This beautifully structured book presents the essentials of William and Caroline Herschel's pioneering achievements in late 18th-century astronomy. Michael Hoskin shows that William Herschel was the first observational cosmologist and one of the first observers to attack the sidereal universe beyond the solar system: Herschel built instruments far better than any being used at the royal observatory. Aided by his sister Caroline, he commenced a great systematic survey that led to his discovery of Uranus in 1781. Unlike observers before him, whose telescopes did not reveal them as astronomical objects, Herschel did not ignore misty patches of light. Hoskins points out Herschel's achievement in surveying, cataloguing, and describing them as "nebulae" and even coming to the correct conclusion that their structure evolved over time, with Newton's gravity being the agent of change. Herschel's surveys established a new astronomy - looking at the universe rather than the planets! Michael Hoskin's account includes sketches and diagrams from Herschel's manuscripts in the Royal Astronomical Society Archives in which he attempts to delineate the structure of the Milky Way galaxy. While it is well-known that Herschel was a revolutionary in telescope design who constructed the world's largest telescopes, Hoskin also gives the full picture of the man as an entrepreneur who built and traded some 400 telescopes. Hoskin also pays close attention to the role of William's sister Caroline Herschel, who is usually portrayed as a "helpmate" to her brother. But in fact she became a significant astronomer in her own right. This book also offers a wealth of information of the wider Herschel family. It is enriched by a complete set of portraits of William and Caroline Herschel with an extensive set of images of their residences and closes with a charming appendix on how visitors to the Herschels recorded their encounters. William and Caroline Herschel - Pioneers in Late 18th-Century Astronomy will appeal to amateur astronomers and all those interested in popular astronomy. This book will rapidly establish itself as the primary introductory work for students, astronomers, and scholars working on the history of natural science in the late 18th century.

This collection of articles emerged from the Nobel Symposium 98 that celebrated the centenary of the Nobel Prize as well as the one of the famous Swedish astronomer Bertil Lindblad. Many outstanding scientists contributed to this unique review of the state of the art in barred galaxy research. Theoretical papers describe their evolution, the dynamics as well as fundamental physical effects near their nuclei. Other contributions cover numerical and observational aspects and thus represent a very active area in astrophysics. The centre of our galaxy was also amply dealt with. The collection addresses researchers as well as graduate students.

Intelligent information Retrieval comprehensively surveys scientific information retrieval, which is characterized by growing convergence of information expressed in varying complementary forms of data - textual, numerical, image, and graphics; by the fundamental transformation which the scientific library is currently being subjected to; and by computer networking which as become an essential element of the research fabric. Intelligent Information Retrieval addresses enabling technologies, so-called `wide area network resource discovery tools', and the state of the art in astronomy and other sciences. This work is essential reading for astronomers, scientists in related disciplines, and all those involved in information storage and retrieval.

The book contains the notes of the lectures presented by outstanding experts at the 7th EADN School on plasma astrophysics. It is an up-to-date review of a number of basic topics in the physics of cosmic plasmas. The subject is treated both from a theoretical point of view and from that of the observational and diagnostic tools that provide us with the physically relevant data. The reader will have at hands a comprehensive and rather complete presentation of the subject, thanks also to the parallel development of the theoretical and experimental aspects. The book addresses graduate students and researchers in different areas who want to have a rapid and up-to-date introduction to this subject.

The five lectures presented in this volume address very timely mathematical problems in relativity and cosmology. "Part I" is devoted to the initial value and evolution problems of the Einstein equations. Especially it deals with the Einstein-Yang-Mills-Boltzmann system, fluid models with finite or infinite conductivity, global evolution of a new (two-phase) model for gravitational collapse and the structure of maximal, asymptotically flat, vacuum solutions of the constraint equations which have the additional property of containing trapped surfaces. "Part II" focuses on geometrical-topological problems in relativity and cosmology: on the role of cosmic censorship for the global structure of the Einstein-Maxwell equations and on the mathematical structure of quantum conformal superspace.

Modern astronomy has been characterized by an enormous growth in data acquisition - from new technologies in telescopes, detectors, and computation. One can now compile catalogs of tens or hundreds of millions of stars or galaxies and databases from satellite-based observations are reaching terabit proportions. This wealth of data gives rise to statistical challenges not previously encountered in astronomy. This book is the result of a workshop held at Pennsylvania State University in August 1991 that brought together leading astronomers and statisticians to consider statistical challenges encountered in modern astronomical research. The chapters have all been thoroughly revised in the light of the discussions at the conference, and some of the lively discussion is recorded here as well.

Several decades have elapsed since the publication of any similar book in the German language. The lack of such a book has been felt keenly by all friends of astronomy. In our space age, astronomical knowledge arouses public interest more and more. Practical observation at the telescope depends more than anything else on such knowledge. The educational value of such a training is undisputed. On the other hand, the work of the amateur astronomer can also contribute essentially to the work of the professionals. It is from these points of view that this handbook aims to help with versatile advice. At the same time, the book intends to show the wide range of applied astronomy, as it presents itself to the friend of the stars; in mathematical-physical fields, in precision mechanics and optics, and last but not least in the area of social relations. Beyond the circle of amateur astronomers the book is addressed to lecturers, teachers, students and pupils. It wishes to serve them as a guide to "astronomical experiments," which we suggest should be performed in primary and secondary schools, specialist colleges, and extramural courses.

There have been many developments in the field of light pollution over the last few years, and this second edition of 'Light Pollution - Responses and Remedies' will introduce them in detail. Examples include the appearance of anti-light pollution legislation in various countries, new departures in lighting design, human health implications, and the growing realization among the general public that lighting is not always a good thing. In this title, author Bob Mizon discusses the various ways in which wasted artificial light has damaged the quality of modern life, and suggest solutions. This book is for anyone who has experienced glare, discomfort, or nuisance from poorly directed lights; has wondered why we waste so much money lighting the sky; or anyone who simply wants to see the stars instead of a baleful urban glow. "Light Pollution, 2nd Edition" offers practical and inexpensive solutions to the world-wide problem of wasted artificial light, and emphasizes that light pollution is not just an astronomers' problem, but affects everyone in various ways.

The first edition of this text was written primarily by one of the present authors (HAS), with a chapter on instrumentation contributed by a second (NLA). The volume was well received, and to keep the text up-to-date a second edition was planned. For this second edition, a third author (WEK) was invited, whose background complemented that of the other two. Each of the authors was assigned several chapters as his primary task while the complete manuscript remained the second ary responsibility of all three. It is hoped that this approach has resulted in a work that is even more thorough than the first edition in covering the basic concepts of infrared spectroscopy. NELSON L. ALPERT WILLIAM E. KEISER HERMAN A. SZYMANSKI v PREFACE TO THE FIRST EDITION My experience with the many infrared spectroscopy institutes held at Canisius College and many discussions with both beginners and experienced practitioners in infrared spectroscopy have convinced me that there is a need for an introductory text devoted entirely to infrared spectroscopy, a text which can be utilized even by those who approach this study with only a limited background. This volume sprang from that conviction. It is intended for all who wish to use infrared spec troscopy in research - especially chemists doing structural work - in routine control work, in industrial development, or in medical appli cations or those military applications where it is employed as an analytical tool.

It would seem that any specialist in plasma physics studying a medium in which the interaction between particles is as distance-dependent as the inter action between stars and other gravitating masses would assert that the role of collective effects in the dynamics of gravitating systems must be decisive. However, among astronomers this point of view has been recog nized only very recently. So, comparatively recently, serious consideration has been devoted to theories of galactic spiral structure in which the dominant role is played by the orbital properties of individual stars rather than collec tive effects. In this connection we would like to draw the reader's attention to a difference in the scientific traditions of plasma physicists and astrono mers, whereby the former have explained the delay of the onset of controlled thermonuclear fusion by the "intrigues" of collective processes in the plasma, while many a generation of astronomers were calculating star motions, solar and lunar eclipses, and a number of other fine effects for many years ahead by making excellent use of only the laws of Newtonian mechanics. Therefore, for an astronomer, it is perhaps not easy to agree with the fact that the evolution of stellar systems is controlled mainly by collective effects, and the habitual methods of theoretical mechanics III astronomy must make way for the method of self-consistent fields."

The Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) is a NASA Explorer mission that is the first space mission dedicated to imaging of the Earth's magnetosphere. IMAGE was launched from Vandenberg AFB into an elliptical polar orbit by a Delta II launch vehicle on March 25, 2000. The two-year prime sci entific mission of IMAGE began on May 25, 2000 after instrument commissioning was successfully completed. IMAGE has now been approved for operation until October 1,2005, and an additional two-year extension is now being considered by NASA. The papers in this volume represent many of the scientific results obtained dur ing the IMAGE prime mission and include some of the early correlative research with ground-based measurements, measurements from other spacecraft such as Cluster II, and relevant theory and modeling programs. All of the reported work is related to the overall IMAGE science objective: How does the magnetosphere respond globally to the changing conditions in the solar wind? IMAGE addresses this question with multi-spectral imaging of most of the important plasma pop ulations of the inner magnetosphere, combined with radio sounding of gradients of total plasma content. The new experimental techniques fall into the following areas: neutral atom imaging (NAI) over an energy range from 10 eV to 500 keY for detection of ionospheric outflow, the plasma sheet, and the ring current; far ultraviolet (FUV) imaging at 121-190 nm for detection of precipitating protons and the global aurora; extreme ultraviolet (EUV) imaging at 30.

Thework described in this has somewhat erratically, over monograph grown, of than a more interest inthe was firstaroused period thirty My subject years. thebeautiful and inBroucke.'sthesis also by see computations drawings (1963; Broucke where familiesof orbits in the restricted three 1968), periodic body for the Earth Moon ratio = were mass problem investigated (/.I 0.012155). These that natural for the existence ofthe a explanation drawingssuggested observed familiesand for the found the of orbits could be shapes perhaps by to the limit ] 0. a recourse y As first it a to as as step, appeared catalog completely possible necessary the orbits obtained in this limit. orbits of the first generaiing Generating hadbeen studied andother authors. Poincar6 specZes by (1892) Surprisingly, the two other had been Orbits ofthe however, species apparently neglected. second orbits with or consecutive a species, collisions, present comparatively the ofthe simple problem, only two body problem; no using equations yet had been done.An ofthe systematic ever constituent arcs study inventory was inH6non presented (1968). Also little work had been done on farmlies of orbits of the third very to Hill's A numerical species, was corresponding problem. investigation pub lished inR6non (1969).

These are the proceedings of international conference on Numerical As trophysics 1998 (NAP98), held at National Olympic Memorial Youth Cen ter, in Tokyo, Japan in the period of March 10 - 13, 1998, and hosted by the National Astronomical Observatory, Japan (NAOJ). In the last decade numerical simulations have grown up as a major tool for astrophysics. Numerical simulations give us invaluable informa tion on complex systems and physical processes under extreme conditions which can be neither realized by experiments nor directly observed. Super computers and special purpose computers may work as very large telescopes and special purpose telescopes for theoretical astrophysics, respectively. Nu merical astrophysics ranks with other tool-oriented astronomy such as ra dio astronomy, infrared astronomy, ultraviolet astronomy, X-ray astronomy, and ')'-ray astronomy. This conference, NAP98, was planned to explore recent advances in astrophysics aided by numerical simulations. The subjects of the confer ence included the large-scale structure formation, galaxy formation and evolution, star and planets formation, accretion disks, jets, gravitational wave emission, and plasma physics. NAP98 had also sessions on numerical methods and computer science. The conference was attended by 184 sci entists from 21 countries. We enjoyed excellent talks, posters, videos, and discussions: there are 40 oral presentations, 96 posters and 16 video pre sentations. We hope that these proceedings and accompanying CD-ROM replay the friendly but inspiring atmosphere of the conference."

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.

Over the last few years it has become apparent that fluid turbulence shares many common features with plasma turbulence, such as coherent structures and self-organization phenomena, passive scalar transport and anomalous diffusion. This book gathers very high level, current papers on these subjects. It is intended for scientists and researchers, lecturers and graduate students because of the review style of the papers.

This book gives a comprehensive overview of the current observational and theoretical status in the field of the local and general interstellar medium. It contains contributions presented at the IAU Colloquium No. 166. Review articles and highlight talks will serve both as an introduction to the field for the undergraduate or the non-specialist and also give a summary of the most recent developments for the expert and researcher. These articles are supplemented by a representative number of original research papers. All contributions are fully refereed and have been edited with extensive care to provide a high-standard reference book. The scientific content spans a wide range from solar system measurements of dust grains to X-ray emission from distant galaxies.

The book contains courses taught to a public of Ph. D. students, post-docs and con?rmed researchers in all ?elds of heliospheric plasma physics. It aims at identifying physical issues which are common to two di?erent ?elds of astr- omy: solar and magnetospheric physics. Emphasis is given to basic processes of transport and conversion of energy: magnetic reconnection is discussed in detail from the viewpoints of MHD and kinetic physics. Processes of charged particle acceleration are reviewed and confronted with recent observations. The subject is introduced by a summary of MHD and the basic structures and parameters of the solar atmosphere, terrestrial ionosphere and mag- tosphere are reviewed. The book combines a pedagogic and comprehensive presentation of physical issues and raises fully open questions, with the c- plementary and sometimes con?icting views of geophysicists and solar phy- cists. The book's focus, while basic, opens new avenues. Observatory of Meudon, France Ludwig Klein IAS, Orsay, France Jean-Claude Vial OCA, France Jean-Pierre Rozelot August 2000 The Editors Preface Following the great success of the ?rst two CNRS Summer Schools on Solar Astrophysics held in Oleron (May 1996 and May 1997 - two schools devoted to the highlights of solar physics), I came to the conclusion that the initiative should be continued."

This specialized workshop was conceived during the workshop on "Non isotropic and Variable Outflows from Stars", which was held at the Space Telescope Science Institute in October, 1991. At that meeting, the four of us collectively decided that the time was ripe for an even more focussed discussion of the basic issues in the area of hot-star wind instability and its observable manifestations. Not that the big problems have been solved! Rather, we are currently in a phase of rapid development, both with regard to the models and to the observations. The key issue at this new workshop would be to decide how the time-dependent structures observed in hot-star winds (e. g. , NACs, DACs, blobs, clumps, filaments, shells, puffs, jets, etc. ) relate to radiative and other instabilities. Further questions concern the role of turbulence and the nature of its driver, and the effect of stellar rotation, pulsation, and magnetic fields on time-dependent phenomena in hot-star winds. Of no less importance is the impact of stellar wind variability on the derivation of mass-loss rates, on stellar evolution, and on momentum/energy deposition in the interstellar medium. To attain our goal of maximum confrontation (in the positive sense!) we decided: (1) to limit the workshop to the observers and theoreticians most active in this field in the world; (2) to insist that virtually all participants present a talk, thereby avoiding the distraction of poster sessions; and (3) to allocate approximately half of the allotted time to discussion.

This book is a collection of essays written by the very scientists and engineers who have led, and continue to lead, the scientific quest known as SETI, the search for extraterrestrial intelligence. Divided into three parts, the first section, 'The Spirit of SETI Past', written by the surviving pioneers of this then emerging discipline, reviews the major projects undertaken during the first 50 years of SETI science and the results of that research. In the second section, 'The Spirit of SETI Present', the present-day science and technology is discussed in detail, providing the technical background to contemporary SETI instruments, experiments, and analytical techniques, including the processing of the received signals to extract potential alien communications. In the third and final section, 'The Spirit of SETI Future', the book looks ahead to the possible directions that SETI will take in the next 50 years, addressing such important topics as interstellar message construction, the risks and assumptions of interstellar communications, when we might make contact, what aliens might look like and what is likely to happen in the aftermath of such a contact.

The objective of the book is to find an answer to the rationale behind the human quest for the Mars exploration. As a comprehensive assessment for this query is undertaken, it is realized that the basic question 'Why Mars?' seeks various responses from technological, economic and geopolitical to strategic perspectives. The book is essentially targeted to understand India's desire to reach Mars. In the process, it also undertakes some implicit questioning of Mars programmes of various other states essentially to facilitate the setting up of the context for an assessment. The book is divided into two parts: Part I: This covers both science and politics associated with Mars missions in global scenario and discusses the salient features of various Mars Missions undertaken by various countries. Part II: This provides details in regards to India's Mars Mission.

Laser physics and nonlinear optics are fields which have been intimately con nected from their beginning. Nonlinear optical effects such as second-har monic generation fulfil vital functions in many laser systems. Conversely advances in laser development quickly lead to progress in nonlinear optics. Of particular importance has been the development of tunable visible and uv lasers. With the ability to tune the laser frequency into close resonance with atomic transition frequencies, one can produce a large resonance en hancement of the nonlinearity. This permits the observation of a great var iety of nonlinear optical processes in dilute media such as atomic vapours. In recent years much of the research effort in nonlinear optics has been directed towards the use of such media, and it is this area which forms the subject of the present book. We review a wide range of nonlinear optical processes in atomic vapours, molecular gases and cryogenic liquids. At the same time we have tried to treat the subject in sufficient depth to be useful to research workers in the field. To achieve this, a measure of selectivity has been introduced by emphasising those nonlinear processes which are seen to have applications as sources of tunable coherent radiation. Thus we have not discussed in any detail those nonlinear processes whose main applications are in spec troscopy, such as Doppler-free two-photon absorption."

Although recent works on Galileo's trial have reached new heights of erudition, documentation, and sophistication, they often exhibit inflated complexities, neglect 400 years of historiography, or make little effort to learn from Galileo. This book strives to avoid such lacunae by judiciously comparing and contrasting the two Galileo affairs, that is, the original controversy over the earth's motion ending with his condemnation by the Inquisition in 1633, and the subsequent controversy over the rightness of that condemnation continuing to our day. The book argues that the Copernican Revolution required that the hypothesis of the earth's motion be not only constructively supported with new reasons and evidence, but also critically defended from numerous old and new objections. This defense in turn required not only the destructive refutation, but also the appreciative understanding of those objections in all their strength. A major Galilean accomplishment was to elaborate such a reasoned, critical, and fair-minded defense of Copernicanism. Galileo's trial can be interpreted as a series of ecclesiastic attempts to stop him from so defending Copernicus. And an essential thread of the subsequent controversy has been the emergence of many arguments claiming that his condemnation was right, as well as defenses of Galileo from such criticisms. The book's particular yet overarching thesis is that today the proper defense of Galileo can and should have the reasoned, critical, and fair-minded character which his own defense of Copernicus had.

These words are written on the SOOth anniversary of Columbus' discovery of the New World. Surely the deep-space exploration of other worlds in our Solar System over the past few decades is an event of similar magnitude. Man has traveled far enough to see Spaceship Earth suspended alone in black space. And he has voyaged even farther to marvel at the crescent Earth rising over the Moon's cratered terrain. Instrumented spacecraft have toured the entire Solar System even beyond the ninth planet Pluto. This work of science Morphology of the Rocky Members of the Solar System is an inquiry about our extended home. As with the Darwinian and Copernican paradigms, the nature of our planetary system, as the extended world around us, has great significance for those who ponder the human condition. The deep-space views of our Planet Ocean with its sweeping clouds, and moving oceans and creeping continents must rank as the greatest photograph ever taken. Viewing Spaceship Earth hanging in the vast void is an almost frightening experience. We are so alone! It is easy to understand why so many are attracted to a simpler account of origins, like the allegorical tale of creation written in heroic style (but eschewing math, maps, figures, tables, references, and evidence) in the first eleven chapters of Genesis. This treatise examines the morphology of the six rocky planets and their 27 satellites from a broad perspective.

The nationally recognized credit-by-exam DSST (R) program helps students earn college credits for learning acquired outside the traditional classroom such as; learning from on-the-job training, reading, or independent study. DSST (R) tests offer students a cost-effective, time-saving way to use the knowledge they've acquired outside of the classroom to accomplish their education goals. Peterson's (R) Master the (TM) DSST (R) Astronomy Exam provides a general overview of the subjects students will encounter on the exam such as the history of the Science of Astronomy, Astrophysics, Celestial Systems, the Science of Light, Planetary Systems, Nature and Evolution of the Sun and Stars, Galaxies and the Universe. This valuable resource includes: Diagnostic pre-test with detailed answer explanations Assessment Grid designed to help identify areas that need focus Subject Matter Review proving a general overview of the subjects, followed by a review of the relevant topics and terminology covered on the exam Post-test offering 60 questions all with detailed answer explanations Key information about the DSST (R) such as, what to expect on test day and how to register and prepare for the DSST (R)