@phdthesis{Dziourkevitch2005, author = {Dziourkevitch, Natalia}, title = {Interstellar turbulence driven by magneto-rotational instability}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-5306}, school = {Universit{\"a}t Potsdam}, year = {2005}, abstract = {Origin and symmetry of the observed global magnetic fields in galaxies are not fully understood. We intend to clarify the question of the magnetic field origin and investigate the global action of the magneto-rotational instability (MRI) in galactic disks with the help of 3D global magneto-hydrodynamical (MHD) simulations. The calculations were done with the time-stepping ZEUS 3D code using massive parallelization. The alpha-Omega dynamo is known to be one of the most efficient mechanisms to reproduce the observed global galactic fields. The presence of strong turbulence is a pre-requisite for the alpha-Omega dynamo generation of the regular magnetic fields. The observed magnitude and spatial distribution of turbulence in galaxies present unsolved problems to theoreticians. The MRI is known to be a fast and powerful mechanism to generate MHD turbulence and to amplify magnetic fields. We find that the critical wavelength increases with the increasing of magnetic fields during the simulation, transporting the energy from critical to larger scales. The final structure, if not disrupted by supernovae explosions, is the structure of `thin layers' of thickness of about 100 pcs. An important outcome of all simulations is the magnitude of the horizontal components of the Reynolds and Maxwell stresses. The result is that the MRI-driven turbulence is magnetic-dominated: its magnetic energy exceeds the kinetic energy by a factor of 4. The Reynolds stress is small and less than 1\% of the Maxwell stress. The angular momentum transport is thus completely dominated by the magnetic field fluctuations. The volume-averaged pitch angle is always negative with a magnitude of about -30. The non-saturated MRI regime is lasting sufficiently long to fill the time between the galactic encounters, independently of strength and geometry of the initial field. Therefore, we may claim the observed pitch angles can be due to MRI action in the gaseous galactic disks. The MRI is also shown to be a very fast instability with e-folding time proportional to the time of one rotation. Steep rotation curves imply a stronger growth for the magnetic energy due to MRI. The global e-folding time is from 44 Myr to 100 Myr depending on the rotation profile. Therefore, MRI can explain the existence of rather large magnetic field in very young galaxies. We also have reproduced the observed rms values of velocities in the interstellar turbulence as it was observed in NGC 1058. We have shown with the simulations that the averaged velocity dispersion of about 5 km/s is a typical number for the MRI-driven turbulence in galaxies, which agrees with observations. The dispersion increases outside of the disk plane, whereas supernovae-driven turbulence is found to be concentrated within the disk. In our simulations the velocity dispersion increases a few times with the heights. An additional support to the dynamo alpha-effect in the galaxies is the ability of the MRI to produce a mix of quadrupole and dipole symmetries from the purely vertical seed fields, so it also solves the seed-fields problem of the galactic dynamo theory. The interaction of magneto-rotational instability and random supernovae explosions remains an open question. It would be desirable to run the simulation with the supernovae explosions included. They would disrupt the calm ring structure produced by global MRI, may be even to the level when we can no longer blame MRI to be responsible for the turbulence.}, subject = {Magnetohydrodynamik}, language = {en} } @phdthesis{Gressel2008, author = {Gressel, Oliver}, title = {Supernova-driven turbulence and magnetic field amplification in disk galaxies}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-29094}, school = {Universit{\"a}t Potsdam}, year = {2008}, abstract = {Supernovae are known to be the dominant energy source for driving turbulence in the interstellar medium. Yet, their effect on magnetic field amplification in spiral galaxies is still poorly understood. Analytical models based on the uncorrelated-ensemble approach predicted that any created field will be expelled from the disk before a significant amplification can occur. By means of direct simulations of supernova-driven turbulence, we demonstrate that this is not the case. Accounting for vertical stratification and galactic differential rotation, we find an exponential amplification of the mean field on timescales of 100Myr. The self-consistent numerical verification of such a "fast dynamo" is highly beneficial in explaining the observed strong magnetic fields in young galaxies. We, furthermore, highlight the importance of rotation in the generation of helicity by showing that a similar mechanism based on Cartesian shear does not lead to a sustained amplification of the mean magnetic field. This finding impressively confirms the classical picture of a dynamo based on cyclonic turbulence.}, language = {en} } @misc{Gronau2005, author = {Gronau, Norbert}, title = {Ermittlung der Zukunftsf{\"a}higkeit unternehmensweiter Anwendungssysteme}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-6843}, year = {2005}, abstract = {Bei Entscheidungen {\"u}ber abzul{\"o}sende oder neue Anwendungssysteme kann mit Hilfe funktionaler Anforderungen immer nur der gegenw{\"a}rtige oder vorhersehbare Bedarf ermittelt werden. In einem turbulenten Umfeld sind die Anwendungssysteme jedoch h{\"a}ufig langere Zeit im Einsatz als die Anforderungen g{\"u}ltig sind, mit Hilfe derer sie ausgew{\"a}hlt wurden. An der Universit{\"a}t Potsdam wird im Rahmen des BMBF-Projektes CHANGE eine Vorgehensweise zur Ermittlung der Zukunftsf{\"a}higkeit unternehmensweiter Anwendungssysteme entwickelt, deren wesentliche Merkmale in diesem Beitrag beschrieben werden.}, subject = {Enterprise-Resource-Planning}, language = {de} } @misc{HoffmannSchulzHankeAlbaetal.2017, author = {Hoffmann, Mathias and Schulz-Hanke, Maximilian and Alba, Juana Garcia and Jurisch, Nicole and Hagemann, Ulrike and Sachs, Torsten and Sommer, Michael and Augustin, J{\"u}rgen}, title = {A simple calculation algorithm to separate high-resolution CH4 flux measurements into ebullition- and diffusion-derived components}, series = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, journal = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, number = {604}, issn = {1866-8372}, doi = {10.25932/publishup-41665}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-416659}, pages = {109 -- 118}, year = {2017}, abstract = {Processes driving the production, transformation and transport of methane (CH4) in wetland ecosystems are highly complex. We present a simple calculation algorithm to separate open-water CH4 fluxes measured with automatic chambers into diffusion- and ebullition-derived components. This helps to reveal underlying dynamics, to identify potential environmental drivers and, thus, to calculate reliable CH4 emission estimates. The flux separation is based on identification of ebullition-related sudden concentration changes during single measurements. Therefore, a variable ebullition filter is applied, using the lower and upper quartile and the interquartile range (IQR). Automation of data processing is achieved by using an established R script, adjusted for the purpose of CH4 flux calculation. The algorithm was validated by performing a laboratory experiment and tested using flux measurement data (July to September 2013) from a former fen grassland site, which converted into a shallow lake as a result of rewetting. Ebullition and diffusion contributed equally (46 and 55 \%) to total CH4 emissions, which is comparable to ratios given in the literature. Moreover, the separation algorithm revealed a concealed shift in the diurnal trend of diffusive fluxes throughout the measurement period. The water temperature gradient was identified as one of the major drivers of diffusive CH4 emissions, whereas no significant driver was found in the case of erratic CH4 ebullition events.}, language = {en} } @phdthesis{Jappsen2005, author = {Jappsen, Anne-Katharina}, title = {Present and early star formation : a study on rotational and thermal properties}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-7591}, school = {Universit{\"a}t Potsdam}, year = {2005}, abstract = {We investigate the rotational and thermal properties of star-forming molecular clouds using hydrodynamic simulations. Stars form from molecular cloud cores by gravoturbulent fragmentation. Understanding the angular momentum and the thermal evolution of cloud cores thus plays a fundamental role in completing the theoretical picture of star formation. This is true not only for current star formation as observed in regions like the Orion nebula or the ρ-Ophiuchi molecular cloud but also for the formation of stars of the first or second generation in the universe. In this thesis we show how the angular momentum of prestellar and protostellar cores evolves and compare our results with observed quantities. The specific angular momentum of prestellar cores in our models agree remarkably well with observations of cloud cores. Some prestellar cores go into collapse to build up stars and stellar systems. The resulting protostellar objects have specific angular momenta that fall into the range of observed binaries. We find that collapse induced by gravoturbulent fragmentation is accompanied by a substantial loss of specific angular momentum. This eases the "angular momentum problem" in star formation even in the absence of magnetic fields. The distribution of stellar masses at birth (the initial mass function, IMF) is another aspect that any theory of star formation must explain. We focus on the influence of the thermodynamic properties of star-forming gas and address this issue by studying the effects of a piecewise polytropic equation of state on the formation of stellar clusters. We increase the polytropic exponent γ from a value below unity to a value above unity at a certain critical density. The change of the thermodynamic state at the critical density selects a characteristic mass scale for fragmentation, which we relate to the peak of the IMF observed in the solar neighborhood. Our investigation generally supports the idea that the distribution of stellar masses depends mainly on the thermodynamic state of the gas. A common assumption is that the chemical evolution of the star-forming gas can be decoupled from its dynamical evolution, with the former never affecting the latter. Although justified in some circumstances, this assumption is not true in every case. In particular, in low-metallicity gas the timescales for reaching the chemical equilibrium are comparable or larger than the dynamical timescales. In this thesis we take a first approach to combine a chemical network with a hydrodynamical code in order to study the influence of low levels of metal enrichment on the cooling and collapse of ionized gas in small protogalactic halos. Our initial conditions represent protogalaxies forming within a fossil HII region -- a previously ionized HII region which has not yet had time to cool and recombine. We show that in these regions, H2 is the dominant and most effective coolant, and that it is the amount of H2 formed that controls whether or not the gas can collapse and form stars. For metallicities Z <= 10-3 Zsun, metal line cooling alters the density and temperature evolution of the gas by less than 1\% compared to the metal-free case at densities below 1 cm-3 and temperatures above 2000 K. We also find that an external ultraviolet background delays or suppresses the cooling and collapse of the gas regardless of whether it is metal-enriched or not. Finally, we study the dependence of this process on redshift and mass of the dark matter halo.}, subject = {Sternentstehung}, language = {en} } @phdthesis{Klessen2004, author = {Klessen, Ralf S.}, title = {The relation between interstellar turbulence and star formation}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-0001118}, school = {Universit{\"a}t Potsdam}, year = {2004}, abstract = {Eine der zentralen Fragestellungen der modernen Astrophysik ist es, unser Verst{\"a}ndnis fuer die Bildung von Sternen und Sternhaufen in unserer Milchstrasse zu erweitern und zu vertiefen. Sterne entstehen in interstellaren Wolken aus molekularem Wasserstoffgas. In den vergangenen zwanzig bis dreißig Jahren ging man davon aus, dass der Prozess der Sternentstehung vor allem durch das Wechselspiel von gravitativer Anziehung und magnetischer Abstossung bestimmt ist. Neuere Erkenntnisse, sowohl von Seiten der Beobachtung als auch der Theorie, deuten darauf hin, dass nicht Magnetfelder, sondern {\"U}berschallturbulenz die Bildung von Sternen in galaktischen Molek{\"u}lwolken bestimmt. Diese Arbeit fasst diese neuen {\"U}berlegungen zusammen, erweitert sie und formuliert eine neue Theorie der Sternentstehung die auf dem komplexen Wechselspiel von Eigengravitation des Wolkengases und der darin beobachteten {\"U}berschallturbulenz basiert. Die kinetische Energie des turbulenten Geschwindigkeitsfeldes ist typischerweise ausreichend, um interstellare Gaswolken auf großen Skalen gegen gravitative Kontraktion zu stabilisieren. Auf kleinen Skalen jedoch f{\"u}hrt diese Turbulenz zu starken Dichtefluktuationen, wobei einige davon die lokale kritische Masse und Dichte f{\"u}r gravitativen Kollaps {\"u}berschreiten koennen. Diese Regionen schockkomprimierten Gases sind es nun, aus denen sich die Sterne der Milchstrasse bilden. Die Effizienz und die Zeitskala der Sternentstehung h{\"a}ngt somit unmittelbar von den Eigenschaften der Turbulenz in interstellaren Gaswolken ab. Sterne bilden sich langsam und in Isolation, wenn der Widerstand des turbulenten Geschwindigkeitsfeldes gegen gravitativen Kollaps sehr stark ist. {\"U}berwiegt hingegen der Einfluss der Eigengravitation, dann bilden sich Sternen in dichten Gruppen oder Haufen sehr rasch und mit grosser Effizienz. Die Vorhersagungen dieser Theorie werden sowohl auf Skalen einzelner Sternentstehungsgebiete als auch auf Skalen der Scheibe unserer Milchstrasse als ganzes untersucht. Es zu erwarten, dass protostellare Kerne, d.h. die direkten Vorl{\"a}ufer von Sternen oder Doppelsternsystemen, eine hochgradig dynamische Zeitentwicklung aufweisen, und keineswegs quasi-statische Objekte sind, wie es in der Theorie der magnetisch moderierten Sternentstehung vorausgesetzt wird. So muss etwa die Massenanwachsrate junger Sterne starken zeitlichen Schwankungen unterworfen sein, was wiederum wichtige Konsequenzen f{\"u}r die statistische Verteilung der resultierenden Sternmassen hat. Auch auf galaktischen Skalen scheint die Wechselwirkung von Turbulenz und Gravitation maßgeblich. Der Prozess wird hier allerdings noch zus{\"a}tzlich moduliert durch chemische Prozesse, die die Heizung und K{\"u}hlung des Gases bestimmen, und durch die differenzielle Rotation der galaktischen Scheibe. Als wichtigster Mechanismus zur Erzeugung der interstellaren Turbulenz l{\"a}sst sich die {\"U}berlagerung vieler Supernova-Explosionen identifizieren, die das Sterben massiver Sterne begleiten und große Mengen an Energie und Impuls freisetzen. Insgesamt unterst{\"u}tzen die Beobachtungsbefunde auf allen Skalen das Bild der turbulenten, dynamischen Sternentstehung, so wie es in dieser Arbeit gezeichnet wird.}, language = {en} } @phdthesis{Schmeja2006, author = {Schmeja, Stefan}, title = {Properties of turbulent star-forming clusters : models versus observations}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-7364}, school = {Universit{\"a}t Potsdam}, year = {2006}, abstract = {Stars are born in turbulent molecular clouds that fragment and collapse under the influence of their own gravity, forming a cluster of hundred or more stars. The star formation process is controlled by the interplay between supersonic turbulence and gravity. In this work, the properties of stellar clusters created by numerical simulations of gravoturbulent fragmentation are compared to those from observations. This includes the analysis of properties of individual protostars as well as statistical properties of the entire cluster. It is demonstrated that protostellar mass accretion is a highly dynamical and time-variant process. The peak accretion rate is reached shortly after the formation of the protostellar core. It is about one order of magnitude higher than the constant accretion rate predicted by the collapse of a classical singular isothermal sphere, in agreement with the observations. For a more reasonable comparison, the model accretion rates are converted to the observables bolometric temperature, bolometric luminosity, and envelope mass. The accretion rates from the simulations are used as input for an evolutionary scheme. The resulting distribution in the Tbol-Lbol-Menv parameter space is then compared to observational data by means of a 3D Kolmogorov-Smirnov test. The highest probability found that the distributions of model tracks and observational data points are drawn from the same population is 70\%. The ratios of objects belonging to different evolutionary classes in observed star-forming clusters are compared to the temporal evolution of the gravoturbulent models in order to estimate the evolutionary stage of a cluster. While it is difficult to estimate absolute ages, the realtive numbers of young stars reveal the evolutionary status of a cluster with respect to other clusters. The sequence shows Serpens as the youngest and IC 348 as the most evolved of the investigated clusters. Finally the structures of young star clusters are investigated by applying different statistical methods like the normalised mean correlation length and the minimum spanning tree technique and by a newly defined measure for the cluster elongation. The clustering parameters of the model clusters correspond in many cases well to those from observed ones. The temporal evolution of the clustering parameters shows that the star cluster builds up from several subclusters and evolves to a more centrally concentrated cluster, while the cluster expands slower than new stars are formed.}, subject = {Sternentstehung}, language = {en} }