Deze collectie duikt in de uitgestrektheid van de kosmos en biedt lezers een boeiende reis door astronomie en astrofysica. De serie verkent een breed scala aan onderwerpen, van planetenstelsels en hemelse fenomenen tot de fundamentele theorieën van het universum. Elk deel is zorgvuldig samengesteld om zowel diepgaand wetenschappelijk inzicht als meeslepende verhalen te bieden. Het is een essentiële bron voor iedereen die gefascineerd is door de mysteries van het universum en de wetenschap die probeert deze te ontrafelen.
In this third corrected and revised edition students and lecturers in astronomy and planetary science as well as planet observers will find a mine of up-to-date information on the solar system and its interaction with the interplanetary medium, its various objects, comparative planetology, discussion of questions for further research and future space exploration.
The Evolution from Optical to Radio Reference Frames
Celestial fundamental catalogues are a prerequisite for the determination of absolute positions and motions in space. Presently, positional astrometry is at the watershed between classical fundamental catalogues, based on moving reference stars, and modern catalogues, based on extragalactic reference objects with non-measurable motion. This book addresses the concepts and methods of the respective construction techniques leading to the stellar frame of the FK5 (fifth fundamental catalogue) and to the newly adopted extragalactic radio reference frame, ICRF (international celestial reference frame), with its extension to optical wavelengths by the Hipparcos Catalogue. While principal outlines of meridian circle observations are given, emphasis is put in some detail on the VLBI technique as applied to astrometry, and to the observational techniques used in the Hipparcos mission, including the tie of the originally non-anchored rigid Hipparcos sphere into the ICRF.
Devised for a quantitative understanding of the physics of the universe from the solar system through the milky way to clusters of galaxies all the way to cosmology, this acclaimed text offers among the most concise and most critical ones of extant works. Special chapters are devoted to magnetic and radiation processes, disks, black-hole candidacy, bipolar flows, cosmic rays, gamma-ray bursts, image distortions, and special sources. At the same time, planet earth is viewed as the arena for life, with plants and animals having evolved to homo sapiens during cosmic time. This text is unique in covering the basic qualitative and quantitative tools, formulae as well as numbers, needed to for the precise interpretation of frontline phenomena.
This classic text - aimed at senior undergraduates and beginning graduate students in physics and astronomy - presents a wide range of concepts in sufficient depth to give the reader a quantitative understanding of the subject. Emphasising physical concepts, it provides the student with a series of astrophysical sketches, concluding with a synthesis of all the subjects discussed in the book, sketching the history of the universe from its beginning to the formation of the Sun and the planets.
Focusing on the chemical evolution of various galaxy types—elliptical, spiral, and irregular—this book highlights the significance of star formation history in shaping star populations. It offers a comprehensive comparison of theoretical models against two decades of observational data, providing insights into the intricate processes governing galaxy development and composition.
Kenneth Lang's classic work Astrophysical Formulae. (Vol. I and II) is now available as soft cover edition in a set. This volume is a reference source of fundamental formulae in physics and astrophysics. In contrast to most of the usual compendia it carefully explains the physical assumptions entering the formulae. All the important results of physical theories are covered: electrodynamics, hydrodynamics, general relativity, atomic and nuclear physics, and so on. Over 2100 formulae are included, and the original papers for the formulae are cited together with papers on modern applications in a bibliography of over 1900 entries. For the third edition (first published in 1999), a chapter on space, time, matter and cosmology had been included and the other chapters carefully revised.
Stellar Physics is a rather unique book among the growing literature on star formation and evolution. Not only does the author, a leading expert in the field, give a very thorough description of the current knowledge about stellar physics but he handles with equal care the many problems that this field of research still faces. A bibliography with well over 650 entries makes this book an unparalleled source of references. Fundamental Concepts and Stellar Equilibrium is the first of two volumes, and can be read, as can the second volume, as an independent work. It provides an extensive introduction into all physical processes that play a role in star formation and evolution. The basic equations describing stellar equilibrium are discussed, where attention is paid to both the theoretical and the numerical aspects.
This volume is concerned essentially with the modern developments in reflecting telescope optics. In the last twenty years, modern technology has revolutionized not only manufacturing and test procedures but also the whole area of quality specification with the introduction of active control into the functioning telescope. Other subjects covered here are alignment of telescope optics, atmospheric optics, including adaptive optics, reflecting coatings and ancillary equipment (adapters and baffles). Although an independent work, Vol. II is heavily cross-referenced with Vol. I. It is richly illustrated and gives, together with Vol. I, the most complete list of references available; it can also therefore be regarded as a source book.
The?rsteditionofthistextappearedin1994.Shortlyafterthethirdprinting, our editor suggested that we attempt a second edition because new devel- mentsinstellarstructureandevolutionhadmadeouroriginalworkoutdated. We (the original authors, CJH and SDK) reluctantly agreed but with res- vations due to the e?ort involved. Our initial reluctance disappeared when we were able to convince (cajole, twist the arm of, etc.) our new coauth- colleague Virginia Trimble to join us. (Welcome Virginia!) We (i.e., all three of us) hope that you agree that the present edition is a great improvement compared to the 1994 e?ort. Our objectives in this edition are the same ones we set forth in 1994: Whatyouwill?ndisatextdesignedforourtargetaudience:thety- cal senior undergraduate or beginning graduate student in astronomy or astrophysics who wishes an overview of stellar structure and e- lution with just enough detail to understand the general picture. She or he can go on from there to more specialized texts or directly to the research literature depending on talent and interests. To this end, this text presents the basic physical principles without chasing all the (interesting!) details. For those of you familiar with the ?rst edition, you will ?nd that some things have not been changed substantially (F = ma is still F = ma), while othersde?nitelyhave.Forexample,Chapter2hasbeencompletelyrewritten.
Neutron stars are the smallest dense stars known, with densities some 1014 times that of Earth. This text discusses the physics of these extreme objects and includes the needed background in classical general relativity in nuclear and particle physics.
High-redshift galaxies emerged as a distinct research field in the late 20th century, facilitated by the Lyman-break technique, which enabled the identification of significant samples, and the advent of 8 to 10-meter telescopes that provided quality spectroscopic data. Today, these galaxies represent a crucial topic in astrophysics, comprising 5–10% of publications in major astronomy journals. The rapid development of this field, coupled with the constant influx of new results, makes writing a comprehensive book challenging. However, the vast amount of existing research and the ongoing interest in high-redshift galaxies justify the need for a summary and evaluation of the available data. This serves as an introduction for newcomers or those interested in the findings. The end of the first decade of the 21st century is an opportune moment for such a summary, as the current generation of ground-based optical telescopes, the Hubble Space Telescope, and key large radio telescopes have been operational for about one to two decades. While these instruments will continue to yield significant scientific results, many initial programs that utilized their unique capabilities have now been completed.
Focusing on the formulation of mathematical models, this book delves into the light curves of eclipsing binary stars and the algorithms used to create these models. The latest edition introduces new physics relevant to light curve modeling and distance fitting, along with fresh applications and updated references, enhancing its relevance for researchers in the field.
G. Beutler's Methods of Celestial Mechanics is a coherent textbook for students as well as an excellent reference for practitioners. The first volume gives a thorough treatment of celestial mechanics and presents all the necessary mathematical details that a professional would need. The reader will appreciate the well-written chapters on numerical solution techniques for ordinary differential equations, as well as that on orbit determination. In the second volume applications to the rotation of earth and moon, to artificial earth satellites and to the planetary system are presented. The author addresses all aspects that are of importance in high-tech applications, such as the detailed gravitational fields of all planets and the earth, the oblateness of the earth, the radiation pressure and the atmospheric drag. The concluding part of this monumental treatise explains and details state-of-the-art professional and thoroughly-tested software for celestial mechanics. The CD-ROM accompanying Volume II enables readers to employ this software themselves and also serves as to illustrate and reinforce the related theoretical concepts.
Over the past ten years, the discovery of extrasolar planets has opened a new field of astronomy, and this area of research is rapidly growing, from both the observational and theoretical point of view. The presence of many giant exoplanets in the close vicinity of their star shows that these newly discovered planetary systems are very different from the solar system. New theoretical models are being developed in order to understand their formation scenarios, and new observational methods are being implemented to increase the sensitivity of exoplanet detections. In the present book, the authors address the question of planetary systems from all aspects. Starting from the facts (the detection of more than 300 extraterrestrial planets), they first describe the various methods used for these discoveries and propose a synthetic analysis of their global properties. They then consider the observations of young stars and circumstellar disks and address the case of the solar system as a specific example, different from the newly discovered systems. Then the study of planetary systems and of exoplanets is presented from a more theoretical point of view. The book ends with an outlook to future astronomical projects, and a description of the search for life on exoplanets. This book addresses students and researchers who wish to better understand this newly expanding field of research.
This fourth edition of the book offers a comprehensive review of advancements in cosmology over the last fourteen years. It features newly written chapters on the standard model, quantum field theory implications, and structure formation. Emphasis is placed on recent observations, particularly of cosmic microwave background anisotropies.
In the first part, the book gives an up-to-date summary of the observational data. In the second part, it deals with the kinetic description of cosmic ray plasma. The underlying diffusion-convection transport equation, which governs the coupling between cosmic rays and the background plasma, is derived and analyzed in detail. In the third part, several applications of the solutions of the transport equation are presented and how key observations in cosmic ray physics can be accounted for is demonstrated.
Concerned with the theory and history of reflecting telescope optics, this volume comprises contributions from specialists in this field, working both in the astronomical community and in industry. The text covers subjects including practical alignment, test techniques and maintenance.
Starburst regions in galaxies significantly enhance our understanding of the early universe. This updated edition of Norbert Schulz’s book explores the complex physical processes involved in star creation and early evolution. It highlights how these processes manifest across various wavelengths, from radio to high-energy X-rays and gamma rays, with a focus on high-energy signatures. Key analysis techniques are discussed, showcasing modern research methods in the field. New chapters cover massive star formation, proto-planetary disks, and observations of young exoplanets. Recent advancements and contemporary research on star formation theory are presented, alongside new observations from the Spitzer Space Telescope, Hubble Space Telescope, and Chandra X-Ray Observatory, which collectively enhance high-resolution space-based observations. The inclusion of chapters on proto-planetary disks and young exoplanets reflects the evolving landscape of the subject. Enhanced with numerous color images, the book illustrates both established and emerging topics. The author updates theories on fragmentation, dust, and circumstellar disks, while placing a stronger emphasis on computational approaches, targeting graduate students and young researchers.
Theory of Orbits treats celestial mechanics as well as stellar dynamics from the common point of view of orbit theory, making use of concepts and techniques from modern geometric mechanics. It starts with elementary Newtonian mechanics and ends with the dynamics of chaotic motion. The two volumes are meant for students in astronomy and physics alike. Prerequisite is a physicist's knowledge of calculus and differential geometry.
Physics of Planetary Rings describes striking structures of the planetary rings of Saturn, Uranus, Jupiter, and Neptune: Narrow ringlets, spiral waves, and a chain of clumps. The author has contributed essential ideas to the full understanding of planetary rings via the stability analysis of dynamical systems. The combination of a high-quality description, the set of interesting illustrations, as well as the fascinating and natural presentation will make this book of considerable interest to astronomers, physicists, and mathematicians as well as students. There is no competing text for this book so far.
This book deals with stars during a short episode before they undergo a ma jor, and fatal, transition. Soon the star will stop releasing nudear energy, it will become a planetary nebula for abrief but poetic moment, and then it will turn into a white dwarf and slowly fade out of sight. Just before this dramatic change begins the star has reached the highest luminosity and the largest diameter in its existence, and while it is a star detectable in galaxies beyond the Local Group, its structure contains already the inconspicuous white dwarf it will become. It is called an "asymptotic giant branch star" or "AGB star". Over the last 30 odd years AGB stars have become a topic of their own although individual members of this dass had already been studied for cen turies without realizing what they were. In the early evolution, so called "E-AGB"-phase, the stars are a bit bluer than, but otherwise very similar to, what are now called red giant branch stars (RGB stars). It is only in the sec ond half of their anyhow brief existence that AGB stars differ fundamentally from RGB stars.
G. Beutler's Methods of Celestial Mechanics is a coherent textbook for students as well as an excellent reference for practitioners. The first volume gives a thorough treatment of celestial mechanics and presents all the necessary mathematical details that a professional would need. The reader will appreciate the well-written chapters on numerical solution techniques for ordinary differential equations, as well as that on orbit determination. In the second volume applications to the rotation of earth and moon, to artificial earth satellites and to the planetary system are presented. The author addresses all aspects that are of importance in high-tech applications, such as the detailed gravitational fields of all planets and the earth, the oblateness of the earth, the radiation pressure and the atmospheric drag. The concluding part of this monumental treatise explains and details state-of-the-art professional and thoroughly-tested software for celestial mechanics.
, This is the updated, widely revised, restructured and expanded third edition of Léna et al.'s successful work Observational Astrophysics. It presents a synthesis on tools and methods of observational astrophysics of the early 21st century. Written specifically for astrophysicists and graduate students, this textbook focuses on fundamental and sometimes practical limitations on the ultimate performance that an astronomical system may reach, rather than presenting particular systems in detail. In little more than a decade there has been extraordinary progress in imaging and detection technologies, in the fields of adaptive optics, optical interferometry, in the sub-millimetre waveband, observation of neutrinos, discovery of exoplanets, to name but a few examples. The work deals with ground-based and space-based astronomy and their respective fields. And it also presents the ambitious concepts behind space missions aimed for the next decades. Avoiding particulars, it covers the whole of the electromagnetic spectrum, and provides an introduction to the new forms of astronomy becoming possible with gravitational waves and neutrinos. It also treats numerical aspects of observational astrophysics: signal processing, astronomical databases and virtual observatories.
A wealth of new experimental and theoretical results has been obtained in solar physics since the first edition of this textbook appeared in 1989. Thus all nine chapters have been thoroughly revised, and about 100 pages and many new illustrations have been added to the text. The additions include element diffusion in the solar interior, the recent neutrino experiments, methods of image restoration, observational devices used for spectroscopy and polarimetry, and new developments in helioseismology and numerical simulation. The book takes particular advantage of the results of several recent space missions, which lead to substantial progress in our understanding of the Sun, from the deep interior to the corona and solar wind.
G. Beutler's Methods of Celestial Mechanics is a coherent textbook for students as well as an excellent reference for practitioners. The first volume gives a thorough treatment of celestial mechanics and presents all the necessary mathematical details that a professional would need. The reader will appreciate the well-written chapters on numerical solution techniques for ordinary differential equations, as well as that on orbit determination. In the second volume applications to the rotation of earth and moon, to artificial earth satellites and to the planetary system are presented. The author addresses all aspects that are of importance in high-tech applications, such as the detailed gravitational fields of all planets and the earth, the oblateness of the earth, the radiation pressure and the atmospheric drag. The concluding part of this monumental treatise explains and details state-of-the-art professional and thoroughly-tested software for celestial mechanics.
This textbook addresses students and practitioners. It attempts to give an outline of the methods and tools of radio astronomy needed by the astronomer who wants to relate the message from interstellar space to physical processes. It gives a unified treatment of the entire field of radioastronomy from the centimetre to the sub-millimetre wavelength range, discussing both single telescopes and interferometric devices. It describes the basic physical principles and gives a reasonably complete outline of the instruments and methods of measurements and analysis, including both continuum radiation and spectral lines. This second edition has been largely rewritten and expanded. It includes the most recent developments in astronomy.
This book effectively combines Special and General Relativity with key elements of nuclear and particle physics. It includes problem sets for various chapters, making it suitable for courses focused on the physics of white dwarf and neutron star interiors.
This book provides astronomers with a guide to specifying an astrophysical model for a set of observations, selecting an algorithm to determine the parameters of the model, and estimating the errors of the parameters.
This book explores the evolution of Dynamical Astronomy, highlighting key texts on Celestial Mechanics and Stellar Dynamics. It discusses notable works such as Chandrasekhar's "Principles of Stellar Dynamics" and Binney and Tremaine's "Galactic Dynamics," emphasizing the impact of chaos theory on the field.
Numerous books on Dynamical Astronomy exist, focusing on Celestial Mechanics, Stellar Dynamics, and Galactic Dynamics. Early works on stellar dynamics primarily addressed the statistics of stellar motions, such as Smart's "Stellar Dynamics" (1938) and Trumpler and Weaver's "Statistical Astronomy" (1953). Chandrasekhar's "Principles of Stellar Dynamics" (1942) is a significant contribution, emphasizing relaxation times, Liouville's equation, and cluster dynamics. The 1960 Dover edition included a modern Appendix on the statistical mechanics of stellar systems. For classroom use, Mihalas and Routly's "Galactic Astronomy" (1969) served as a key resource. The most comprehensive work in the field is Binney and Tremaine's "Galactic Dynamics" (1987), which covers classical stellar dynamics and contemporary topics. Another notable reference is Hagihara's extensive 4-volume treatise "Celestial Mechanics" (1970-1975). Recently, advancements in the theory of chaos have emerged as a vital area of interest, significantly impacting stellar and galactic dynamics. The exploration of order and chaos has introduced a new dimension to the study of dynamics.
On the occasion ofthe second edition ofthe book, it appeared necessary to up date information that was already seven years old. Astrometry has recorded tremendous advances during these last years, so that, in addition to cor recting identified errors and misprints, there are many major modifications. Among the events that forced me to modify significantly the contents of the book, the most important are the release of the Hipparcos and Tycho cata logues, the introduction of CCD astrometry, the decision of the International Astronomical Union to adopt a new celestial reference frame, the dramatic improvement of accurate time and frequency standards, the decision taken by space agencies to prepare several new space astrometry satellites and the development of optical interferometry. The description and the consequences of these events have been included in this edition. One of them is that a mi crosecond of arc or microarcsecond (uas) has become a widely used unit. On the contrary, the result was also that the importance of some in struments such as astrolabes or transit circles has decreased. However, I left but because their description unchanged, not only for their historical interest, newer techniques often use similar data reduction methods so that one can refer to them. Conversely, some methods or instruments have evolved and new information is included. Finally, many new references were added to the original list.
For about half a century the general theory of relativity attracted little attention from physicists. However, the discovery of compact objects such as quasars and pulsars, as well as candidates for black holes on the one hand, and the microwave background radiation on the other hand completely changed the picture. In addition, developments in elementary particle physics, such as predictions of the behavior of matter at the ultrahigh energies that might have prevailed in the early stages of the big bang, have greatly en hanced the interest in general relativity. These developments created a large body of readers interested in general relativity, and its applications in astrophysics and cosmology. Having neither the time nor the inclination to delve deeply into the technical literature, such readers need a general introduction to the subject before exploring applica tions. It is for these readers that the present volume is intended. Keeping in mind the broad range of interests and wanting to avoid mathematical compli cations as much as possible, we have ventured to combine all three topics relativity, astrophysics, and cosmology-in a single volume. Naturally, we had to make a careful selection of topics to be discussed in order to keep the book to a manageable length.
In this corrected and enlarged edition of Börner's well respected textbook, you will find an up-to-date account of the interplay between particle physics and astrophysics upon which modern cosmology is founded. The author describes some of the theories which have been developed to model the fundamental interaction of elementary particles in the extremely high temperatures of the early universe, taking care to distinguish facts and well- established results from hypotheses and speculations. The three parts of the book discuss the standard hot big bang model of the early universe, the basic ideas of the standard and the grand unified theories of elementary particles, and the influence of dark matter of the large- scale evolution of structure. In addition to making some minor corrections, the author has added an appendix presenting new results and an updated bibliography. Two main groups of readers are research students in astronomy can use this book to understand the impact of elementary particle theory on cosmology, while research students in particle physics can use it to acquaint themselves with the basic facts of cosmology. The book is written carefully enough to appeal also to a wider audience of physicists.
S. Chandrasekhar's influential work presents stellar dynamics as a branch of classical dynamics, akin to celestial mechanics. It explores the evolution of stellar dynamics through three main perspectives: celestial mechanics, fluid mechanics, and statistical mechanics, addressing complex problems in interpreting stellar systems.
In the last 45 years, X-ray astronomy has become an integral part of modern astrophysics and cosmology. There is a wide range of astrophysical objects and phenomena, where X-rays provide crucial diagnostics. In particular they are well suited to study hot plasmas and matter under extreme physical conditions in compact objects. This book summarizes the present status of X-ray astronomy in terms of observational results and their astrophysical interpretation. It is written for students, astrophysicists as well a growing community of physicists interested in the field. An introduction including historical material is followed by chapters on X-ray astronomical instrumentation. The next two parts summarize in 17 chapters the present knowledge on various classes of X-ray sources in the galactic and extragalactic realm. While the X-ray astronomical highlights discussed in this book are mainly based on results from ROSAT, ASCA, RXTE, BeppoSAX, Chandra and XMM-Newton, a final chapter provides an outlook on observational capabilities and projects discussed for the future.
Half a century ago, S. Chandrasekhar wrote these words in the preface to his l celebrated and successful In this monograph an attempt has been made to present the theory of stellar dy namics as a branch of classical dynamics - a discipline in the same general category as celestial mechanics. [ ... J Indeed, several of the problems of modern stellar dy namical theory are so severely classical that it is difficult to believe that they are not already discussed, for example, in Jacobi's Vorlesungen. Since then, stellar dynamics has developed in several directions and at var ious levels, basically three viewpoints remaining from which to look at the problems encountered in the interpretation of the phenomenology. Roughly speaking, we can say that a stellar system (cluster, galaxy, etc.) can be con sidered from the point of view of celestial mechanics (the N-body problem with N » 1), fluid mechanics (the system is represented by a material con tinuum), or statistical mechanics (one defines a distribution function for the positions and the states of motion of the components of the system).
Light observed from distant objects is found to be deflected by the gravitational field of massive objects near the line of sight - an effect predicted by Einstein in his first paper setting forth the general theory of relativity, and confirmed by Eddington soon afterwards. If the source of the light is sufficiently distant and bright, and if the intervening object is massive enough and near enough to the line of sight, the gravitational field acts like a lens, focusing the light and producing one or more bright images of the source. This book, by renowned researchers in the field, begins by discussing the basic physics behind gravitational lenses: the optics of curved space-time. It then derives the appropriate equations for predicting the properties of these lenses. In addition, it presents up-to-date observational evidence for gravitational lenses and describes the particular properties of the observed cases. The authors also discuss applications of the results to problems in cosmology.
Written by a well-known astrophysicist, who is also a superbly talented writer, this work deals with the matter and radiation content of the universe, the formation of galaxies, and provides a comprehensive introduction into relativistic astrophysics as needed for the clarification of cosmological ideas.
Compact objects are a crucial focus in contemporary astronomical research. Supermassive black holes are key to understanding galaxy formation in the early Universe, while old white dwarfs serve as benchmarks for determining the Universe's age. Mergers of neutron stars and black holes generate intense gravitational waves, which will soon be measured by upcoming detectors. This work provides a thorough introduction and current overview of the physical processes governing these objects, encompassing everything from foundational concepts to the latest findings and observations. It begins with a classification of compact objects, followed by essential principles of general relativity. The author delves into the physics and observations of white dwarfs and neutron stars, presenting the latest equations of state for neutron star matter, and explores the gravitational fields of rapidly rotating compact objects and black holes, including ray tracing and magnetospheres. Additionally, the text covers gravitational waves and new insights into accretion processes through magnetorotational instability in accretion disks. Utilizing a 3+1 split approach to Einstein's equations and relativistic hydrodynamics, each chapter includes problems and solutions to enhance comprehension. This advanced textbook will be valuable for both students and researchers in the field of astrophysics.
The updated textbook incorporates significant advancements in solar physics since its 1989 edition, featuring nine revised chapters with an additional 100 pages and numerous new illustrations. Key topics include element diffusion in the solar interior, recent neutrino experiments, and innovative observational techniques for spectroscopy and polarimetry. It also highlights breakthroughs in helioseismology and numerical simulations, leveraging findings from recent space missions to enhance understanding of the Sun, from its core to the corona and solar wind.
Our purpose in writing this book is to show how physics has been applied to developing our current understanding of the phase structure, physical condi tions, chemical makeup and, evolution of the (thermal) interstellar medium. We hope it provides an up-to-date overview which postgraduates, advanced undergraduates, and professionals in astrophysics can use as a „reference of first resort“ before going on to read the more specialist monographs or research literature. We have covered the exciting observational results, but without consideration of the experimental techniques or instruments required. An elementary understanding of mathematical physics and of quantum me chanics has been assumed, and a knowledge of basic astrophysics would be helpful. Older textbooks on interstellar physics have tended to develop the subject matter in an order which reflects the historical development of the field. Here a more pedagological approach has been adopted, based on our lecture course experience. We cover successively more complex physical systems found in the diffuse universe. Detailed mathematical rigour is eschewed in favour of provid ing the reader with a basic physical insight into these systems. Astrophysical problems are treated as practical applications of the physics. In practice, the material is generally ranked in order of decreasing entropy, since the hottest and most diffuse phases tend to be physically less complex.
This long-awaited second edition of the classical textbook on Stellar Structure and Evolution by Kippenhahn and Weigert is a thoroughly revised version of the original text. Taking into account modern observational constraints as well as additional physical effects such as mass loss and diffusion, Achim Weiss and Rudolf Kippenhahn have succeeded in bringing the book up to the state-of-the-art with respect to both the presentation of stellar physics and the presentation and interpretation of current sophisticated stellar models. The well-received and proven pedagogical approach of the first edition has been retained. The book provides a comprehensive treatment of the physics of the stellar interior and the underlying fundamental processes and parameters. The models developed to explain the stability, dynamics and evolution of the stars are presented and great care is taken to detail the various stages in a star’s life. Just as the first edition, which remained astandard work for more than 20 years after its first publication, the second edition will be of lasting value not only for students but also for active researchers in astronomy and astrophysics.
Using information and scale as central themes, this comprehensive survey explains how to handle real problems in astronomical data analysis through a modern arsenal of powerful techniques. The coverage includes chapters or appendices on: detection and filtering; image compression; multichannel, multiscale, and catalog data analytical methods; wavelets transforms, Picard iteration, and software tools.
Unique in its breadth of coverage and level of presentation, this revised textbook provides more on the nature of galaxies, extragalactic objects, the large-scale structure of the Universe, and cosmology than is available in general textbooks on astronomy. It remains, however, accessible to advanced undergraduate students. One or more chapters are devoted to each of the following: the classification and morphology of galaxies; the galactic interstellar medium; galactic kinematics; elliptical, spiral, and barred spiral galaxies; the interactions between galaxies; extragalactic radio sources, quasars and their line spectra, and other active galactic nuclei; the formation of galaxies; the Universe as a whole; and cosmology.
A comprehensive account of solar astrophysics and how our perception and knowledge of this star have gradually changed as mankind has elucidated ever more of its mysteries. The emphasis here is on the last decade, which has seen three successful solar spacecraft missions: SOHO, Ulysses and Yohkoh. Together, these have confirmed many aspects of the solar standard model and provided new clues to the numerous open questions that remain. The author, a leading researcher in the field, writes in a clear and concise style. Known also for his famous books „Astrophysical Formulae“, „Sun, Earth and Sky“ and the prize-winning „Wanderers in Space“, he has succeeded once again in addressing a complex scientific topic in a very approachable way.
Rotation is ubiquitous at each step of stellar evolution, from star formation to the final stages, and it affects the course of evolution, the timescales and nucleosynthesis. Stellar rotation is also an essential prerequisite for the occurrence of Gamma-Ray Bursts. In this book the author thoroughly examines the basic mechanical and thermal effects of rotation, their influence on mass loss by stellar winds, the effects of differential rotation and its associated instabilities, the relation with magnetic fields and the evolution of the internal and surface rotation. Further, he discusses the numerous observational signatures of rotational effects obtained from spectroscopy and interferometric observations, as well as from chemical abundance determinations, helioseismology and asteroseismology, etc. On an introductory level, this book presents in a didactical way the basic concepts of stellar structure and evolution in „track 1“ chapters. The other more specialized chapters form an advanced course on the graduate level and will further serve as a valuable reference work for professional astrophysicists.
Describing interstellar matter in our galaxy in all of its various forms, this book also considers the physical and chemical processes that are occurring within this matter. The first seven chapters present the various components making up the interstellar matter and detail the ways that we are able to study them. The following seven chapters are devoted to the physical, chemical and dynamical processes that control the behaviour of interstellar matter. These include the instabilities and cloud collapse processes that lead to the formation of stars. The last chapter summarizes the transformations that can occur between the different phases of the interstellar medium. Emphasizing methods over results, The Interstellar Medium is written for graduate students, for young astronomers, and also for any researchers who have developed an interest in the interstellar medium.
Relativistic Astrophysics and Cosmology provides a comprehensive overview of general relativity and its applications to compact objects, gravitational waves, and cosmology. It balances theoretical concepts with observational discussions and includes 140 exercises. Ideal for advanced undergraduates and beginning graduate students in (astro)physics.
Focusing on the intricate processes of star formation, this book explores both theoretical and observational aspects, emphasizing current star formation in our galaxy due to the wealth of available data. It compares various star formation scenarios and delves into the fundamental physics behind each. The narrative tracks a star's journey from its inception in interstellar gas to its final equilibrium state, presenting robust evidence for the evolutionary path and highlighting methods for comparing theoretical predictions with observational findings.
Astronomical Optics and Elasticity Theory provides a very thorough and comprehensive account of what is known in this field. After an extensive introduction to optics and elasticity, the book discusses variable curvature and multimode deformable mirrors, as well as, in depth, active optics, its theory and applications. Further, optical design utilizing the Schmidt concept and various types of Schmidt correctors, as well as the elasticity theory of thin plates and shells are elaborated upon. Several active optics methods are developed for obtaining aberration corrected diffraction gratings. Further, a weakly conical shell theory of elasticity is elaborated for the aspherization of grazing incidence telescope mirrors.The very didactic and fairly easy-to-read presentation of the topic will enable PhD students and young researchers to actively participate in challenging astronomical optics and instrumentation projects.
Conceived more than six years ago, this book took much effort to develop, and several updates in parts of the book became necessary because significant ad vances in the field of Interplanetary Dust had occurred. Now, at the beginning of the new millennium, this book provides up-to-date coverage of all major aspects of dust in the Solar System. The volume is conceived as a source book for researchers in the field as well as a graduate-level textbook. In order to achieve the highest standard the individual chapters are written by experts in the field, preserving the somewhat different style and language of the sub-topic. The book follows the comprehensive review of the „Cosmic Dust“ field assembled by Tony McDonnell more than 20 years ago. That book covered dust in its various physical appearances as the common theme, but it described phenomena that appeared rather unrelated. The topics ranged from zodiacal light over lunar craters to dust particles collected in the atmosphere, from interstellar dust to comets, and from dust dynamics to laboratory simulation of dusty phenomena.
"Stellar Physics" is a rather unique book in the growing literature on star formation and evolution. Not only does the author, a leading expert in the field, give a very thorough description of the current knowledge about stellar physics, but he handles with equal care the many problems that this field of research still faces. A bibliography with well over 650 entries makes this book an unparalleled source of references. "Stellar Evolution and Stability" is the second volume and can be read, as can the first volume, as a largely independent work. It traces in great detail the evolution of the protostar towards the main sequence and beyond this to the last stage of stellar evolution, with the corresponding vast range from white dwarfs to the mighty supernovae explosions and blackhole formation. The book concludes with special chapters on the dynamical, thermal and pulsing stability of stars.
Planetary nebulae are a classic subject in astrophysics, encompassing various physical processes in highly ionized gaseous media. These include the formation of emission lines under specific conditions and continuous emissions ranging from far ultraviolet to infrared and radio frequencies. The generation of exotic radiation forms predicted by atomic physics, along with methods for analyzing observed spectra and detecting physical and kinematic parameters of the radiating medium, are foundational to the physical theory of gaseous nebulae. This knowledge is crucial for understanding the diverse processes in the Universe, including those in gaseous envelopes around stars of different classes, stellar chromospheres and coronae, unstable stars, circumstellar clouds, and shells formed in nova and supernova explosions. It also applies to diffuse nebulae, the interstellar medium, interacting binary systems, emission-line galaxies, and quasars. Over the last thirty years, significant advancements have been made in understanding the nature of planetary nebulae. Notably, the discovery of radio emissions from PNs, predicted theoretically, and the unexpected powerful infrared emissions in both the continuum and emission lines have marked a turning point in this field.
Gamma-ray astronomy began in the mid-1960s with balloon satellite, and, at very high photon energies, also with ground-based instruments. However, the most significant progress was made in the last decade of the 20th century, when the tree satellite missions SIGMA, Compton, and Beppo-Sax gave a completely new picture of our Universe and made gamma-ray astronomy an integral part of astronomical research. This book, written by well-known experts, gives the first comprehensive presentation of this field of research, addressing both graduate students and researchers. Gamma-ray astronomy helps us to understand the most energetic processes and the most violent events in the Universe. After describing cosmic gamma-ray production and absorption, the instrumentation used in gamma-ray astronomy is explained. The main part of the book deals with astronomical results, including the somewhat surprising result that the gamma-ray sky is continuously changing.