This book is the first to document in depth the history of lunar and planetary cartography in Russia. The first map of the far side of the Moon was made with the participation of Lomonosov Moscow University (Sternberg Astronomical Institute, MSU) in 1960. The developed mapping technologies were then used in preparing the "Complete Map of the Moon" in 1967 as well as other maps and globes. Over the years, various maps of Mars have emerged from the special course "Mapping of extraterrestrial objects" in the MSU Geography Department, including the hypsometric map of Mars at a scale of 1:26,000,000, compiled by J.A. Ilyukhina and published in 2004 in an edition of 5,000 copies. A more detailed version of this map has since been produced with a new hypsometric scale. In addition, maps of the northern and southern hemispheres of Mars have been compiled for the hypsometric globe of Mars. Relief maps of Venus were made in 2008, 2010, and 2011, and hypsometric maps of Phobos and Deimos at a scale of 1:60,000 were published in 2011. History of Lunar and Planetary Cartography in Russia provides detailed information on the compilation of this diverse range of maps and will be of interest to all lunar and planetary cartographers.

Comet Hale-Bopp defines a milestone event for cometary science: it is the first "really big" comet observed with modern equipment on the ground and from space and due to that; it is considered the new reference object in cometary sciences.

At the beginning of a new era in spacecraft exploration of comets and five years after Hale-Bopp's perihelion passage these proceedings of invited and contributed papers for IAU Colloquium 186 "Cometary Science after Hale-Bopp" review the state-of-the-art knowledge on comets, the icy, dusty and most primordial left-overs of the formation disk of our own solar system.

The majority of this volume is devoted to the subject of high energy radiation from galactic and extragalactic black holes. The volume also covers future space missions to primitive bodies and fine structures in the middle atmosphere and their origin. In total, 27 papers are presented, the final two included in the appendix emanating from the previous COSPAR meeting in Washington.

The conversion of energy generated in the Sun's interior creates its hot corona and a wealth of dynamical phenomena such as flares and mass ejections. Based on recent significant progress in understanding magnetic reconnection and a wealth of new observations of energetic particle signatures from the Sun, the present volume reviews the current theoretical and experimental status in the field. Paying attention to both the details and the broader picture, this book addresses both the experienced researcher as well as nonspecialist researchers from related areas and postgraduate students in astrophsics.

This is the eleventh volume in the series Light Scattering Reviews, devoted to current knowledge of light scattering problems and both experimental and theoretical research techniques related to their solution. The focus of this volume is to describe modern advances in radiative transfer and light scattering optics. This book brings together the most recent studies on light radiative transfer in the terrestrial atmosphere, while also reviewing environmental polarimetry. The book is divided into nine chapters: * the first four chapters review recent advances in modern radiative transfer theory and provide detailed descriptions of radiative transfer codes (e.g., DISORT and CRTM). Approximate solutions of integro-differential radiative transfer equations for turbid media with different shapes (spheres, cylinders, planeparallel layers) are detailed; * chapters 5 to 8 focus on studies of light scattering by single particles and radially inhomogeneous media; * the final chapter discusses the environmental polarimetry of man-made objects.

Planetary Aeronomy is a modern and concise introduction to the underlying physical and chemical processes that govern the formation and evolution of the upper atmospheres of planets. The general approach employed permits consideration of the growing number of extrasolar planets, the detailed observation of which will become possible over the next decades. The book explains the physics behind many atmospheric processes, which are relevant for the evolution of planetary atmospheres and their water inventories, and also contains useful scaling laws and analytical expressions that can be applied to any planet. Readers thus gain insight into the evolution of terrestrial planets and their long-time habitability, atmospheric stability, etc. This volume can be used both as graduate textbook for students wishing to specialize in the field as well as succinct compendium for researchers in the field.

A quantitative measure of the accuracy of the rate coefficients and the excess energies is a desirable goal of this analysis. There are two major sources of uncertainties: The atomic and molecular data and the solar irradiance. The cross sections and branching ratios used in this analysis come from many different sources; many of them without any error indications. For this reason, we must confine ourselves to a qualitative indication of the reliability of the results. Specifically we give a quality scale in Table II for the data of each mother molecule; A indicating the highest quality of atomic and molecular data and F the lowest quality. The letter B typically means that the threshold is uncertain. For most molecules the cross section at threshold is very small and the rate coefficient for these molecules is therefore not influenced by this uncertainty. For atomic species the cross section is usually large near threshold, but for these species the threshold is known quite accurately. The letter B, therefore, indicates that the rate coefficient is most likely quite accurate, but the excess energy is less accurately known. The letter C usually means that the branching ratios are not well known. This means that the total rate coefficient is very good, but the rate coefficients and the excess energies for the individual branches are less accurate.

Camille Flammarion (1842-1925) began his career at 16 as a human computer under the great mathematician U. J. J. Le Verrier at the Paris Observatory. He soon tired of the drudgery; he was drawn to more romantic vistas, and at 19 wrote a book on an idea that he was to make his own-the habitability of other worlds. There followed a career as France's greatest popularizer of astronomy, with over 60 titles to his credit. An admirer granted him a chateau at Juvisy-sur-l'Orge, and he set up a first-rate observatory dedicated to the study of the planet Mars. Finally, in 1892, he published his masterpiece, La Planete Mars et ses conditions d'habitabilite, a comprehensive summary of three centuries' worth of literature on Mars, much of it based on his own personal research into rare memoirs and archives. As a history of that era, it has never been surpassed, and remains one of a handful of indispensable books on the red planet. Sir Patrick Moore (1923-2012) needs no introduction; his record of popularizing astronomy in Britain in the 20th century equaled Flammarion's in France in the 19th century. Moore pounded out hundreds of books as well as served as presenter of the BBC's TV program "Sky at Night" program for 55 years (a world record). Though Moore always insisted that the Moon was his chef-d'oeuvre, Mars came a close second, and in 1980 he produced a typescript of Flammarion's classic. Unfortunately, even he found the project too daunting for his publish ers and passed the torch of keeping the project alive to a friend, the amateur astronomer and author William Sheehan, in 1993. Widely regarded as a leading historian of the planet Mars, Sheehan has not only meticulously compared and corrected Moore's manuscript against Flammarion's original so as to produce an authoritative text, he has added an important introduction showing the book's significance in the history of Mars studies. Here results a book that remains an invaluable resource and is also a literary tour-de-force, in which the inimitable style of Flammarion has been rendered in the equally unique style of Moore.

Since its launch in 1991, the Yohkoh satellite has been returning unprecedented observations of solar flares and the dynamic solar corona. This book is a collection of papers presented at a meeting held in: Yoyogi, Tokyo, on the occasion of Yohkoh's fifth anniversary of operation. The papers constitute a summary of observations and results over the five years, including contributions based on data from Yohkoh's hard and soft X-ray telescopes and its spectrometer experiments. The five years of data, covering approximately one-half of a solar cycle, reveal a fresh perspective on solar science, with a new picture of solar flares and the active Sun emerging. Also, for the first time there are extensive results from Yohkoh observations of the Sun during the solar minimum period. This wide-ranging volume will be of interest to workers in solar physics and X-ray astronomy. It also contains material appropriate for supplemental reading for graduate students in solar physics.

Magnetic fields are responsible for much of the variability and structuring in the universe, but only on the Sun can the basic magnetic field related processes be explored in detail. While several excellent textbooks have established a diagnostic foundation for exploring the physics of unmagnetized stellar atmospheres through spectral analysis, no corresponding treatise for magnetized stellar atmospheres has been available. The present monograph fills this gap. The theoretical foundation for the diagnostics of stellar magnetism is developed from first principles in a comprehensive way, both within the frameworks of classical physics and quantum field theory, together with a presentation of the various solar applications. This textbook can serve as an introduction to solar and stellar magnetism for astronomers and physicists at the graduate or advanced undergraduate level and will also become a resource book for more senior scientists with a general interest in cosmic magnetic fields.

The systematic study of the planets has experienced a slow but steady progress from the efforts of a single individual (Galileo Galilei, 1564-1642) to nations that individually and collectively create whole agencies and complex infrastructures devoted to the exploration and understanding of our solar system. This quest for knowledge continues in earnest today as we attempt to understand Earth's unique place among its closest neighbors. Known diversities emphasize fractionation processes that may have occurred in the nebula during early solar system formation, and the vastly different evolutionary paths taken by the planets and their satellites. The discovery of similarities and differences among the planets has given rise to a discipline of "Comparative Planetology. " Here terrestrial properties and giant planet atmospheres are viewed and probed, surface geologies are related to atmospheres and oceans, interior structures are envisioned, magnetic fields mapped, and bizarre differences in satellites and ring systems continue to enlighten, amaze and confound the detectives of planetary science. A science organizing committee with international participation was formed to develop a conference program to address the basic issues and the fundamental processes that are common among the planets. The goals of the meeting were twofold: first the production of a reference source on comparative planetology for academia, and second, the provision of an impetus for NASA to begin a program devoted to this emerging science discipline. The conference program accommodated seventeen invited papers and nineteen poster presentations.

A Corotating Interaction Region (CIR) is the result of the interaction of fast solar wind with slower solar wind ahead. CIRs have a very large three-dimensional ex tent and are the dominant large-scale structure in the heliosphere on the declining and minimum phase of the solar activity cycle. Until recently, however, CIRs could only be observed close to the ecliptic plane, and their three-dimensional structure was therefore not obvious to observers and theoreticians alike. Ulysses was the first spacecraft allowing direct exploration of the third dimen sion of the heliosphere. Since 1992, when it has entered a polar orbit that takes it 0 up to 80 latitude, the spacecraft's performance has been flawless and the mission has provided excellent data from a superbly matched set of instruments. Perhaps the most exciting observation during Ulysses' first passage towards the south pole of the Sun was a strong and long lasting CIR whose energetic particle effects were observed up to unexpectedly high latitudes. These observations, documented in a number of publications, stimulated considerable new theoretical work.

Les deuxiernes "Rencontres de l'Observatoire", qui ont eu lieu a l'Observatoire de Paris a Meudon du 10 au 14 Janvier 2000, ont reuni autour du theme "Problernes ernergents en physique de I'espace" 120 physiciens et astrophysiciens venus d'une vingtaine de pays differents. Nous avons voulu honorer a cette occasion Jean-Louis Steinberg pour ses con- tributions majeures a la recherche spatiale, ala radioastronomie et a la physique de I'espace. L'approche explicitement pluridisciplinaire de ce colloque, qui ne s'est pas laisse confiner dans les limites etroites de la physique spatiale ni dans celles imposees par certains programmes officiels, suit l'esprit de sa carriere scientifique: sortir des limites des sujets deja etudies ou sur Ie point de l'etre, et appliquer les connaissances acquises pour explorer de nouveaux domaines. Ce dernier quart de siecle a vu une croissance vertigineuse des performances spatiales. La technologie moderne ne perrnet pas encore de jongler avec les univers comme Ie prestidigitateur de Grandville (Grandville, Un autre monde, ed. H. Four- nier, Paris, 1844); mais quelques decades ont suffi pour voir des instruments soph- istiques explorer les frontieres du systerne solaire, et la cornmunaute de la recher- che spatiale a depasse rapidement Ie sujet etroit de I'environnement soleil-terre pour s'interesser a I'ensemble de l'heliosphere, OU les memes processus physiques sont a I'ceuvre.

IAU Symposium 172 Dynamics, Ephemerides and Astrometry of the Solar System was held in Paris in July, 1995. 250 scientists from 33 countries attended the symposium; 24 invited lectures and 165 contributed papers were presented (117 of which were posters). The papers covered topics on celestial mechanics (chaos and evolution of the solar system, asteroids, theories of the motion of the planets, the moon and the natural satellites), methods (symplectic mappings and elliptic functions), astrometry (CCD observations, VLBI and radar observations), ephemerides (representation and numerical integration) and on the history of celestial mechanics.

This unique volume contains the proceedings of two "Non-Sleeping Universe" conferences: "Stars and the ISM" and "From Galaxies to the Horizon." The book provides an overview of recent developments in a variety of areas, covering a very wide range of spatial and temporal scales.

Starting from Mars outward this concise handbook provides thorough information on the satellites of the planets in the solar system. Each chapter begins with a section on the discovery and the naming of the planet s satellites or rings. This is followed by a section presenting the historic sources of those names. The book contains tables with the orbital and physical parameters of all satellites and is illustrated throughout with modern photos of the planets and their moons as well as historical and mythological drawings. The Cyrillic transcriptions of the satellite names are provided in a register.

Readers interested in the history of astronomy and its mythological backgrounds will enjoy this beautiful volume.

"

This volume covers different aspects of recent theoretical and observational work on magnetic reconnection, a fundamental plasma-physical process by which energy stored in magnetic field is converted, often explosively, into heat and kinetic energy. This collection of papers from the fields of solar and space physics, astrophysics, and laboratory plasma physics is especially timely in view of NASA's upcoming Magnetospheric Multiscale mission, which will use Earth's magetosphere as a laboratory to test, through in-situ measurement of the plasma, energetic particles, and electric and magnetic fields, the various and sometimes competing models and theories of magnetic reconnection.
This volume is aimed at researchers in solar physics, magnetospheric physics and plasma physics.
Previously published in Space Science Reviews journal, Vol. 160/1-4, 2011.

Representatives of several scientific communities, such as planetary scientists, astronomers, space physicists, chemists and astrobiologists have met with the aim to review the knowledge on four major themes: (1) the study of the formation and evolution processes of the outer planets and their satellites, beginning with the formation of compounds and planetesimals in the solar nebula, and the subsequent evolution of the interiors of the outer planets, (2) a comparative study of the atmospheres of the outer planets and Titan, (3) the study of the planetary magnetospheres and their interactions with the solar wind, and (4) the formation and properties of satellites and rings, including their interiors, surfaces, and their interaction with the solar wind and the magnetospheres of the outer planets. Beyond these topics, the implications for the prebiotic chemical evolution on Europa and Titan are reviewed. At the time of publication, the study of the outer planets is particularly motivated by the fact that the Saturn system is being investigated by the Cassini-Huygens mission.

Captures advances being made in the field of coronal magnetism, from theory to observations and instrumentation. This volume is a collection of research articles on the subject of the solar corona, and particularly, coronal magnetism. The book was motivated by the Workshop on Coronal Magnetism: Connecting Models to Data and the Corona to the Earth, which was held 21 - 23 May 2012 in Boulder, Colorado, USA. This workshop was attended by approximately 60 researchers. Articles from this meeting are contained in this topical issue, but the topical issue also contains contributions from researchers not present at the workshop. This volume is aimed at researchers and graduate students active in solar physics. Originally published in Solar Physics, Vol. 288, Issue 2, 2013 and Vol. 289, Issue 8, 2014.

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 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.

The 19th ESLAB Symposium on 'The Sun and the Heliosphere in Three Dimensions' was held in Les Diablerets (Switzerland) on 4-6 June 1985. Organised almost exactly ten years after the Goddard Space Fl i ght Center Sympos i um dea 1 i ng with the Sun and the i nterp 1 anetary medium in three dimensions, the aim of this Symposium was not only to review the progress made in understanding the three-dimensional structure and dynamics of the heliosphere, but also to look ahead to the scientific return to be expected from the Ulysses mission. Scheduled for launch in May 1986, the scientific instrumentation on board Ulysses will shed light on the conditions and processes occurring away from the ecliptic plane, thereby adding literally a new dimension to our understanding of the only stellar plasmasphere to which we have direct access. The scientific programme of the Symposium was built around a series of invited review papers dealing with aspects of the corona and its influence on the interplanetary medium via transient ejecta, the solar wind, energetic solar particles and galactic cosmic rays, interplanetary dust and neutral gas. These invited talks were supplemented by a number of contributed and poster papers. With the exception of three contributed talks and Wibberenz' review of coronal and acceleration of energetic particles, all papers propagation presented at the Symposium are included in this volume.

This Second Edition of Sun, Earth and Sky updates the popular text by providing comprehensive accounts of the most recent discoveries made by five modern solar spacecraft during the past decade. Their instruments have used sound waves to peer deep into the Sun's inner regions and measure the temperature of its central nuclear reactor, and extended our gaze far from the visible Sun to record energetic outbursts that threaten Earth. Breakthrough observations with the underground Sudbury Neutrino Observatory are also included, which explain the new physics of ghostly neutrinos and solve the problematic mismatch between the predicted and observed amounts of solar neutrinos. This new edition of Sun, Earth and Sky also describes our recent understanding of how the Sun's outer atmosphere is heated to a million degrees, and just where the Sun's continuous winds come from. As humans we are more intimately linked with our life-sustaining Sun than with any other astronomical object, and the new edition therefore provides modern interpretations of ozone depletion and global warming that are related to both the Sun and to human activities. introduces the Sun and its physics, and describes all aspects of the Sun's interaction with us on Earth.

It is now a well-established tradition that every four years, at the end of winter, a group of 'celestial mechanicians' from all over the world gather in the Austrian Alps at the invitation of R. Dvorak. This time the colloquium was held at Badhofgastein from March 19 to March 25, 2000 and was devoted to the 'New Developments in the Dynamics of Planetary Systems'. The papers covered a large range of questions of current interest: t- oretical questions (resonances, KAM theory, transport, ... ) and questions about numerical tools (synthetic elements, indicators of chaos, ... ) were particularly well represented; of course planetary theories and Near Earth Objects were also quite popular. Three special lectures were delivered in honor of deceased colleagues whom, to our dismay, we will no longer meet at the 'Austrian Colloquia'. W. Jefferys delivered the Heinrich Eichhorn lecture on 'Statistics for the Twenty-first Century Astrometry', a topic on which Heinrich Eichhorn was a specialist. A. Roy delivered a lecture honoring Victor Szehebely on 'Lifting the Darkness: Science in the Third Millenium', in which in wove anecdotes and remembrances of Victor which moved the audience very much. A. Lemaitre spoke in honor of Michele Moons on 'Mech anism of Capture in External Resonance'. The end of her talk was devoted to a short and moving biography of Michele illustrated by many slides."

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.