In Small Astronomical Observatories, Patrick Moore has collected descriptions of amateur and small professional observatories currently in use in Europe and America, showing how many astronomers have built their own observatory, often with effective and sometimes extraordinary improvisations to reduce the cost. There is a photograph of each, along with details of its construction and a foreword written by Patrick Moore. In addition to providing a fascinating study for its own sake, Small Astronomical Observatories offers a unique fund of ideas and practical details for anyone who wants to build an amateur or small professional observatory.

Magnetism is one of the basic properties of matter. Mankind has trav­ elled a long road in discovering and utilizing magnetism, and in this respect the ancient Chinese people have made outstanding contribu­ tions. In the book 'Lu's Spring and Autumn', written near the end of the Warring States Period, i. e. in the third century B. C. , there is a statement on the "attraction of iron by lodestones". So at that time it was known that magnets can attract ferromagnetic material. At the be­ ginning ofthe first century A. D. , viz. in the early years ofthe East Hang Dynasty, the famous scholar Wang Chong wrote in his masterpiece 'Len Hen' that the handle of a magnetic dipper pointed to the south. It was thus discovered at the time that magnets can point to the poles of the geomagnetic field. At the beginning of the twelfth century, during the reign of Emperor Hui of the Sung Dynasty, in the two books written by Zhu Yo and Xu Jin, respectively, there are descriptions of the com­ pass used in navigation. This tells us that the application of compasses was rather widespread at that time. The distinguished scientist Sen Go (1031-1085) discovered the declination of the terrestrial magnetic field. This is four hundred and more years earlier than its discovery by Christopher Columbus in 1492 during his voyage across the Atlantic Ocean. Such facts as these manifest the important contributions of ancient China to global civilization.

Solar flares are very complex electromagnetic phenomena of a cataclysmic nature. Particles are accelerated to very high velocities and a variety of physical processes happen inside and outside flares. These processes can be studied by a large number of techniques from Earth and from space. The aim is to discover the physics behind solar flares. This goal is complicated because information about the flare mechanism can be obtained only in an indirect way by studying the secondary effects.

One of the most spectacular discoveries of molecular astronomy has been the detection of maser emission. The same radiation that is generated in the laboratory only with elaborate, special equipment occurs naturally in interstellar space. This intense radiation probes the smallest structures that can be studied with radio telescopes. By a fortunate coincidence maser radiation is generated in both star forming regions and the envelopes of late-type stars. The early and late stages in the life of a star are considered to be the most interesting phases of stellar evolution. Maser emission has also been detected in external galaxies.

"Meteoric phenomena" is the accepted term for the complex of physi­ cal phenomena that accompany the entry of meteoric bodies into the at­ mosphere of the earth (or of any planet). "Meteoric bodies" are usually defined as cosmic bodies observed by optical or radar techniques, when they enter the atmosphere. The limiting sensitivity of present-day radar equipment makes it possible to record meteors of up to stellar magnitude +14, while the most brilliant bolides may reach magnitude -19. On a mass 7 7 scale this corresponds approximately to a range of 10- to 10 g. How­ ever, met~or astronomy is also concerned with larger objects, namely crater-forming meteorites, or objects that cause large-scale destruction when they arrive through the atmosphere (an example is the Tunguska River meteorite). Consideration of the interaction of such objects with 12 the terrestrial atmosphere extends the mass range to 10 g. On the other hand, scientists studying fragmentation processes in meteoric bod­ 7 ies have to consider particles with masses less than 10- g, and the use of data from meteoric-particle counters on rockets and artificial satel­ lites, from microcraters on the lunar surface, and from noctilucent clouds 12 lowers the minimum mass to 10- g. Therefore, the mass range of meteoric bodies, or meteoroids, encompasses 24 orders of magnitude. Although recent years have witnessed considerable development in meteor research, both in the Soviet Union and elsewhere, the main mono­ graphs on meteor physics were published twenty or more years ago.

Proceedings of Symposium No. 47 organized by the IAU held in Newcastle upon Tyne, England, March 22-26, 1971

THE MOON IX PREFACE TO THE SPRINGER EDITION When this collection of Babylonian astronomical purpose of column of the lunar ephemerides (by texts was published in 1955 (a date omitted by Aaboe) and the explanation of the method of computing the eclipse text ACT No. 6o (by Hamilton mistake from the title page), it contained all texts of this type that I could lay my hands on. As was to be and Aaboe). Some of these advances I have tried to incorporate into my History of Ancient Mathematical expected, the past 25 years provided more fragments, identified by A. Sachs and A. Aaboe in the British Astronomy (1975), which should be used as a guide to Museum and listed below. Also, some new joins the more recent literature. could be made and some errors of mine corrected. My sincerest thanks go to Springer-Verlag for Nevertheless, I think one still can consider the making this work again available to students of material of 1955 to be representative of what has been ancient astronomy. The Institute for Advanced preserved of the mathematical astronomy of the Study, which together with Brown University has Seleucid period. supported my work for more than four decades, has In the meantime, far more progress has been made graciously given its permission for this reprint. in our understanding of Babylonian astronomy, mainly by the publications of Aaboe, Hamilton, Maeyama, Sachs, van der Waerden, and others. As an Princeton 0.

This book presents two candidates for astrophysical accelerators of cosmic rays with petaelectron-volt (PeV) energies in our Galaxy, the so-called PeVatrons, through the observation of sub-PeV gamma rays performed by the Tibet air shower array. The two gamma-ray sources are TASG J1844-038—a newly detected source in this presented work—and HESS J1849-000. Reconstructing their gamma-ray energy spectra up to the sub-PeV range and also analyzing the archive data published by a radio survey, the book discusses in depth the emission mechanisms of the observed gamma rays and suggests that these two gamma-ray sources are candidates for PeVatrons. The results give insights into the population of PeVatron in the Galaxy, which is important to consider their contribution to the PeV cosmic rays observed at the Earth.

Since the dawn of mankind, observers of the sky have wondered at the sudden appearance of new stars on the seemingly unchanging heavens and, for at least 2000 years, have recorded these phenomena in their annals and archives. Even in more modern times, since the discovery of SN1885A in S Andromeda which ?gured in the important “island universe” discussions of the 1920’s, the puzzle of supernovae (SNe) has played an important role in astrophysics. Only with the seminal work of Fritz Zwicky and Walter Baade in the 1930’s did we begin to understand the di?erences between novae and SNe and the importance of SNe as the fonts of energy for the interstellar medium and as drivers of chemical evolution in galaxies. As recently as the 1940’s and 1950’s the early days of radio astronomy were heavily in?uenced by the familiar names of Cassiopeia A and Taurus A, two young supernova remnants, and two Nobel prizes have been awarded for discovery and study of a related phenomenon, pulsars. In spite of the great age of the study of SNe, since at least the Chinese records of SN185and probably earlier, the ?eld is, in fact, very young having only attracted a large devoted following since the spectacular Type II SN1987A in the Large Magellanic Cloud, the ?rst naked-eye SN in more than 400 years.

With its many beautiful colour pictures, this book gives fascinating insights into the unusual forms and behaviour of matter under extremely high pressures and temperatures. These extreme states are generated, among other things, by strong shock, detonation and electric explosion waves, dense laser beams, electron and ion beams, hypersonic entry of spacecraft into dense atmospheres of planets, and in many other situations characterized by extremely high pressures and temperatures.

This book results from recent studies aimed at answering questions raised by astrophycists who use values of transport coefficients that are old and often unsatisfactory. The few books dealing with the rigorous kinetic theory of a ionized plasma are based on the so called Landau (Fokker-Planck) equation and they seldom relate the microscopic results with their macroscopic counterpart provided by classical non-equilibrium thermodynamics. In this book both issues are thoroughly covered. Starting from the full Boltzmann equation for inert dilute plasmas and using the Hilbert-Chapman-Enskog method to solve the first two approximations in Knudsen´s parameter, we construct all the transport properties of the system within the framework of linear irreversible thermodynamics. This includes a systematic study of all possible cross effects (which, except for a few cases, were never treated in the literature) as well as the famous H-theorem. The equations of magneto-hydrodynamics for dilute plasmas, including the rather surprising results obtained for the viscomagnetic effects, may be now fully assessed. This book will be of immediate interest to the plasma physics community, as well as to astrophysicists. It is also likely to make an impact in the field of cold plasmas, involving laser cooled Rydberg atoms.

Most of the visible matter in the universe exists in the plasma state. Plasmas are of major importance for space physics, solar physics, and astrophysics. On Earth they are essential for magnetic controlled thermonuclear fusion.

This edited volume presents the current state of gas accretion studies from both observational and theoretical perspectives, and charts our progress towards answering the fundamental yet elusive question of how galaxies get their gas. Understanding how galaxies form and evolve has been a central focus in astronomy for over a century. These studies have accelerated in the new millennium, driven by two key advances: the establishment of a firm concordance cosmological model that provides the backbone on which galaxies form and grow, and the recognition that galaxies grow not in isolation but within a “cosmic ecosystem” that includes the vast reservoir of gas filling intergalactic space. This latter aspect in which galaxies continually exchange matter with the intergalactic medium via inflows and outflows has been dubbed the “baryon cycle”. The topic of this book is directly related to the baryon cycle, in particular its least well constrained aspect, namely gas accretion.

This textbook is intended as an introduction to the physics of solar and stellar coronae, emphasizing kinetic plasma processes. It is addressed to observational astronomers, graduate students, and advanced undergraduates without a back­ ground in plasma physics. Coronal physics is today a vast field with many different aims and goals. Sort­ ing out the really important aspects of an observed phenomenon and using the physics best suited for the case is a formidable problem.

Our purpose in writing this book is to show how physics has been applied to developing our current understanding of the phase structure, physical condi­ tions, chemical makeup and, evolution of the (thermal) interstellar medium. We hope it provides an up-to-date overview which postgraduates, advanced undergraduates, and professionals in astrophysics can use as a "reference of first resort" before going on to read the more specialist monographs or research literature.