The Euclidean approach to Quantum Gravity was initiated almost 15 years ago in an attempt to understand the difficulties raised by the spacetime singularities of classical general relativity which arise in the gravitational collapse of stars to form black holes and the entire universe in the Big Bang. An important motivation was to develop an approach capable of dealing with the nonlinear, non-perturbative aspects of quantum gravity due to topologically non-trivial spacetimes. There are important links with a Riemannian geometry. Since its inception the theory has been applied to a number of important physical problems including the thermodynamic properties of black holes, quantum cosmology and the problem of the cosmological constant. It is currently at the centre of a great deal of interest.This is a collection of survey lectures and reprints of some important lectures on the Euclidean approach to quantum gravity in which one expresses the Feynman path integral as a sum over Riemannian metrics. As well as papers on the basic formalism there are sections on Black Holes, Quantum Cosmology, Wormholes and Gravitational Instantons.

The winner of UCL's annual HEP thesis prize, this work describes an analysis of the data from the second flight of the Antarctica Impulsive Transient Antenna (ANITA). ANITA is a balloon-borne experiment that searches for radio signals originating from ultra-high energy neutrinos and cosmic rays interacting with the Antarctic ice or air. The search for ultrahigh energy neutrinos of astrophysical origin is one of the outstanding experimental challenges of the 21st century. The ANITA experiment was designed to be the most sensitive instrument to ultra-high energy neutrinos that originate from the interactions of cosmic rays with the cosmic microwave background. The methodology and results of the neutrino and cosmic ray searches are presented in the thesis.

This is volume 2 of Planets, Stars and Stellar Systems, a six-volume compendium of modern astronomical research, covering subjects of key interest to the main fields of contemporary astronomy. This volume on Astronomical Techniques, Software, and Data edited by Howard E. Bond presents accessible review chapters on Astronomical Photometry, Astronomical Spectroscopy, Infrared Astronomy Fundamentals, Astronomical Polarimetry: Polarized Views of Stars and Planets, Sky Surveys, Techniques of Radio Astronomy, Radio and Optical Interferometry: Basic Observing Techniques and Data Analysis, Absolute Calibration of Spectrophotometric Standard Stars, Virtual Observatories, Data Mining, and Astroinformatics, Statistical Methods for Astronomy, Numerical Techniques in Astrophysics .

All chapters of the handbook were written by practicing professionals. They include sufficient background material and references to the current literature to allow readers to learn enough about a specialty within astronomy, astrophysics and cosmology to get started on their own practical research projects. In the spirit of the series Stars and Stellar Systems published by Chicago University Press in the 1960s and 1970s, each chapter of Planets, Stars and Stellar Systems can stand on its own as a fundamental review of its respective sub-discipline, and each volume can be used as a textbook or recommended reference work for advanced undergraduate or postgraduate courses. Advanced students and professional astronomers in their roles as both lecturers and researchers will welcome Planets, Stars and Stellar Systems as a comprehensive and pedagogical reference work on astronomy, astrophysics and cosmology.

A sweeping history of the Greeks, from the Bronze Age to today.

More than two thousand years ago, the Greek city-states, led by Athens and Sparta, laid the foundation for much of modern science, the arts, politics, and law. But the influence of the Greeks did not end with the rise and fall of this classical civilization. As historian Roderick Beaton illustrates, over three millennia Greek speakers produced a series of civilizations that were rooted in southeastern Europe but again and again ranged widely across the globe.

In The Greeks, Beaton traces this history from the Bronze Age Mycenaeans who built powerful fortresses at home and strong trade routes abroad, to the dramatic Eurasian conquests of Alexander the Great, to the pious Byzantines who sought to export Christianity worldwide, to today’s Greek diaspora, which flourishes on five continents. The product of decades of research, this is the story of the Greeks and their global impact told as never before. 

This book provides an introduction to relativistic dissipative fluid dynamics, with particular emphasis on its derivation from microscopic transport theory. After a phenomenological derivation of relativistic dissipative fluid dynamics from the second law of thermodynamics, the intrinsic instabilities of relativistic Navier-Stokes theory are discussed. In turn, analytical solutions of relativistic dissipative fluid dynamics are presented. Following, the authors discuss several theories and approaches to derive transport coefficients in dissipative fluid dynamics such as the Chapman-Enskog theory, the theory of Israel and Stewart, and a more recent derivation of relativistic dissipative fluid dynamics based on kinetic theory, which constitutes the main focus of the second part of this book. This book is intended for advanced graduate students and researchers in physics and requires basic knowledge of the theory of special and general relativity. It should be of particular interest to researchers that apply relativistic fluid dynamics in cosmology, astrophysics, and high-energy nuclear physics.

The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) satellite was launched on 5 February 2002. Its objective is to study the energy release and particle acceleration in solar flares through observations of X-rays and gamma rays. Two novel technologies are combined to obtain both spectra and images over a broad energy range. For the spectroscopy, cooled hyperpure germanium detectors are used to cover the energy range from 3 keV to 17 MeV with unprecedented keV-class resolution. Since focusing optics are not possible for making images with such high energy photons, tungsten and molybdenum absorbing grids are used to modulate the X-rays and gamma-rays coming from the Sun as the spacecraft rotates. This allows the spatial Fourier components of the source to be determined so that images can be made in spectral ranges where astronomical images have never been produced before. These new instrumental techniques require equally innovative software to reconstruct X-ray and gamma-ray spectra and images from the observations.

Ample solar activity, abundant observations, and an open data policy have attracted many researchers. Astronomers face in the RHESSI mission an exciting new scientific potential. It has unusually broad possibilities for improving our understanding of the enigmatic solar flare phenomenon that is becoming increasingly important as society depends more and more on space-based technologies.
In this volume, the functioning of RHESSI is explained, the data analysis techniques including spectroscopy and image reconstruction are introduced, and the experiences of the first few months of operation are summarized. First scientific results are presented thatprovide the essential base for more extended studies using RHESSI data and complementary observations by instruments on other spacecraft and at ground-based solar observatories.

The accompanying CD-ROM contains X-ray and EUV movies showing the dynamics of several solar flares. It also contains color versions of the graphics in the printed papers and additional material.

Scientists and students will find here the latest discoveries in solar flare research, as well as inspiration for future work. The papers will serve as references for the many new discoveries to come from the continuing RHESSI observations.

Stellar Structure and Evolution, the second volume in the Ohio State Astrophysics Series, takes advantage of our new era of stellar astrophysics, in which modern techniques allow us to map the interiors of stars in unprecedented detail. This textbook for upper-level undergraduate and graduate students aims to develop a broad physical understanding of the fundamental principles that dictate stellar properties. The study of stellar evolution focuses on the 'life cycle' of stars: how they are born, how they live, and how they die. As elements ejected by one generation of stars are incorporated into the next generation, stellar evolution is intertwined with the chemical evolution of our galaxy. Focusing on key physical processes without going into encyclopedic depth, the authors present stellar evolution in a contemporary context, including phenomena such as pulsations, mass loss, binary interactions, and rotation, which contribute to our understanding of stars.

These are the proceedings of a meeting celebrating Michael Thompson's seminal work on solar and stellar physics, as well as his major contributions to the development of the National Center for Atmospheric Research. The meeting also marked Michael J. Thompson's untimely death in October 2018. Michael played a key role in the development of helioseismology and its application to the study of the structure and dynamics of the solar interior, and he provided a strong foundation for the extension of seismic studies for other stars. After focusing for several years on more administrative activities, he was returning to leading the seismic studies of solar interior rotation and he was deeply involved in the understanding of the dynamics of the core of stars, when his life was tragically lost. The conference focused on dynamical aspects of the sun and stars, based on the large amount of data available on solar and stellar oscillations, and the extensive and detailed modelling now becoming feasible. Combining observations, seismic analysis, and modelling the meeting and this book serve as a fitting memorial to a close colleague and friend, much missed.

Interstellar dust grains catalyse chemical reactions, absorb, scatter, polarise and re-radiate starlight and constitute the building blocks for the formation of planets. Understanding this interstellar component is therefore of primary importance in many areas of astronomy & astrophysics. For example, observers need to understand how dust effects light passing through molecular clouds. Astrophysicists wish to comprehend how dust enables the collapse of clouds or how it determines the spectral behaviour of protostars, star forming regions or whole galaxies. This book gives a thorough theoretical description of the fundamental physics of interstellar dust: its composition, morphology, size distribution, dynamics, optical and thermal properties, alignment, polarisation, scattering, radiation and spectral features.
This encyclopedic book provides the basic physics towards understanding the solid matter in interstellar space. It includes all the necessary physics, including solid state physics, radiative transport, optical properties, thermodynamics, statistical mechanics and quantum mechanics. It then uses all of this basic physics in the specific case of dust grains in the interstellar medium.
Interstellar dust clouds catalyze simple chemical reactions, absorbs, scatters, polarizes and re-radiates starlight and forms the building blocks for planet and stellar formation. Understanding this interstellar medium is then of primary importance in many areas of astronomy & astrophysics. For example observers need to understand how it effects light passing through dust and molecular clouds, astrophysicists need to comprehend the formation and structure of dust clouds and how it collapses to form stars and planets.
Written in an accessible and descriptive manner, this will be essential supplementary reading for advanced undergraduate and graduate students taking courses on the interstellar medium and active researchers in need of a single source of well illustrated and detailed information.

The small bodies in planetary systems are indicative of the material evo- tion, the dynamical evolution, and the presence of planets in a system. Recent astronomicalresearch,spaceresearch,laboratoryresearch,andnumericals- ulationsbroughtawealthofnewandexciting?ndingsonextra-solarplanetary systems and on asteroids, comets, meteoroids, dust, and trans-Neptunian - jects in the solar system. Progress in astronomical instrumentation led to the discovery and investigation of small bodies in the outer solar system and to observations of cosmic dust in debris disks of extra-solar planetary systems. Space research allowed for close studies of some of the small solar system bodies from spacecraft. This lecture series is intended as an introduction to the latest research results and to the key issues of future research. The ch- ters are mainly based on lectures given during a recent research school and on research activities within the 21st Century COE Program "Origin and Evolution of Planetary Systems" at Kobe University, Japan. In Chap. 1, Taku Takeuchi discusses the evolution of gas and dust from protoplanetary disks to planetary disks. Using a simple model, he studies v- cous evolution and photoevaporation as possible mechanisms of gas dispersal. He further considers how the dust grows into planetesimals. Motion of dust particles induced by gas drag is described, and then using a simple analytic model, the dust growth timescale is discussed.

Studying the complex physical systems of stellar jets necessitates the incorporation of nonlinear effects which occur on a wide variety of length and timescales. One of the primary methods used to study the physics of jets is numerical simulations that apply high performance computing techniques. Such techniques are also required for analysing the huge modern astrophysical datasets.

This book examines those computing techniques. It is a collection of the lectures from the fifth and final school of the JETSET network, "Jets From Young Stars V: High Performance Computing in Astrophysics." It begins with an introduction to parallel programming techniques, with an emphasis on Message Passing Interface (MPI), before it goes on to review grid technology techniques and offer a practical introduction to Virtual Observatory. The second half of the book, then, is devoted to applications of high performance computing techniques, including 3D radiation transfer, to jet and star formation processes.

Aimed at graduate students in astrophysics, this book presents state-of-the-art methods, thereby offering interesting new insights to researchers in the field.

This book is a comprehensive survey of the current state of knowledge about the dynamics and gravitational properties of cosmic strings treated in the idealized classical approximation as line singularities described by the Nambu-Goto action. The author's purpose is to provide a standard reference to all work that has been published since the mid-1970s and to link this work together in a single conceptual framework and a single notational formalism. A working knowledge of basic general relativity is assumed. The book will be essential reading for researchers and postgraduate students in mathematics, theoretical physics, and astronomy interested in cosmic strings.

Olbers' paradox states that given the Universe is unbounded, governed by the standard laws of physics, and populated by light sources, the night sky should be ablaze with light. Obviously this is not so. However, the paradox does not lie in nature but in our understanding of physics. A Universe with a finite age, such as follows from big-bang theory, necessarily has galaxies of finite age. This means we can only see some of the galaxies in the Universe, which is the main reason why the night sky is dark. Just how dark can be calculated using the astrophysics of galaxies and stars and the dynamics of relativistic cosmology.
We know from the dynamics of individual galaxies and clusters of galaxies that the majority of matter that exerts gravitational forces is not detectable by conventional telescopes. This dark matter could have many forms, and candidates include various types of elementary particles as well as vacuum fluctuations, black holes, and others. Most of these candidates are unstable to decay and produce photons. So dark matter does not only affect the dynamics of the Universe, but the intensity of intergalactic radiation as well. Conversely, we can use observations of background radiation to constrain the nature and density of dark matter.
By comparing observational data with cosmological theory based on general relativity and particle physics, Dark Sky, Dark Matter reviews our present understanding of the universe and the astrophysics of the night sky and dark matter.

This textbook is a pedagogic introduction to a number of phenomena employing fluid mechanics. Beginning with basic concepts and conservation laws for neutral and charged fluids, the authors apply and develop them to understand aerodynamics, locomotion of micro-organisms, waves in air and water, shock waves, hydrodynamic and hydromagnetic instabilities, stars and black holes, blood flow in humans, and superfluids. The approach is to consider various striking topics on fluid mechanics, without losing necessary mathematical rigor. The book balances the qualitative explanations with formal treatment, in a compact manner. A special focus is given to the important and difficult subject of turbulence and the book ends with a discussion on turbulence in quantum fluids. The textbook is dotted by a number of illustrative examples, mostly from real life, and exercises. The textbook is designed for a one semester course and addresses students at undergraduate and graduate level in physics or engineering, who want to research in the fields as diverse as aeronautics, meteorology, cosmology, biomechanics, and mathematical physics. It is requested knowledge of an undergraduate level course on mathematical methods to better understand the topics presented here.

This book is about the mathematical theory of light propagation in media on general-relativistic spacetimes. The first part discusses the transition from Maxwell's equations to ray optics. The second part establishes a general mathematical framework for treating ray optics as a theory in its own right, making extensive use of the Hamiltonian formalism. This part also includes a detailed discussion of variational principles (i.e., various versions of Fermat's principle) for light rays in general-relativistic media. Some applications, e.g. to gravitational lensing, are worked out. The reader is assumed to have some basic knowledge of general relativity and some familiarity with differential geometry. Some of the results are published here for the first time, e.g. a general-relativistic version of Fermat's principle for light rays in a medium that has to satisfy some regularity condition only.

A thorough introduction to modern ideas on cosmology and on the physical basis of the general theory of relativity, An Introduction to the Science of Cosmology explores various theories and ideas in big bang cosmology, providing insight into current problems. Assuming no previous knowledge of astronomy or cosmology, this book takes you beyond introductory texts to the point where you are able to read and appreciate the scientific literature, which is broadly referenced in the book. The authors present the standard big bang theory of the universe and provide an introduction to current inflationary cosmology, emphasizing the underlying physics without excessive technical detail.
The book treats cosmological models without reliance on prior knowledge of general relativity, the necessary physics being introduced in the text as required. It also covers recent observational evidence pointing to an accelerating expansion of the universe. The first several chapters provide an introduction to the topics discussed later in the book. The next few chapters introduce relativistic cosmology and the classic observational tests. One chapter gives the main results of the hot big bang theory. Next, the book presents the inflationary model and discusses the problem of the origin of structure and the correspondingly more detailed tests of relativistic models. Finally, the book considers some general issues raised by expansion and isotropy. A reference section completes the work by listing essential formulae, symbols, and physical constants.
Beyond the level of many elementary books on cosmology, An Introduction to the Science of Cosmology encompasses numerous recent developments and ideas in the area. It provides more detailed coverage than many other titles available, and the inclusion of problems at the end of each chapter aids in self study and makes the book suitable for taught courses.

The review papers in this volume provide an in-depth examination of complex astrophysical phenomena of star formation via multi-wavelength observations and modeling. Among the fundamental issues discussed in the book are: The role of gravity and magnetized turbulence in the formation and evolution of molecular clouds The stellar feedback (supernovae, HII regions, winds, cosmic rays) in regulating star formation The origin of the stellar initial mass function and its universality across various environments Jets, magnetic fields and high energy particles in stellar clusters The origin of the first stars and black holes The goal of these papers is to review the major processes governing star formation and to investigate how they are interlinked. In doing so, they provide an in-depth look at the tremendous theoretical and observational progress that has been made in the recent past and also outline future perspectives. Previously published in Space Science Reviews in the Topical Collection "Star Formation"

A Telegraph Best Science Book of the Year "A witty yet in-depth exploration of the prospects for human habitation beyond Earth...Spacefarers is accessible, authoritative, and in the end, inspiring." -Richard Panek, author of The Trouble with Gravity It's been over fifty years since Apollo 11 landed on the moon. So why is there so little human presence in space? Will we ever reach Mars? And what will it take to become a multiplanet species? While many books have speculated on the possibility of living beyond the Earth, few have delved into the practical challenges. A wry and compelling take on the who, how, and why of near-future colonies in space, Spacefarers introduces us to the engineers, scientists, planners, dreamers, and entrepreneurs who are striving right now to make life in space a reality. While private companies such as SpaceX are taking the lead and earning profits from human space activity, Christopher Wanjek is convinced this is only the beginning. From bone-whittling microgravity to eye-popping profits, the risks and rewards of space settlement have never been so close at hand. He predicts we will have hotels in low-earth orbit, mining and tourism on the Moon, and science bases on Mars-possibly followed (gravity permitting) by full blown settlements. "Nerdily engaging (and often funny)...Technology and science fiction enthusiasts will find much here to delight them, as Wanjek goes into rich detail on rocketry and propulsion methods, including skyhooks and railguns to fling things into orbit...He is a sensible skeptic, yet also convinced that, in the long run, our destiny is among the stars." -The Guardian "If the events of this year have had you daydreaming about abandoning the planet entirely, [Spacefarers] is a geekily pleasurable survey of the practicalities and challenges." -The Telegraph "The best book I've read on space exploration since Isaac Asimov." -Michael Shermer, publisher of Skeptic

This book seeks to present a new way of thinking about the interaction of gravitational fields with quantum systems. Despite the massive amounts of research and experimentation, the myriad meetings, seminars and conferences, all of the articles, treatises and books, and the seemingly endless theorization, quantization and just plain speculation that have been engaged in regarding our evolving understanding of the quantum world, that world remains an enigma, even to the experts. The usefulness of general relativity in this regard has proven to be imperfect at best, but there is a new approach. We do not simply have to accept the limitations of Einstein's most celebrated theorem in regard to quantum theory; we can also embrace them, and thereby utilize them, to reveal new facts about the behavior of quantum systems within inertial and gravitational fields, and therefore about the very structure of space-time at the quantum level. By taking existing knowledge of the essential functionality of spin (along with the careful identification of the omnipresent inertial effects) and applying it to the quantum world, the book gives the reader a much clearer picture of the difference between the classical and quantum behaviors of a particle, shows that Einstein's ideas may not be as incompatible within this realm as many have come to believe, sparks new revelations of the way in which gravity affects quantum systems and brings a new level of efficiency-quantum efficiency, if you will-to the study of gravitational theory.

Black holes present one of the most fascinating predictions of Einstein's general theory of relativity. There is strong evidence of their existence through observation of active galactic nuclei, including the centre of our galaxy, observations of gravitational waves, and others. There exists a large scientific literature on black holes, including many excellent textbooks at various levels. However, most of these steer clear from the mathematical niceties needed to make the theory of black holes a mathematical theory. Those which maintain a high mathematical standard are either focused on specific topics, or skip many details. The objective of this book is to fill this gap and present a detailed, mathematically oriented, extended introduction to the subject. The book provides a wide background to the current research on all mathematical aspects of the geometry of black hole spacetimes.

Accretion disks are ubiquitous in our universe, and produce intense brightening. How does the gas in the disk lose its angular momentum to release massive amounts of gravitational energy? This is one of the biggest open questions in astronomy. This book studies four types of newly detected outbursts in dwarf novae through optical observations and/or numerical simulations and puts forward physical interpretations of these outbursts on the basis of the disk instability model, the most plausible model for dwarf-nova outbursts. It demonstrates that the disk-instability model can explain rich variety in dwarf-nova outbursts if some new aspects are taken into account (e.g. the extremely slow growth of tidal instability and thermal instability in the disk misaligned against the binary orbital plane). Moreover, it shares valuable insights on the evolution of binary systems by finding period bouncers and dwarf novae with F-type companion stars, which are rare objects.

This thesis develops the dispersive optical model into a tool that allows for the assessment of the validity of nuclear reaction models, thereby generating unambiguous removal probabilities of nucleons from valence orbits using the electron-induced proton knockout reaction. These removal probabilities document the substantial quantitative degree in which nuclei deviate from the independent-particle model description. Another outcome reported within is the prediction for the neutron distribution of Ca-40, Ca-48, and Pb-208. The neutron radii of these nuclei have direct relevance for the understanding of neutron stars and are currently the subject of delicate experiments. Unlike other approaches, the current method is consistent with all other relevant data and describes nuclei beyond the independent-particle model. Finally, a new interpretation of the saturation probabilities of infinite nuclear matter is proposed suggesting that the semi-empirical mass formula must be supplemented with a better extrapolation from nuclei to infinite matter.

The origin of the solar system has been a matter of speculation for many centuries, and since the time of Newton it has been possible to apply scientific principles to the problem. A succession of theories, starting with that of Pierre Laplace in 1796, has gained general acceptance, only to fall from favor due to its contradiction in some basic scientific principle or new heavenly observation. Modern observations by spacecraft of the solar system, the stars, and extra-solar planetary systems continuously provide new information that may be helpful in finding a plausible theory as well as present new constraints for any such theory to satisfy.
The Origin and Evolution of the Solar System begins by describing historical (pre-1950) theories and illustrating why they became unacceptable. The main part of the book critically examines five extant theories, including the current paradigm, the solar nebula theory, to determine how well they fit with accepted scientific principles and observations. This analysis shows that the solar nebula theory satisfies the principles and observational constraints no better than its predecessors. The capture theory put forward by the author fares better and also indicates an initial scenario leading to a causal series of events that explain all the major features of the solar system.