Nanodust and nanometer-sized structures are important components of many objects in space. Nanodust is observed in evolved stars, young stellar objects, protoplanetary disks, and dust debris disks. Within the solar system, nanodust is observed with in-situ experiments from spacecraft. Nanometer-sized substructures are found in the collected cometary and interplanetary dust particles and in meteorites. Understanding the growth and destruction of dust, its internal evolution, as well as the optical properties and the detection of nanoparticles is of fundamental importance for astrophysical research. This book provides a focused description of the current state of research and experimental results concerning nanodust in the solar system. It addresses three major questions: What is nanodust? How was it discovered in the solar system? And how do we interpret the observations? The book serves as a self-contained reference work for space researchers and provides solid information on nanodust in cosmic environments for researchers working in astrophysics or in other fields of physics.

The knowledge of the amount and nature of matter present in the Universe is undoubtedly one of the most relevant topics in astrophysics and cosmology. It started with the pioneering work of Zwicky in 1933, who found the need for a large amount of dark matter in the Coma cluster. An important step has been the recent finding through the observation of distant type Ia supernovae of the presence of a significant vacuum energy density causing an accelerating expansion of the Universe. Nevertheless, the nature of most of the matter in the Universe is still unknown. Its solution requires the interplay of several fields of astrophysics and cosmology as well as particle physics, all of which are covered in this volume: Cosmic Microwave Background radiation, large scale structures, galaxy clusters, intergalactic absorption, dark matter components of galaxies, globular clusters, supernovae of type Ia distance measurements, gravitational lensing, X-ray observations, Lyman-alpha observations, dark energy, direct detection of weakly interacting massive particles (WIMPS), detection of neutrino oscillations, particle candidates for dark matter, and Big Bang nucleosynthesis of baryonic matter.

Therefore, this volume presents a very useful synopsis of all constituents of matter in the Universe.

The book reviews methods for the numerical and statistical analysis of astronomical datasets with particular emphasis on the very large databases that arise from both existing and forthcoming projects, as well as current large-scale computer simulation studies. Leading experts give overviews of cutting-edge methods applicable in the area of astronomical data mining. Case studies demonstrate the interplay between these techniques and interesting astronomical problems. The book demonstrates specific new methods for storing, accessing, reducing, analysing, describing and visualising astronomical data which are necessary to fully exploit its potential.

The continuing success of helio- and asteroseismology in studying the internal structure and dynamics of the Sun, and of other single stars, has been highlighted in recent years by many topical meetings. The present Proceedings document the first Seismology symposium ever held in conjunction with an IAU General Assembly. This substantially influenced the layout of the scientific programme and demonstrates the vitality of this field of astronomy. The invited reviews are intended to address an audience that includes many non-specialists. Therefore, this volume is particularly valuable as an introduction to the general concepts of the field, and for conveying the excitement that comes with discussions of the most recent observational and theoretical results. There are two chapters on the many facets of asteroseismology, which also compare solar and stellar achievements. A major focus of the symposium was the new developments resulting from the observations of unprecedented quality obtained from global multi-site networks, and especially from the Solar and Heliospheric Observatory SoHO, currently continuing its observations from the Lagrangian point L1. From the center of the Sun to its outer layers, the reader will learn how modern diagnostic techniques reveal the inextricable links between the complex structure of the interior and atmosphere of our nearest star. The book is recommended for undergraduates, postgraduates, and professionals with a strong interest in modern developments in astrophysics.

A few years ago, a real break-through happened in observational astronomy: the un derstanding of the effect of atmospheric turbulence on the structure of stellar images, and of ways to overcome this dramatic degradation. This opened a route to diffraction-limited observations with large telescopes in the optical domain. Soon, the first applications of this new technique led to some outstanding astrophysical results, both at visible and infrared wavelengths. Yet, the potential of interferometric observations is not fully foreseeable as the first long-baseline arrays of large optical telescopes are being built or cOIIllnissioned right now. In this respect a comparison with the evolution of radio-astronomy is tempting. From a situation where, in spite of the construction of giant antennas, low angular resolution was prevailing, the introduction of long baseline and very long baseline interferometry and the rapid mastering of sophisticated image reconstruction techniques, have brought on a nearly routine basis high dynamic range images with milliarcseconds resolution. This, of course, has completely changed our views of the radio sky."

Astronomical photographs contain an enormous amount of information. This presents extremely interesting problems when one wishes to produce digitized sky atlases, to archive the digitized material, to develop sophisticated devices to do the digitizing, and to create software to process the vast amounts of data. All these activities are necessary to be able to carry out astronomy work. One such activity is the important, large-scale optical identification of objects which also emit radiation at other wavelengths. Other activities of the past decade include a multiplicity of surveys that have been made on galaxies and clusters of galaxies. This book treats, in five sections, the existing and future surveys, their digitization and their impact on astronomy. It is designed to serve as a reference for people in the field and for those who wish to engage in using or producing sky surveys.

This textbook presents ultraviolet and X-ray astronomy, gamma-ray astronomy, cosmic ray astronomy, neutrino astronomy, and gravitational wave astronomy as distinct research areas, focusing on the astrophysics targets and the requirements with respect to instrumentation and observation methods. The purpose of the book is to bridge the gap between the reference books and the specialized literature. For each type of astronomy, the discussion proceeds from the orders of magnitude for observable quantities. The physical principles of photon and particle detectors are then addressed, and the specific telescopes and combinations of detectors, presented. Finally the instruments and their limits are discussed with a view to assisting readers in the planning and execution of observations. Astronomical observations with high-energy photons and particles represent the newest additions to multimessenger astronomy and this book will be of value to all with an interest in the field.

This monograph, unique in the literature, is the first to develop a mathematical theory of gravitational lensing. The theory applies to any finite number of deflector planes and highlights the distinctions between single and multiple plane lensing. Introductory material in Parts I and II present historical highlights and the astrophysical aspects of the subject. Among the lensing topics discussed are multiple quasars, giant luminous arcs, Einstein rings, the detection of dark matter and planets with lensing, time delays and the age of the universe (Hubble's constant), microlensing of stars and quasars. The main part of the book---Part III---employs the ideas and results of singularity theory to put gravitational lensing on a rigorous mathematical foundation and solve certain key lensing problems. Results are published here for the first time. Mathematical topics discussed: Morse theory, Whitney singularity theory, Thom catastrophe theory, Mather stability theory, Arnold singularity theory, and the Euler characteristic via projectivized rotation numbers. These tools are applied to the study of stable lens systems, local and global geometry of caustics, caustic metamorphoses, multiple lensed images, lensed image magnification, magnification cross sections, and lensing by singular and nonsingular deflectors. Examples, illustrations, bibliography and index make this a suitable text for an undergraduate/graduate course, seminar, or independent thesis project on gravitational lensing. The book is also an excellent reference text for professional mathematicians, mathematical physicists, astrophysicists, and physicists.

Neutron stars hold a central place in astrophysics, not only because they are made up of the most extreme states of the condensed matter, but also because they are, along with white dwarfs and black holes, one of the stable configurations that stars reach at the end of stellar evolution. Neutron stars posses the highest rotation rates and strongest magnetic fields among all stars. They radiate prolifically, in high energy electromagnetic radiation and in the radio band.

This book is devoted to the selected lectures presented in the 6th NATO-ASI series entitled "The Electromagnetic Spectrum of Neutron Stars" in Marmaris, Turkey, on 7-18 June 2004. This ASI is devoted to the spectral properties of neutron stars. Spectral observations of neutron stars help us to understand the magnetospheric emission processes of isolated radio pulsars and the emission processes of accreting neutron stars. This volume includes spectral information from the neutron stars in broadest sense, namely neutrino and gravitational radiation along with the electromagnetic spectrum. We believe that this volume can serve as graduate level of text including the broad range of properties of neutron stars.

This IAU Symposium brought together researchers who use CCDs and arrays, designers and manufacturers of CCDs and array mosaics, and those who write the software to control these devices and to reduce the large amounts of data contained in each frame. At the meeting such topics as plans for applying the new technology to the new large telescopes that have been built recently and those planned in the near future, new developments in infra-red arrays, advances and concerns with the use of CCDs in photometry and spectroscopy and the creation of large mosaics in photometry and spectroscopy, and the creation of large mosaics of chips which allow larger areas of the sky to be covered in a single frame were discussed. There were sessions devoted to the following topics: new developments in CCD technology; new developments in IR detector arrays; direct imaging with CCDs and other arrays; spectroscopy with CCDs and other arrays; and large field imaging with array mosaics. Scientific results of studies made with this technology were covered in the poster sessions. CCD and array detectors have become the detectors of choice at all the world's optical observatories. Such instruments on small university and college telescopes have turned these telescopes into instruments that can now do observations which in the past were done only on the largest telescopes. CCDs and arrays are known as "the people's detector" because of their ability to turn small telescopes into true research instruments. On large telescopes observations can be made of extremely faint and crowded objects that were impossible to observe before the advent of CCD and Array technology. The proceedings of this meeting should be useful to all those who are interested in the design, manufacture and use of CCDs and arrays for astronomical observations.

Chaos theory plays an important role in modern physics and related sciences, but -, the most important results so far have been obtained in the study of gravitational systems applied to celestial mechanics. The present set of lectures introduces the mathematical methods used in the theory of singularities in gravitational systems, reviews modeling techniques for the simulation of close encounters and presents the state of the art about the study of diffusion of comets, wandering asteroids, meteors and planetary ring particles. The book will be of use to researchers and graduate students alike.

The papers in this volume aim to represent the most up-to-date research contributions on the observations, theoretical interpretations, and empirical and physical models of variations observed in solar and stellar irradiances, as well as on Sun-climate connections. Both theoretical studies and irradiance observations show that the energy output of the Sun and solar-type stars varies, changing on time scales related to the short-term surface manifestations of solar/stellar magnetic activity as well as long-term modulations driven by processes in the interiors of the stars. Papers presented in this book point out that at the Earth these variations influence the terrestrial climate, radiative environment and upper atmospheric chemistry.

This book provides an exhaustive account of the origin and dynamics of cosmic rays. Divided into three parts, it first gives an up-to-date summary of the observational data, then -- in the following theory section -- 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. The applications include cosmic ray modulation, acceleration near shock waves and the galactic propagation of cosmic rays. While the book is primarily of interest to scientists working at the forefront of research, the very careful derivations and explanations make it suitable also as an introduction to the field of cosmic rays for graduate students.

Magnetized plasmas in the universe exhibit complex dynamical behavior over a huge range of scales. The fundamental mechanisms of energy transport, redistribution and conversion occur at multiple scales. The driving mechanisms often include energy accumulation, free-energy-excited relaxation processes, dissipation and self-organization. The plasma processes associated with energy conversion, transport and self-organization, such as magnetic reconnection, instabilities, linear and nonlinear waves, wave-particle interactions, dynamo processes, turbulence, heating, diffusion and convection represent fundamental physical effects. They demonstrate similar dynamical behavior in near-Earth space, on the Sun, in the heliosphere and in astrophysical environments. 'Multi-scale Dynamical Processes in Space and Astrophysical Plasmas' presents the proceedings of the International Astrophysics Forum Alpbach 2011. The contributions discuss the latest advances in the exploration of dynamical behavior in space plasmas environments, including comprehensive approaches to theoretical, experimental and numerical aspects. The book will appeal to researchers and students in the fields of physics, space and astrophysics, solar physics, geophysics and planetary science.

This volume contains the lectures presented at the first course of the Inter national School of Space Chemistry held in Erice (Sicily) from May 10 to May 20 at the 'E. Majorana Centre for Scientific Culture'. The course was attended by 57 participants from 11 countries. The recognition by Professor A. Zichichi that space chemistry is one of the important and rapidly growing scientific disciplines with many and varied appli cations provided the stimulation to initiate this new school. Historically, the study of chemistry in space had its major origins in comets, the solar nebula and circumstellar envelopes before the interstellar medium achieved its current prominence. A remarkably rapid development in interstellar chemistry was precipitated by the discovery of formaldehyde in the late 1960's made possible by the new radio observational techniques. A four atom molecule in interstellar space was indeed a surprise considering that only a short time ear lier there were still arguments about the existence of the simplest of all molecules - the hydrogen molecule. The application of ion-molecule reactions to interstellar cloud chemistry provided a rich variety of new possibilities which were, however, continuously under pressure to keep pace with radio-astronomical discoveries of more and more complex molecules."

The study of orbits in dynamical systems and the theory of order and chaos has progressed enormously over the last few decades. It thus became an essential tool in dynamical astronomy. The book is the first to provide a general overview of order and chaos in dynamical astronomy. The progress of the theory of chaos has a profound impact on galactic dynamics. It has even invaded celestial mechanics, since chaos was found in the solar system which in the past was considered as a prototype of order. The book provides a unifying approach to these topics from an author who has spent more than 50 years of research in the field. The first part treats order and chaos in general. The other two parts deal with order and chaos in galaxies and with other applications in dynamical astronomy, ranging from celestial mechanics to general relativity and cosmology. This book, addressing especially the astrophysics, is also written as a textbook on dynamical systems for students in physics.

Subrahmanyan Chandrasekhar - known simply as Chandra throughout the scientific world - has become a legendary figure for his prolific contributions to physics, astrophysics, and applied mathematics. Before his death in 1995, Chandra had forbidden a memorial of the conventional sort, celebrating his life. This book, which contains some thirty articles by his former students, his associates, and his colleagues, is in a sense a memorial volume. It says little about Chandra's great scientific achievements, but shows his human side and the various facets of his brilliant personality, his incredible memory, his wit, and the breadth of his knowledge of art, music, literature, and the humanities in general. The contributors to this highly interesting book are among the few who broke the seemingly forbidden barrier surrounding the very private Chandra and came to know him well in one context or another. They include Lalitha Chandrasekhar, Roger Penrose, Richard H Dalitz, J W Cronin, Robert G Sachs, Abhay Ashtekar, and Robert Wald.

The present 15th volume of the ISSI Space Science Series is devoted to Auroral Plasma Physics. The aurora is arguably the most intriguing phenomenon in space plasma physics. Not only is it the most spectacular manifestation of the Sun-Earth connection chain, but the underlying plasma processes are expected to be ubiqui- tous in the plasma universe. Recognizing the enormous progress made over the last decade in the understanding of the physics of the auroral acceleration processes, it seemed timely to write a comprehensive and integrated book on the subject. Re- cent advances concern the clarification of the nature of the acceleration process of the electrons that are responsible for the visible aurora, the recognition of the fundamental role of the large-scale current systems in organizing the auroral mor- phology, and of the interplay between particles and electromagnetic fields. The project began in March 1999, as a natural follow-up of the project on Magnetospheric Plasma Sources and Losses that resulted in volume 6 of this se- ries, with a planning meeting by a core-group that coordinated the project. The group consisted of J. E. Borovsky, Los Alamos National Laboratory; C. W. Carl- son, University of California, Berkeley; G. Haerendel, Max-Planck-Institut fur ex- traterrestrische Physik, Garching; B. Hultqvist, Swedish Intitute ofSpace Physics, H. E. J. Koskinen, Finnish Meteorological Institute, Helsinki; W. Lotko, Kiruna; Dartmouth College, Hanover, New Hampshire; K. A. Lynch, University of New Hampshire, Durham and G. Marklund, Royal Institute ofTechnology, Stockholm. G. Paschmann, ISSI, Bern, was the project leader.

Infrared astronomy has undergone an enormous revolution during the last decade. Despite the great technical difficulties of building detectors in a cryogenic environment, the scientific advances in infrared astronomy have been astounding. In the near future many more advances can be expected from still newer developments in telescope and detector designs. High quality detector arrays and passively cooled telescopes are very promising techniques for achieving considerably larger apertures. This volume contains the refereed papers from the workshop on 'Next Generation Infrared Observatory', dealing with all new aspects of future infrared telescopes.

The workshop "From Dust to Terrestrial Planets" was initiated by a working group of planetary scientists invited to ISSI by Johannes Geiss in November 1997. The group split to focus on three topics, one of which was the history of the early solar system, including the formation of the terrestrial planets in the inner solar system. Willy Benz, Gunter Lugmair, and Frank Podosek were invited to convene planetary scientists, astrophysicists, and cosmochemists to synthesize the current knowledge on the origin and evolution of our inner planetary system. The convenors raised the interest of scientists from all over the world in the detailed assessment of the available astronomical, chronological, geochemical and dynamical constraints of the first period of inner solar system evolution. In partic ular, this included appraisal of the newest results from astronomical observations by the Hubble Space Telescope, the Infrared Space Observatory, and other space and ground-based facilities of solar-like systems and nebular disks, possibly repre senting early stages of the solar accretion disk and planet formation. At the same time, the current models of the origin, evolution, transport, and accretion processes of circum stellar disks were presented. This included the new insights provided by the recent discovery of extrasolar giant planets, which were considered insofar as they are relevant to the overall dynamics of the inner part of the solar system.

Interesting and often unexpected achievements of the mechanics of space flight throw a new light onto several classical problems. The book 's emphasis is on analysis carried out on the level of graphs and drawings, and sometimes numbers, revealing the beauty of the research process leading to the results.

The Swiss Society for Astrophysics and Astronomy organizes each year in the late winter or early spring an advanced course. The format of the school is always iden tical: three leading lecturers are invited to cover the subject in nine or ten lectures each and to deliver a written version of their lecture notes. Lectures are held in the morning and late afternoon, thus leaving ample time for discussion and skiing. These arrangements prove very convivial and lead to an excellent atmosphere in which to learn exciting new subjects and establish contacts with colleagues. A wide variety of people attend the school, including many young students, mostly from Europe, and some experienced researchers. The 20th Advanced Course of the Swiss Society for Astrophysics and Astronomy took place in Les Diablerets from 1 to 6 April 1990. It was devoted to observational and theoretical aspects of active galactic nuclei. The previous advanced courses of the Swiss Society for Astrophysics and Astronomy have regularly taken place in Saas-Fee, a small resort in the Swiss Alps, hence the name "Saas-Fee" used to de scribe the courses and lecture notes. In the last three years, however, the course was organized in Leysin and in Les Diablerets, both also situated in the Swiss Alps."

At the opening of the "Third Meeting on Celestial Mechanics - CELMEC III", strong sensations hit our minds. The conference (18-22 June 2001) was being held in Villa Mondragone, a beautiful complex of buildings and gardens located within the township of Monte Porzio Catone, on the hills surrounding Rome. A former papal residence, the building has been recently restored by the University of Rome "Tor Vergata" to host academic activities and events. The conference room is called "Salone degli Svizzeri": here, Gregory XIII, on February 24, 1582, gave its sanction to the reform of the Julian calendar and declared officially in use the calendar still adopted nowadays. The magnificent high walls and tall ceiling strongly resounded, giving to our voice a peculiar Vatican sound, which took us by surprise. May be - we thought - a distant echo of the very words of Gregory XIII proclaiming the modem calendar was still haunting the room. Around us, in the audience, many countries were represented, thus indicating that the idea of putting together the three "souls" of modem Celestial Mechanics - perturbation theories, solar and stellar system studies, spaceflight dynamic- had been successful. CELMEC III is in fact the latest of a series of meetings (the first two editions took place in 1993 and 1997 in L' Aquila, Italy) whose aim is to establish a common ground among people working in Celestial Mechanics, yet belonging to different institutions such as universities, astronomical observatories, research institutes, space agencies and industries.