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Back to bureaucracy?
No full textIn this contribution, the emergence of the neo-Weberian state (NWS) is analyzed with regard to German public administration. Drawing on the concept of a governance space, which consists of a hierarchy, markets, and networks, we distinguish between four empirical manifestations of the NWS, namely, the NWS as (1) come back of the public/ re-municipalization; (2) re-hierarchization; (3) de-agencification; (4) de-escalation in performance management. These movements can, on the one hand, be interpreted as a (partial) reversal of New Public Management (NPM) approaches and a “swinging back of the pendulum” (see Kuhlmann & Wollmann, 2019) toward public and classical Weberian principles (e.g., hierarchy, regulation, institutional re-aggregation). This reversal re-strengthened the hierarchy within the overall governance space to the detriment of, but without completely replacing, market mechanisms and networks. NPM’s failure to deliver what it promised and its inappropriateness as a response to more recent challenges connected to crises and wicked problems have engendered a partial return of the public and a move away from the economization logic of NPM. On the other hand, post-NPM reversals and managerial de-escalation gave rise to hybrid models that merge NPM and classic Weberian administration. While some well-functioning combinations of NPM and Weberianism exist, the hybridization of “old” and “neo” elements has also provoked ambivalent and negative assessments regarding the actual functioning of the NWS in Germany. Our analysis suggests that the NWS is only partially suitable as a model for reform and future administrative modernization, largely depending on the context surrounding reform and implementation practices
Facilitating and hindering factors for routine adaptations in manufacturing and effects on human performance- unexpected insights from three experimental studies in a special purpose setting
No full textConsumer behaviour changes and strategic management decisions are driving adaptations in manufacturing routines. Based on the theory of situational strength, we investigated how contextual and person-related factors influence workers’ adaptation in a two-worker position routine. Contextual factors, like retrieval cues (Study 1), time pressure (Study 2), and convenience (Study 3), were varied. Person-related factors included retentivity, general and routine-specific self-efficacy, and perceived adaptation costs. Dependent variables included various error types and production time before and after adaptation. In each study, 148 participants were trained in a production routine at t1 and executed an adapted routine at t2, one week later. Repeated measures ANOVA for performance at t1 and t2, and MANOVA for performance at t2, revealed that time increased for all groups at t2. For participants in Studies 1 & 2, error rates remained consistent. Retentivity significantly impacted errors at both t1 and t2, emphasising that routine changes in a ‘running business’ take time, regardless of contextual factors. Workers with lower retentivity may require additional support
Klausur im Medienrecht
No full textDie Privatsphäre prominenter Personen wird häufig durch eine auf Sensationsgier ausgerichtete Presseberichterstattung gefährdet. Während sich die Presse dabei vordergründig auf ein öffentliches Interesse an solchen Berichten beruft, kann die Reputation der Betroffenen in der Öffentlichkeit stark und dauerhaft beeinträchtigt werden. Jedoch folgen aus dem Allgemeinen Persönlichkeitsrecht mehrere Ansprüche, mit denen diese Rechtsverletzungen abgewehrt und mögliche Schäden kompensiert werden können
Cain and Abel
No full textThe biblical story of Cain and Abel in Genesis 4:1–16 appears as the first case of siblings’ rivalry in the Torah. It is the starting point of a socio-ethical process of human development within the book of Genesis. The sibling narrative also includes the first report of homicide, more precisely a fratricide, as Cain slays his own brother Abel (Gen 4:8). The Jewish and Christian reception discourse of the Cain-Abel-story developed early on to deal with a range of open questions and difficult passages provided by the biblical text. The basic assumptions of Jewish and Christian interpretations are initially similar in terms of attempting to explain God’s preference for Abel’s sacrifice and Cain’s motivation for killing his brother
Zivilklausur an der Universität
No full textDie Klausur wurde für den früheren Teil- schwerpunkt Kulturrecht am Fachbereich Rechts- und Wirtschaftswissenschaft der Johannes Gutenberg-Universität Mainz konzipiert, eignet sich aber auch für die Vorbereitung auf die staatliche Pflichtfach- prüfung sowie für den Schwerpunkt Wirtschaft-Staat-Kommunales (SPB 7)
KI in der Justiz
No full textDieser Artikel soll Studierenden einen kurzen Überblick über die Herausforderungen des Einsatzes neuer Technologien, insbes. Künstlicher Intelligenz, in der Justiz geben und den Blick für juristische Probleme des digitalen Zeitalters schärfen
Die Justizpressekonferenz in Karlsruhe
No full textDer Aufsatz basiert auf einer im Wintersemester 2022/23 vorgelegten Probeseminararbeit im SPB "Medien- und Wirtschaftsrecht" (16 P.) bei Prof. Dr. Marcus Schladebach und stellt eine gekürzte Fassung dieser Arbeit dar
Plotinus’ concept of ‘We’ and its relation to the Kantian tradition
No full textHailed as an innovative concept in antiquity, Plotinus’ concept of the ‘we’ occupies a nuanced and somewhat elusive systematic position. On the one hand, it locates itself in the realm of the soul rather than the intellect; at the same time, however, it manifests a self-conscious dimension typically ascribed to the intellect rather than the soul. This paper attempts to resolve this ambiguity by interpreting the ‘we’ as a potential of self-consciousness, which explains why the ‘we’ can become similar to, but not identical with, the actual self-consciousness of the intellect. The proposed definition not only brings clarity to the seemingly paradoxical formulations surrounding the ‘we’ in Plotinus’ philosophy but also sheds light on the allegories that Plotinus employs.
Moreover, my analysis highlights the similarity between the Plotinian ‘we’ and the characterizations of the self within the Kantian tradition. Drawing on Cassirer’s dichotomy between concepts of substance and concepts of function, and Kant’s assertion that the ‘I think’ represents a potentiality rather than an actuality of self-consciousness, this study attempts to provide a conceptual bridge between the Plotinian and Kantian frameworks
Fichte and Hegel on Advancing from the Beginning
No full textIn the Science of Logic, Hegel criticizes Fichte's Wissenschaftslehre for advancing from the beginning through external reflection and thus failing to understand both the nature of the beginning and the proper method to advance from it. This article shows that Fichte's advance from the beginning preempts Hegel's critique and shares Hegel's premises with respect to the method of advancing. The author first analyzes Hegel's critique of Fichte in the Science of Logic, which he follows by showing that Fichte levels a similar critique against Schelling's conception of the beginning set out in his system of 1801. Turning to the Wissenschaftslehre of 1794/5, the author then demonstrates that Fichte's method of advancing from the beginning addresses every point of Hegel's critique. He concludes by identifying the similarity and difference between Fichte's and Hegel's methods of advancing
Untersuchung des Einflusses enger Begleiter auf die späte Sternentwicklung
No full textSterne sind die fundamentalsten Grundbestandteile von Galaxien. Das Alter, die Verteilung und die Zusammensetzung der Sterne geben die Geschichte und weitere Entwicklung der Galaxien wieder, in denen sie sich befinden. Sterne sind außerdem für die Entstehung der schweren Elemente verantwortlich und die Bestimmung ihrer Eigenschaften ist wichtig, um die Eigenschaften ihrer Planetensysteme zu messen. Das Verständnis ihrer Entstehung und Entwicklung ist daher ein zentrales Feld der Astrophysik.
Die meisten Sterne werden nicht alleine geboren, sondern mit einem oder mehreren Begleitern, die gravitativ gebunden umeinander kreisen. In einem erheblichen Anteil dieser Sternsysteme beeinflussen die Sterne sich gegenseitig. Dies kann zu signifikanten Änderungen in der Sternentwicklung führen und kann daher nicht vernachlässigt werden, wenn man die Sternentwicklung verstehen will.
Stern auf den anderen. Abhängig vom Massenverhältnis der Sterne ist dieser Massentransfer
stabil oder instabil. In Systemen, in denen die Massen sehr unterschiedlich sind, ist die Massentransferrate so hoch, dass sich eine gemeinsame Hülle (Common Envelope) um beide Sterne bildet, in der der Kern des Hauptsterns und der Begleiter umeinander kreisen. Reibung mit der Hülle führt zu einer schnellen Verkleinerung der Umlaufbahn auf der Zeitskala von nur einigen tausend Tagen und ist daher schwer zu beobachten. Das Vorhandensein von Sternsystemen, bei denen der Abstand beider Sterne kleiner als der Radius der Vorläufersterne ist, zeigt jedoch, dass es diese Entwicklungsphase geben muss.
Die Common Envelope Phase ist eine der am wenigsten verstandenen Entwicklungsphasen von engen Doppelsternsystemen. Sie ist für das Verständnis einer Vielzahl von interessanten Systemen wichtig, wie z.B. die Vorläufersysteme von Objekten, die irgendwann miteinander verschmelzen werden und dabei Gravitationswellen aussenden. Für das physikalische Verständnis dieser wichtigen Entwicklungsphase müssen Simulationen durchgeführt werden. Um diese zu validieren, braucht es eine statistisch signifikante, untersuchte Stichprobe von Doppelsternen, die diese Phase durchlebt haben.
Mit dieser Arbeit leiste ich einen signifikanten Beitrag zur Beobachtung von Doppelsternen nach der Common Envelope Phase, indem ich die Anzahl der bekannten sowie der analysierten Systeme erheblich erhöhe, sowie deren Eigenschaften untersuche. Außerdem präsentiere ich die detaillierte Analyse von mehreren interessanten engen Doppelsternsystemen, die in ihrer Entwicklung durch eine Phase von instabilen oder stabilen Massentransfer gegangen sind. Dabei werden auch noch andere Arten von stellaren Wechselwirkungen untersucht, wie zum Beispiel der Einfluss von Gezeiten oder Magnetfeldern. In der abschließenden Diskussion werden die Ergebnisse in den Kontext zu den bisherigen Beobachtungen gesetzt. Diese Arbeit ist ein erster wichtiger Schritt für die Bewältigung der in den nächsten Jahren erwarteten Flut an neuen Daten von im Moment im Bau befindlichen Teleskopen und die hierin entdeckten Systeme werden einen bedeutenden Beitrag zum Verständnis der wichtigen, aber sehr schlecht verstandenen, Common Envelope Phase leisten.Stars are the most fundamental constituents of galaxies. The age, distribution, and composition of the stars in a galaxy can be used to derive the history and evolution of the host galaxy. The stars are responsible for synthesizing and distributing heavier elements. The understanding of the host stars is essential to decode the characteristics of planetary systems. This means that studying the formation, evolution, and death of stars is a central field of astrophysics.
Most stars are not born alone but are found to have one or several companions. In a significant fraction of those systems, the companions will interact with each other during their lifetime and so influence each other significantly. This can lead to substantial changes in the evolution of stars in close binary systems and cannot be neglected, if we want to understand stellar evolution. There are different kinds of interactions, which are observed. Tidal interactions can influence the stellar rotation velocity. Strong irradiation can alter the structure of the companions and is vital also for the understanding of close-in planets such as Hot Jupiters. Magnetic interactions can change the orbital period of the binary systems.
The most important interaction is mass transfer from one star to the other. Depending on the initial separation of the system, this can happen in different evolutionary phases. The mass ratio of both stars in the binary system is determining, if the mass transfer is stable or not. Binary systems with two stars of similar mass can experience stable mass transfer when they are close enough. Thereby mass is transferred from one star to the other, changing both stellar masses. The companion accreting the matter is spun-up and so rejuvenated. In systems where the stars have significantly different masses, the mass transfer is expected to happen on a dynamical timescale and the rate of mass transfer will be so high that a common envelope around both stars is formed. Friction in the envelope leads to a rapid shrinking of the orbit on the timescale of a few thousands of days and is difficult to observe. The observation of many evolved systems with orbital separations smaller than the radius of a red giant shows that such a phase must exist. During the spiral-in, energy and angular momentum is transferred to the envelope and can lead to its ejection, when the transferred energy is sufficient to unbind it.
Common-envelope evolution is crucial to understand many exciting systems, which are ob- served in our universe. It is essential for the formation of stellar-mass gravitational merger sources, as it can bring compact-object binaries close enough together so that gravitational waves can lead to a merger within a Hubble time. This phase is also vital for the understanding of progenitor systems of supernovae type Ia, which are used as standard candles to derive distances to far galaxies. With their help the existence of cosmological dark energy could be inferred. Supernovae type Ia are thought to be produced by the explosion of carbon-oxygen white dwarfs exceeding their upper mass limit, the Chandrasekhar mass. The most likely progenitor systems are still under debate.
The common envelope phase is one of the most significant and least-constrained processes in stellar binary evolution, and one of the most important unsolved problems in the understanding of stellar evolution. As it is a short-lived phase, direct observations are very unlikely and a statistically significant sample of systems after this phase is necessary to gain insight into it. For the physical understanding of this process (magneto-) hydrodynamical simulations have to be performed. A large enough sample of post-common envelope systems with observed masses, radii and orbital separations can provide the parameter range that has to be explained by the simulations.
In this thesis, I make a significant contribution to the investigation of binary systems after the common envelope phase by newly discovering a large sample post-common envelope systems and also significantly increasing the number of systems with derived parameters. This sample is a first step to acquire a statistically significant sample for a better understanding of this crucial but not yet understood phase. Moreover, I also present the detailed analysis of several kinds of interesting close binary systems studying different aspects of these systems, as the influence of tidal forces, the effect of mass transfer and orbital period changes among other things.
I will give a short introduction to the current state of knowledge regarding stellar evolution of single stars and the influence of close companions on this evolution. Moreover, I give a short introduction into the different kinds of close binary systems we studied. I also give a short summary of the methods used to investigate those systems. Subsequently, to the appended papers, I will discuss the results and give a short summary