IAU Symposium Number 52 on Interstellar Dust and Related Topics was held at Albany, N.Y., on the campus of the State University of New York at Albany from May 29 to June 2, 1972. The members of the Organizing Committee were: Dr A. D. Code, University of Wisconsin, Madison, Wis., U.S.A. Dr B. D. Donn, Goddard Space Flight Center, Greenbelt, Md., U.S.A. Dr A. Elvius, Stockholm Observatory, Saltsjobaden, Sweden. Dr T. Gehrels, Lunar and Planetary Laboratory, University of Arizona, Tucson, Ariz., U.S.A. Dr J. M. Greenberg (Chairman), State University of New York at Albany, Albany, N.Y., U.S.A. Dr H. C. van de Hulst, Sterrewacht, Leiden, Holland. Dr S. B. Pikel'ner, Sternberg Astronomical Institute, Moscow, U.S.S.R. Dr E. E. Salpeter, Cornell University, Ithaca, N.Y., U.S.A. Dr B. E. Turner, National Radio Astronomy Observatory, Charlottesville, Va., U.S.A. The suggestion was first made in 1971 that a symposium on interstellar grains would be timely. The response to the first preliminary announcement, which was sent out on November 29, 1971, was well beyond our expectations. The meeting was locally sponsored by the State University and by Dudley Observatory. The National Aeronautics and Space Administration and the National Science Foundation con tributed along with the IAU. There were 158 participants of whom 49 were from 15 countries outside the United States. A total of 92 papers were presented."

Solid particles are followed from their creation through their evolution in the Galaxy to their participation in the formation of solar systems like our own, these being now clearly deduced from observations by the Hubble Space Telescope as well as by IR and visual observations of protostellar disks, like that of the famous Beta Pictoris object. The most recent observational, laboratory and theoretical methods are examined in detail. In our own solar system, studies of meteorites, comets and comet dust reveal many features that follow directly from the interstellar dust from which they formed. The properties of interstellar dust provide possible keys to its origin in comets and asteroids and its ultimate origin in the early solar system. But this is a continuing story: what happens to the solid particles in space after they emerge from stellar sources has important scientific consequences since it ultimately bears on our own origins - the origins of solar systems and, especially, of our own earth and life in the universe.

Interstellar dust, meteorites, interplanetary dust particles (IDP's), the zodiacal light, comets, comet dust. Where do they come from, what are they made of, how do they evolve, and finally, are there connections between them? These are the questions discussed in this volume by some of the world's outstanding experts in their respective fields. The techniques used for studying the `small' solid objects of space are thoroughly discussed. Some of the methods involve a synthetic approach using the laboratory to create analog environments and materials which are believed to resemble those in space. Others use direct laboratory methods with state-of-the-art analytical tools to study the material of the objects themselves - meteorites, IDP'S. And others apply the latest in astronomical facilities to provide quantitative data on the material properties of the solids which can only be deduced from remote observations, These are compared with the laboratory results. In one instance there was a possibility to study a solar system body in situ and that was the case of comet Halley and some of the results of these studies obtained from space `laboratories' launched to meet it are discussed here. Finally, there are theoretical papers which are aimed at bridging the results of observational and laboratory methods. This book is recommended to senior scientists as well as graduate students who wish to pursue research in interstellar and solar system astronomy and their connections.

This volume contains the lectures presented at the second course of the International School of Space Chemistry held in Erice (Sicily) from October 20 - 30 1991 at the "E. Majorana Centre for Scientific Culture." The course was attended by 58 participants from 13 countries. The Chemistry of Life's Origins is well recognized as one of the most critical subjects of modem chemistry. Much progress has been made since the amazingly perceptive contributions by Oparin some 70 years ago when he first outlined a possible series of steps starting from simple molecules to basic building blocks and ultimate assembly into simple organisms capable of replicating, catalysis and evolution to higher organisms. The pioneering experiments of Stanley Miller demonstrated already forty years ago how easy it could have been to form the amino acids which are critical to living organisms. However we have since learned and are still learning a great deal more about the primitive conditions on earth which has led us to a rethinking of where and how the condition for prebiotic chemical processes occurred. We have also learned a great deal more about the molecular basis for life. For instance, the existence of DNA was just discovered forty years ago.

What is the nature and composition of the dust grains responsible for the visual extinction in our Galaxy and in other galaxies beyond? What are the ranges in temperature of dust grains? Can these be less than 2.7K? Can the distribution of cold grains be studied optically at unprecedented arcsecond resolution? How does the presence of dust affect the morphology of a galaxy? Is this new dust-penetrated view bringing us to the verge of a breakthrough in understanding the connection between galaxy morphology and the underlying physics of galaxies? How large are the amounts of cold molecular hydrogen gas and cold dust in galactic disks? These are some of the key issues addressed in this book, which takes the postgraduate reader and professional researcher to the cutting edge of this rapidly developing field. Unique features of the book include fourteen in-depth invited review papers and twenty-six pages of discussion transcribed from a television tape. The contributions reflect the entire proceedings of an intensive one week International Conference on cold dust and galaxy morphology held in Johannesburg, South Africa, during January 1996.

IAU Symposium Number 52 on Interstellar Dust and Related Topics was held at Albany, N.Y., on the campus of the State University of New York at Albany from May 29 to June 2, 1972. The members of the Organizing Committee were: Dr A. D. Code, University of Wisconsin, Madison, Wis., U.S.A. Dr B. D. Donn, Goddard Space Flight Center, Greenbelt, Md., U.S.A. Dr A. Elvius, Stockholm Observatory, Saltsjobaden, Sweden. Dr T. Gehrels, Lunar and Planetary Laboratory, University of Arizona, Tucson, Ariz., U.S.A. Dr J. M. Greenberg (Chairman), State University of New York at Albany, Albany, N.Y., U.S.A. Dr H. C. van de Hulst, Sterrewacht, Leiden, Holland. Dr S. B. Pikel'ner, Sternberg Astronomical Institute, Moscow, U.S.S.R. Dr E. E. Sal peter, Cornell University, Ithaca, N.Y., U.S.A. Dr B. E. Turner, National Radio Astronomy Observatory, Charlottesville, Va., U.S.A. The suggestion was first made in 1971 that a symposium on interstellar grains would be timely. The response to the first preliminary announcement, which was sent out on November 29, 1971, was well beyond our expectations. The meeting was locally sponsored by the State University and by Dudley Observatory. The National Aeronautics and Space Administration and the National Science Foundation con tributed along with the JAU. There were 158 participants of whom 49 were from 15 countries outside the United States. A total of 92 papers were presented.

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."

Solid particles are followed from their creation through their evolution in the Galaxy to their participation in the formation of solar systems like our own, these being now clearly deduced from observations by the Hubble Space Telescope as well as by IR and visual observations of protostellar disks, like that of the famous Beta Pictoris object. The most recent observational, laboratory and theoretical methods are examined in detail. In our own solar system, studies of meteorites, comets and comet dust reveal many features that follow directly from the interstellar dust from which they formed. The properties of interstellar dust provide possible keys to its origin in comets and asteroids and its ultimate origin in the early solar system. But this is a continuing story: what happens to the solid particles in space after they emerge from stellar sources has important scientific consequences since it ultimately bears on our own origins - the origins of solar systems and, especially, of our own earth and life in the universe.

The now recognized extensive existence of life on earth very shortly after the destructive bombardment of the earth's surface by early solar system debris has stimulated inquiry into possible exogenous sources of prebiotic molecules from space as well as intensified studies of the early earth's atmosphere. The chapters in this book cover the possible sources of prebiotic molecules and avenues by which life could have evolved, starting from the birth and evolution of the solar system. The relevance of the classic experiments by Stanley Miller on the formation of life's building blocks on an early earth is reexamined. The role of chemistry in space is covered by chapters on interstellar dust, and meteorites to which experimental as well as theoretical investigations have been directed. In various chapters the existence of amino acids as well as other prebiotic molecules in meteorites is clearly established and inferred for interstellar dust and comets. Theories of molecular synthesis in the solar nebula are considered. Extensive coverage is given to the physical conditions and to prebiotic systems on the early earth. Possible pathways to life on an early Mars and the possible messages to be obtained by space exploration are discussed. Questions of effects of clays and of chirality on early chemical evolution are discussed. Recent ideas on the RNA world as the precursor to life are reviewed. The open-endedness of the study of life's origins and the need to investigate whether the prebiotic building blocks formed in outer space or on the earth is emphasized. A good deal of the book is suitable to graduate students.

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."

Interstellar and solar system solids are different stages of the same materials. In this book, the sources and evolution of circumstellar dust, interstellar dust, comets, meteorites and interplanetary dust are carefully discussed in the context of their interrelations. One of the major questions raised is: how do characteristically 1/10 micron interstellar dust particles evolve to rocky materials 1000 times larger or more? The closest we appear to be getting in relating interstellar dust to particles in the solar system is the evidence for submicron organic coated particles in interplanetary dust particles collected in the upper atmosphere, which allow direct laboratory investigation on Earth. What we know about comets, however, either results from remote observation or space measurements in situ. Comet volatiles compare very well with interstellar ices. These astrophysical problems bring to bear a very wide range of theoretical, observational and laboratory expertise in such fields as astronomy, physics and chemistry and, with the evidence of complex prebiotic organics in meteorites.

What is the nature and composition of the dust grains responsible for the visual extinction in our Galaxy and in other galaxies beyond? What are the ranges in temperature of dust grains? Can these be less than 2.7K? Can the distribution of cold grains be studied optically at unprecedented arcsecond resolution? How does the presence of dust affect the morphology of a galaxy? Is this new dust-penetrated view bringing us to the verge of a breakthrough in understanding the connection between galaxy morphology and the underlying physics of galaxies? How large are the amounts of cold molecular hydrogen gas and cold dust in galactic disks? These are some of the key issues addressed in this book, which takes the postgraduate reader and professional researcher to the cutting edge of this rapidly developing field. Unique features of the book include fourteen in-depth invited review papers and twenty-six pages of discussion transcribed from a television tape. The contributions reflect the entire proceedings of an intensive one week International Conference on cold dust and galaxy morphology held in Johannesburg, South Africa, during January 1996.