest. The similarities between the gravitational effect of a laser pulse and Newtonian gravity in two dimensions are pointed out. The spacetime curvature close to the pulse is compared to that induced by gravitational waves from astronomical sources.}, language = {en} } @article{RaetzelWilkensMenzel2016, author = {R{\"a}tzel, Dennis and Wilkens, Martin and Menzel, Ralf}, title = {Gravitational properties of light-the gravitational field of a laser pulse}, series = {NEW JOURNAL OF PHYSICS}, volume = {18}, journal = {NEW JOURNAL OF PHYSICS}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {1367-2630}, doi = {10.1088/1367-2630/18/2/023009}, pages = {16}, year = {2016}, abstract = {The gravitational field of a laser pulse of finite lifetime, is investigated in the framework of linearized gravity. Although the effects are very small, they may be of fundamental physical interest. It is shown that the gravitational field of a linearly polarized light pulse is modulated as the norm of the corresponding electric field strength, while no modulations arise for circular polarization. In general, the gravitational field is independent of the polarization direction. It is shown that all physical effects are confined to spherical shells expanding with the speed of light, and that these shells are imprints of the spacetime events representing emission and absorption of the pulse. Nearby test particles at rest are attracted towards the pulse trajectory by the gravitational field due to the emission of the pulse, and they are repelled from the pulse trajectory by the gravitational field due to its absorption. Examples are given for the size of the attractive effect. It is recovered that massless test particles do not experience any physical effect if they are co-propagating with the pulse, and that the acceleration of massless test particles counter-propagating with respect to the pulse is four times stronger than for massive particles at rest. The similarities between the gravitational effect of a laser pulse and Newtonian gravity in two dimensions are pointed out. The spacetime curvature close to the pulse is compared to that induced by gravitational waves from astronomical sources.}, language = {en} } @misc{RubeyBruneHeineetal.2017, author = {Rubey, Michael and Brune, Sascha and Heine, Christian and Davies, D. Rhodri and Williams, Simon E. and M{\"u}ller, R. Dietmar}, title = {Global patterns in Earth's dynamic topography since the Jurassic}, series = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, journal = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, number = {623}, issn = {1866-8372}, doi = {10.25932/publishup-41824}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-418241}, pages = {899 -- 919}, year = {2017}, abstract = {We evaluate the spatial and temporal evolution of Earth's long-wavelength surface dynamic topography since the Jurassic using a series of high-resolution global mantle convection models. These models are Earth-like in terms of convective vigour, thermal structure, surface heat-flux and the geographic distribution of heterogeneity. The models generate a degree-2-dominated spectrum of dynamic topography with negative amplitudes above subducted slabs (i.e. circum-Pacific regions and southern Eurasia) and positive amplitudes elsewhere (i.e. Africa, north-western Eurasia and the central Pacific). Model predictions are compared with published observations and subsidence patterns from well data, both globally and for the Australian and southern African regions. We find that our models reproduce the long-wavelength component of these observations, although observed smaller-scale variations are not reproduced. We subsequently define "geodynamic rules" for how different surface tectonic settings are affected by mantle processes: (i) locations in the vicinity of a subduction zone show large negative dynamic topography amplitudes; (ii) regions far away from convergent margins feature long-term positive dynamic topography; and (iii) rapid variations in dynamic support occur along the margins of overriding plates (e.g. the western US) and at points located on a plate that rapidly approaches a subduction zone (e.g. India and the Arabia Peninsula). Our models provide a predictive quantitative framework linking mantle convection with plate tectonics and sedimentary basin evolution, thus improving our understanding of how subduction and mantle convection affect the spatio-temporal evolution of basin architecture.}, language = {en} } @phdthesis{Kubas2005, author = {Kubas, Daniel}, title = {Applications of Galactic Microlensing}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-5179}, school = {Universit{\"a}t Potsdam}, year = {2005}, abstract = {Subject of this work is the study of applications of the Galactic Microlensing effect, where the light of a distant star (source) is bend according to Einstein's theory of gravity by the gravitational field of intervening compact mass objects (lenses), creating multiple (however not resolvable) images of the source. Relative motion of source, observer and lens leads to a variation of deflection/magnification and thus to a time dependant observable brightness change (lightcurve), a so-called microlensing event, lasting weeks to months. The focus lies on the modeling of binary-lens events, which provide a unique tool to fully characterize the lens-source system and to detect extra-solar planets around the lens star. Making use of the ability of genetic algorithms to efficiently explore large and intricate parameter spaces in the quest for the global best solution, a modeling software (Tango) for binary lenses is developed, presented and applied to data sets from the PLANET microlensing campaign. For the event OGLE-2002-BLG-069 the 2nd ever lens mass measurement has been achieved, leading to a scenario, where a G5III Bulge giant at 9.4 kpc is lensed by an M-dwarf binary with total mass of M=0.51 solar masses at distance 2.9 kpc. Furthermore a method is presented to use the absence of planetary lightcurve signatures to constrain the abundance of extra-solar planets.}, subject = {Planeten}, language = {en} }