This volume presents the state-of-the-art in selected topics across modern nuclear physics, covering fields of central importance to research and illustrating their connection to many different areas of physics. It describes recent progress in the study of superheavy and exotic nuclei, which is pushing our knowledge to ever heavier elements and neutron-richer isotopes. Extending nuclear physics to systems that are many times denser than even the core of an atomic nucleus, one enters the realm of the physics of neutron stars and possibly quark stars, a topic that is intensively investigated with many ground-based and outer-space research missions as well as numerous theoretical works. By colliding two nuclei at very high ultra-relativistic energies one can create a fireball of extremely hot matter, reminiscent of the universe very shortly after the big bang, leading to a phase of melted hadrons and free quarks and gluons, the so-called quark-gluon plasma. These studies tie up with effects of crucial importance in other fields. During the collision of heavy ions, electric fields of extreme strength are produced, potentially destabilizing the vacuum of the atomic physics system, subsequently leading to the decay of the vacuum state and the emission of positrons. In neutron stars the ultra-dense matter might support extremely high magnetic fields, far beyond anything that can be produced in the laboratory, significantly affecting the stellar properties. At very high densities general relativity predicts the stellar collapse to a black hole. However, a number of current theoretical activities, modifying Einstein's theory, point to possible alternative scenarios, where this collapse might be avoided. These and related topics are addressed in this book in a series of highly readable chapters. In addition, the book includes fundamental analyses of the practicalities involved in transiting to an electricity supply mainly based on renewable energies, investigating this scenario less from an engineering and more from a physics point of view. While the topics comprise a large scope of activities, the contributions also show an extensive overlap in the methodology and in the analytical and numerical tools involved in tackling these diverse research fields that are the forefront of modern science.

This book explores the role of singularities in general relativity (GR): The theory predicts that when a sufficient large mass collapses, no known force is able to stop it until all mass is concentrated at a point. The question arises, whether an acceptable physical theory should have a singularity, not even a coordinate singularity. The appearance of a singularity shows the limitations of the theory. In GR this limitation is the strong gravitational force acting near and at a super-massive concentration of a central mass. First, a historical overview is given, on former attempts to extend GR (which includes Einstein himself), all with distinct motivations. It will be shown that the only possible algebraic extension is to introduce pseudo-complex (pc) coordinates, otherwise for weak gravitational fields non-physical ghost solutions appear. Thus, the need to use pc-variables. We will see, that the theory contains a minimal length, with important consequences. After that, the pc-GR is formulated and compared to the former attempts. A new variational principle is introduced, which requires in the Einstein equations an additional contribution. Alternatively, the standard variational principle can be applied, but one has to introduce a constraint with the same former results. The additional contribution will be associated to vacuum fluctuation, whose dependence on the radial distance can be approximately obtained, using semi-classical Quantum Mechanics. The main point is that pc-GR predicts that mass not only curves the space but also changes the vacuum structure of the space itself. In the following chapters, the minimal length will be set to zero, due to its smallness. Nevertheless, the pc-GR will keep a remnant of the pc-description, namely that the appearance of a term, which we may call "dark energy", is inevitable. The first application will be discussed in chapter 3, namely solutions of central mass distributions. For a non-rotating massive object it is the pc-Schwarzschild solution, for a rotating massive object the pc-Kerr solution and for a charged massive object it will be the Reissner-Nordstroem solution. This chapter serves to become familiar on how to resolve problems in pc-GR and on how to interpret the results. One of the main consequences is, that we can eliminate the event horizon and thus there will be no black holes. The huge massive objects in the center of nearly any galaxy and the so-called galactic black holes are within pc-GR still there, but with the absence of an event horizon! Chapter 4 gives another application of the theory, namely the Robertson-Walker solution, which we use to model different outcomes of the evolution of the universe. Finally the capability of this theory to predict new phenomena is illustrated.

This volume presents the state-of-the-art in selected topics across modern nuclear physics, covering fields of central importance to research and illustrating their connection to many different areas of physics. It describes recent progress in the study of superheavy and exotic nuclei, which is pushing our knowledge to ever heavier elements and neutron-richer isotopes. Extending nuclear physics to systems that are many times denser than even the core of an atomic nucleus, one enters the realm of the physics of neutron stars and possibly quark stars, a topic that is intensively investigated with many ground-based and outer-space research missions as well as numerous theoretical works. By colliding two nuclei at very high ultra-relativistic energies one can create a fireball of extremely hot matter, reminiscent of the universe very shortly after the big bang, leading to a phase of melted hadrons and free quarks and gluons, the so-called quark-gluon plasma. These studies tie up with effects of crucial importance in other fields. During the collision of heavy ions, electric fields of extreme strength are produced, potentially destabilizing the vacuum of the atomic physics system, subsequently leading to the decay of the vacuum state and the emission of positrons. In neutron stars the ultra-dense matter might support extremely high magnetic fields, far beyond anything that can be produced in the laboratory, significantly affecting the stellar properties. At very high densities general relativity predicts the stellar collapse to a black hole. However, a number of current theoretical activities, modifying Einstein's theory, point to possible alternative scenarios, where this collapse might be avoided. These and related topics are addressed in this book in a series of highly readable chapters. In addition, the book includes fundamental analyses of the practicalities involved in transiting to an electricity supply mainly based on renewable energies, investigating this scenario less from an engineering and more from a physics point of view. While the topics comprise a large scope of activities, the contributions also show an extensive overlap in the methodology and in the analytical and numerical tools involved in tackling these diverse research fields that are the forefront of modern science.

This book explores the role of singularities in general relativity (GR): The theory predicts that when a sufficient large mass collapses, no known force is able to stop it until all mass is concentrated at a point. The question arises, whether an acceptable physical theory should have a singularity, not even a coordinate singularity. The appearance of a singularity shows the limitations of the theory. In GR this limitation is the strong gravitational force acting near and at a super-massive concentration of a central mass. First, a historical overview is given, on former attempts to extend GR (which includes Einstein himself), all with distinct motivations. It will be shown that the only possible algebraic extension is to introduce pseudo-complex (pc) coordinates, otherwise for weak gravitational fields non-physical ghost solutions appear. Thus, the need to use pc-variables. We will see, that the theory contains a minimal length, with important consequences. After that, the pc-GR is formulated and compared to the former attempts. A new variational principle is introduced, which requires in the Einstein equations an additional contribution. Alternatively, the standard variational principle can be applied, but one has to introduce a constraint with the same former results. The additional contribution will be associated to vacuum fluctuation, whose dependence on the radial distance can be approximately obtained, using semi-classical Quantum Mechanics. The main point is that pc-GR predicts that mass not only curves the space but also changes the vacuum structure of the space itself. In the following chapters, the minimal length will be set to zero, due to its smallness. Nevertheless, the pc-GR will keep a remnant of the pc-description, namely that the appearance of a term, which we may call "dark energy", is inevitable. The first application will be discussed in chapter 3, namely solutions of central mass distributions. For a non-rotating massive object it is the pc-Schwarzschild solution, for a rotating massive object the pc-Kerr solution and for a charged massive object it will be the Reissner-Nordstroem solution. This chapter serves to become familiar on how to resolve problems in pc-GR and on how to interpret the results. One of the main consequences is, that we can eliminate the event horizon and thus there will be no black holes. The huge massive objects in the center of nearly any galaxy and the so-called galactic black holes are within pc-GR still there, but with the absence of an event horizon! Chapter 4 gives another application of the theory, namely the Robertson-Walker solution, which we use to model different outcomes of the evolution of the universe. Finally the capability of this theory to predict new phenomena is illustrated.

Studienarbeit aus dem Jahr 2010 im Fachbereich BWL - Personal und Organisation, Note: 1,3, Fachhochschule Schmalkalden, Sprache: Deutsch, Abstract: Einleitung Nichts ist so spannend wie Wirtschaft, ausser Fussball. Auch durch einen ent-sprechenden Umkehrschluss dieses Satzes, trifft die Trivialitat zu, dass weder im Fussball, noch in der Wirtschaft vorhersehbar ist, was im nachsten Moment passiert. So kann man den Ball sinnbildlich durch ein Produkt ersetzen, die gegnerische Mannschaft als Mitbewerber verstehen, die Fans auf den Tribunen durch Kunden ersetzen und die Flanke als Kooperationsangebot ansehen. In beiden Bereichen geht es um das Hervorrufen von Leidenschaft, Kampfgeist, Taktik, Gefuhle und letztendlich um das Gewinnen. Im Fussball und Wirtschaft ist die Massgabe des maximalen Erfolgs immer ge-genwartig und bestimmt den Alltag der Mitarbeiter. Um diesen hohen Anforde-rungen gerecht zu werden, bedarf es einer gewissen Entschlossenheit und Zielstrebigkeit jedes Einzelnen. Um ein Maximum an Leistung des Personals zu erreichen, um Angste, individuelle Schwachen und Grenzen zu uberwinden, ist Teamgeist gefragt. Spezielles Konnen, charakterliche Eigenarten und mannschaftliche Geschlossenheit sind dabei miteinander zu vereinen, um folglich eine Synergie zu erzeugen. Wie so etwas erreicht werden kann, soll die vorliegende Arbeit, mit dem Thema: Teambuildung - Was kann man vom Fussball lernen?," aufzeigen. Hierbei soll der Prozess Teambuilding im Ganzen und in den einzelnen Bereichen erklart und dabei konkrete Lerneffekte fur die Wirtschaft aufgezeigt werden. Unter Teambuilding kann die Intention verstanden werden, Personen mit bestimmten Fahigkeiten und Kenntnissen zu identifizieren, um diese mit anderen spezialisierten Personen in einem Team, das eine definierte Aufgabe losen soll, zu vereinen. Hauptbestandteile der anzustellenden Begutachtung werden demnach unter anderem sein, der psychologische Prozess sowie die Teamzusammensetzung als essentieller Ba

Studienarbeit aus dem Jahr 2009 im Fachbereich Jura - Zivilrecht / Arbeitsrecht, Note: 1,0, Fachhochschule Schmalkalden, Sprache: Deutsch, Abstract: Arbeitszeugnisse sind eingebettet in das Rechtssystem Deutschlands und werden dem juristischen Teilbereich Arbeitsrecht zugeordnet. Das Arbeitsrecht ist der Teilbereich unseres Rechtssystems, der das fur die Rechtsbeziehungen zwischen Arbeitgeber und Arbeitnehmer geltende Recht umfasst. Grundtatbestand ist die abhangige Arbeit. Abhangige Arbeit ist gegenwartig die dominante Form der Erwerbstatigkeit. In Deutschland leisten circa 74,5% der Erwerbspersonen eine abhangige Arbeit bzw. suchen eine solche, dagegen sind nur 25,5% der Erwerbstatigen Bundesburger selbstandig oder sind als mithelfende Familienangehorige tatig. Somit bedarf es ei-ner Leistungsbeurteilung bzw. eines Nachweises in Form eines Arbeitszeugnisses fur den Grossteil der abhangig Beschaftigten. Arbeitszeugnisse sind fur Arbeitgeber und Arbeitnehmer gleichermassen von zentraler Bedeutung. Dem Arbeitnehmer dient es als Nachweis seiner beruflichen Tatigkeit, da es Aussagen uber den Werdegang im Unternehmen und die erbrachten Leistungen enthalt. Mithin ist das Arbeitszeugnis ein wichtiger Bestandteil der Bewerbungsunterlagen. Auch in der betrieblichen Personalpraxis nehmen Arbeitszeugnisse eine wichtige Rolle ein, da sie einerseits als Beurteilung fur ausscheidende Arbeitnehmer erstellt werden und andererseits als Instrument der betrieblichen Personalrekrutierung genutzt werden. Die Anspruchsgrundlagen fur die verschiedenen Personenkreise, die Durchsetzungswege und -Moglichkeiten sind anhand von Gesetzen geregelt. Der Inhalt von Arbeitszeugnissen ist gepragt von den Grundsatzen zur Erstellung und der sog. Zeugnissprache. Der Rahmen fur die formale und die inhaltliche Ausgestaltung der Arbeitszeugnisse, wird weitgehend durch die Rechtsprechung der Arbeitsgerichte bestimmt. Aus diesen Grunden werden Arbeitszeugnisse als burokratisch, genau und typisch deuts