Analyses of photometric time series obtained from the MOST, CoRoT and Kepler space missions were presented at the 20th conference on Stellar Pulsations (Granada, September 2011). These results are leading to a re-appraisal of our views on stellar pulsation in some stars and posing some new and unexpected challenges. The very important and exciting role played by innovative ground-based observational techniques, such as interferometric measurements of giant pulsating stars and high-resolution spectroscopy in the near infrared, is also discussed. These Proceedings are distinguished by the format of the conference, which brings together a variety of related but different topics not found in other meetings of this nature.

The open cluster NGC 6791 is now considered both the oldest and the most metal-rich known. Its age is 8 -10 Gyrs, twice as old as the canonical solar-metallicity cluster M67 (Garnavich et al. 1994; Demarque, Green, & Guenther 1992; Tripicco et al. 1995). That its metallicity is significantly above solar is suggested from moderate-resolution spectroscopy and from a mismatch of its color-magnitude diagram (CMD) with solar-metallicity isochrones. Tripicco et al. (1995) find [Fe/H] = +0.27 to +0.44. The cluster population is rich. In addition to about a dozen red giants and two dozen red horizontal-branch stars, the cluster has several very hot HB stars (Kaluzny & Udalski 1992). Liebert et al. (1994) have shown that the extremely blue stars are mostly sdB/sdO stars and at least 3 or 4 are likely cluster members, the first ever discovered in an open cluster. These may provide the key to the puzzling upturn in ultraviolet flux below 1500A seen in many high-metallicity systems (Burstein et al. 1988; Ferguson et al. & Liebert 1993).

Symposium No. 73 of the International Astronomical Union was devoted to the obser vational and theoretical aspects of close binary stars. Just over 100 participants attended. The Local Organizing Committee would like to thank the following: IAU for travel grants. IBM United Kingdom Ltd for very generous support in the form of travel grants. The Royal Society for the provision of travel grants to participants from Eastern Europe. We also thank the Director of the Institute of Astronomy, and our colleagues and research students for their moral support and assistance. Finally we thank Pauline Haughey for assisting with the editorial work. PETER EGGLETON SIMON MITTON JOHN WHELAN SCIENTIFIC ORGANIZING COMMITTEE M. Plavec (Chairman), T. Herczeg, E. P. J. van den Heuvel, J. B. Hutchings, G. Larsson-Leander, L. B. Lucy, L. Mestel, B. Paczynski, J. Sahade, B. Warner, R. E. Wilson. LOCAL ORGANIZING COMMITTEE J. A. J. Whelan (Chairman), P. P. Eggleton, S. A. Mitton LIST OF PARTICIPANTS Baldwin, B. W., Victoria, Canada Icke, V., Cambridge, England Bateson, F. M., Tauranga, New Zealand Koumsiachvilli, M., Moscow, U.S.S.R Bath, G. T., Oxford, England Krzeminski, W. A., Warsaw, Poland Batten, A. H., Victoria, Canada Larsson-Leander, G., Lund, Sweden Berthier, E. J., Paris, France Leung, K.-C., Nebraska, U.S.A."

This is the first scholarly collection of articles focused on the cultural astronomy of the African continent. It weaves together astronomy, anthropology, and Africa and it includes African myths and legends about the sky, alignments to celestial bodies found at archaeological sites and at places of worship, rock art with celestial imagery, and scientific thinking revealed in local astronomy traditions including ethnomathematics and the creation of calendars.

This book is the fourth volume under the title Organizations and Strategies in Astronomy (OSA). These OSA Books are intended to cover a large range of fields and themes. In practice, one could say that all aspects of astronomy-related life and environment are considered in the spirit of sharing specific expertise and lessons learned.
This book offers a unique collection of chapters dealing with socio-dynamical aspects of the astronomy (and related space sciences) community: characteristics of organizations, society activities, strategies for development, operational techniques, observing practicalities, environmental constraints, educational policies, public outreach, journal and magazine profiles, publication studies, electronic-media problematics, research communication, evaluation and selection procedures, research indicators, national policies and specificities, expertise sharing, contemporary history, and so on.
The experts contributing to this book have done their best to write in a way understandable to readers not necessarily hyperspecialized in astronomy while providing specific detailed information and sometimes enlightening 'lessons learned' sections. The book concludes with an updated bibliography of publications related to socio-astronomy and to the interactions of the astronomy community with the society at large.
This book will be most usefully read by researchers, teachers, editors, publishers, librarians, sociologists of science, research planners and strategists, project managers, public-relations officers, plus those in charge of astronomy-related organizations, as well as by students aiming at a career in astronomy or related space science.

"Astrochemistry and Astrobiology" is the debut volume in the new series "Physical Chemistry in Action." Aimed at both the novice and experienced researcher, this volume outlines the physico-chemical principles which underpin our attempts to understand astrochemistry and predict astrobiology. An introductory chapter includes fundamental aspects of physical chemistry required for understanding the field. Eight further chapters address specific topics, encompassing basic theory and models, up-to-date research and an outlook on future work. The last chapter examines each of the topics again but addressed from a different angle. Written and edited by international experts, this text is accessible for those entering the field of astrochemistry and astrobiology, while it still remains interesting for more experienced researchers.

In recent years aperture synthesis and interferometry have become very powerful tools in radioastronomy. Investigation of distant galaxies, for example, have revealed structures with sizes of less than a kiloparsec. In general, the study of galaxies has benefited from the great power of these techniques. Radar applications have also dramatically increased their quality by using the interferometry principle. Tracking and airborne radar can now determine position and velocity of objects with a much higher accuracy. This book describes in the first six, short chapters the basics of interferometry and aperture synthesis. The following two, long chapters treat the aspects of radioastronomical interferometers and radar applications of interferometry in great detail. The text offers readers a very good opportunity to familiarize themselves with the mathematical background of these very complex techniques. For researchers and students in radioastronomy and electrical engineering.

Present and Future of Nuclear Physics; Introductory Lecture. Cluster Decay, Fission and Fusion: Cluster Radioactivity; P.B. Price. Recent Advances in Cluster Radioactivities; D.N. Poenaru, W. Greiner. Heavy Elements: Multinucleon Transfer Reactions-An Alternative Path to Heavy Element Synthesis; M.T. Magda. Microscopic and Semi-microscopic Approach to the Properties of Transactinide Nuclei; L. Bitaud, et al. Nuclear Structure: On the Origin of Rotations and Vibrations in Atomic Nuclei; J.P. Draayer, et al. Particle-rotor Model Description of Deformed Nuclei; A. Covello, et al. Weak Interaction and Double Beta Decay: Nuclear Aspects of Double Beta Decay; S. Stoica. A New Look to the Nuclear Structure Calculations of the PNC Cases in A=1821 Nuclei; M. Horoi. Nuclear Astrophysics: Recent Topics from Nuclear Reactions in the Energies Ranging from keV to GeV; K. Kubo. Heavy Ion Collisions: Processes in Peripheral Ultrarelativistic Heavy Ion Collisions; M. Greiner, et al. Miscellaneous Topics: Gamma and Meson Production by Cherenkovlike Effects in Nuclear Media; W. Stocker, D.B. Ion. 58 additional articles. Index.

The recent meeting of the world's white dwarf specialists was held in Leicester, in July 1992, reporting on the wealth of astronomical data that has been made available from a new generation of space-based observatories and recent theoretical advances which are essential for interpretation of the results. Astronomers now have access to previously unavailable spectral ranges and dramatically improved sensitivity in those wavebands already explored. Results from the ROSAT all-sky survey, Hubble Space Telescope, Hopkins Ultraviolet Telescope and the Colorado Rocket-borne Spectrometer shed new light on the composition of white dwarfs and their evolution. Considerable progress has been made in understanding the internal structure of white dwarfs with asteroseismological techniques which are outlined in several papers. New observational results, which utilize this theoretical work are also presented. This text is suitable for graduate students and postdoctoral researchers interested in isolated white dwarfs or binary systems containing a white dwarf component.

This thesis presents the results of indirect dark matter searches in the gamma-ray sky of the near Universe, as seen by the MAGIC Telescopes. The author has proposed and led the 160 hours long observations of the dwarf spheroidal galaxy Segue 1, which is the deepest survey of any such object by any Cherenkov telescope so far. Furthermore, she developed and completely characterized a new method, dubbed "Full Likelihood", that optimizes the sensitivity of Cherenkov instruments for detection of gamma-ray signals of dark matter origin. Compared to the standard analysis techniques, this novel approach introduces a sensitivity improvement of a factor of two (i.e. it requires 4 times less observation time to achieve the same result). In addition, it allows a straightforward merger of results from different targets and/or detectors. By selecting the optimal observational target and combining its very deep exposure with the Full Likelihood analysis of the acquired data, the author has improved the existing MAGIC bounds to the dark matter properties by more than one order of magnitude. Furthermore, for particles more massive than a few hundred GeV, those are the strongest constraints from dwarf galaxies achieved by any gamma-ray instrument, both ground-based or space-borne alike.

Digital sky surveys, data from orbiting telescopes, and advances in computation have increased the quantity and quality of astronomical data by several orders of magnitude in recent years. Making sense of this wealth of data requires sophisticated statistical and data analytic techniques. Fortunately, statistical methodologies have similarly made great strides in recent years. Powerful synergies thus emerge when astronomers and statisticians join in examining astrostatistical problems and approaches. The volume focuses on several themes: · The increasing power of Bayesian approaches to modeling astronomical data · The growth of enormous databases, leading an emerging federated Virtual Observatory, and their impact on modern astronomical research · Statistical modeling of critical datasets, such as galaxy clustering and fluctuations in the microwave background radiation, leading to a new era of precision cosmology · Methodologies for uncovering clusters and patterns in multivariate data · The characterization of multiscale patterns in imaging and time series data As in earlier volumes in this series, research contributions discussing topics in one field are joined with commentary from scholars in the other. Short contributed papers covering dozens of astrostatistical topics are also included.

Jupiter's ice moon Europa is widely regarded as the most likely place to find extraterrestrial life. This book tells the engaging story of Europa, the oceanic moon. It features a large number of stunning images of the ocean moon's surface, clearly displaying the spectacular crack patterns, extensive rifts and ridges, and refrozen pools of exposed water filled with rafts of displaced ice. Coverage also features firsthand accounts of Galileo's mission to Jupiter and its moons. The book tells the rough and tumble inside story of a very human enterprise in science that lead to the discovery of a fantastic new world that might well harbor life.

Our Galactic center's proximity allows astronomers to study physical pro cesses within galactic nuclei at a level of detail that will never be possible in the more distant, but usually also more spectacular, extragalactic systems. Recent advances in instrumentation from the radio, through the submillime ter and infrared wavebands, and out to the X- and "'(-ray bands now allow observations of the Galactic Center over thirteen orders of magnitude in wave length. Our knowledge about the central few hundred parsecs of our Galaxy has consequently increased vastly over the past decade. The same new instru ments provide high resolution, high quality measurements of nearby ''normal'' galactic nuclei; that is, nuclei whose modest energy output is comparable to that of our own (and most other) galaxies. Theorists, spurred in part by the new observations, have been able to refine models of the energetics, dynam ics, and evolution of the gas and stellar systems deep within galactic nuclei."

I. Current Missions.- The Hubble Space Telescope.- Early Results from the Cosmic Background Explorer (COBE).- The Status of the DIRBE Instrument on the COBE.- The Automatic Spacecraft Granat.- The Hipparcos Mission: Will It Be a Scientific Success?.- The International Ultraviolet Explorer (IUE).- X-Ray Astronomy Satellite Ginga.- Extreme and Far Ultraviolet Astronomy from Voyagers 1 and 2.- II. Future Missions.- Roentgen Satellite.- The Gamma-Ray Observatory.- The Advanced X-Ray Astrophysics Facility.- The Astro-D Mission.- The X-Ray Timing Explorer.- The Joint European Telescope for X-Ray Astronomy (JET-X).- SODART Telescope on Spectrum-Roentgen-Gamma and Its Instrumentation.- ESA's X-Ray Astronomy Mission, XMM.- The SAX Mission for X-Ray Astronomy.- The Extreme Ultraviolet Explorer Mission.- Lyman the Far Ultraviolet Spectroscopic Explorer.- Far and Extreme Ultraviolet Astronomy with Orfeus.- The Spectrum - UV Project.- The Space Infrared Telescope Facility (SIRTF).- The Infrared Space Observatory.- IRTS: Infrared Telescope in Space.- FIRST - Far Infrared and Submillimetre Space Telescope.- A Submillimeter Mission for the 1990s: SMMM.- The Submillimeter Wave Astronomy Satellite.- International VLBI Satellite (IVS).- VSOP, A Space VLBI Programme.- VLBI with TDRSS.- SOHO - An Observatory to Study the Solar Interior and the Solar Atmosphere.- An Overview of the Orbiting Solar Laboratory.- The Planetenteleskop Mission.- The Astrometric Imaging Telescope: Near-Term Discovery and Study of Other Planetary Systems.- Ultraviolet Polarimetry.- The Hopkins Ultraviolet Telescope.- The Ultraviolet Imaging Telescope for Astro 1.- The Broad Band X-Ray Telescope (BBXRT) on Astro-1.- Future Solar System Missions.- The Ulysses Mission in the High Latitude Heliosphere.- Science Operations for Future Space Astrophysics Missions.- III. Launch Vehicles.- United States Launch Vehicle Systems.- ESA's Space Transportation Programme.- Launch Vehicles of ISAS.- U.S.S.R. LAUNCH SYSTEMS 343.- Launch Vehicles of the Future: Earth to Near-Earth Space.- Future Deep Space Propulsion Systems.- IV. Relative Merits of Various Observatories.- Lunar-Based Astronomy.- Relative Merits of Low-Earth, Eccentric, Geosynchronous, and Interplanetary Orbits and Sites in Space.- Humanity or Robotics in Space?.- Astrophysics from the Moon.- Use of Libration-Point Orbits for Space Observatories.- Major Observatories Versus Economy-Class Observatories in Space.- V. Long Term Future Issues.- Does Theory Advance with Technology?.- Occultation Astronomy.- Comments.- The Astrophysics of the Future.- Evolution of the Unsolved Problems.- Contributed Papers.- SIXA: The Solid State Spectrometer Array Onboard Spectrum-X-Gamma.- The X-Ray Large Array.- The Stellar X-Ray Polarimeter for the Spectrum-X-Gamma Mission.- The All-Sky Extragalactic X-Ray Foreground.- A Low Energy Gas Scintillation Proportional Counter for the SAX-X-Ray Astronomy Satellite.- The EXOSAT Results Database.- An X-Ray All Sky Monitor for a Japanese Experimental Module on the Space Station.- The Astro Mission.- The UV Imager for the Israeli Scientific Satellite.- ORFEUS-SPAS: The Berkeley EUV Spectrometer.- An Observatory for Mapping the Far UV Diffuse Galactic Emission Line Background.- Project of a Three Reflection Telescope for Wide Field Ultraviolet Observations.- Santa Maria: An Orbiting Multispectral Observatory.- Cryogenic Testing of Optics for ISOCAM.- EDISON: A Second Generation Infrared Space Observatory.- Merits of Space VLBI Missions for Geodynamics.- Low Frequency Radio Astronomy from Earth Orbit.- High-Resolution Imaging Spectroscopy at TeraHertz Frequencies.- Science Observations with the IUE Using the One Gyro Mode.- New Methods of Determining Spacecraft Attitude.- Knowledge Based Automated Scheduling and Planning Tools for IUE.- Earth Observation System Plans of India.- The Stability of the Planetary Triangular Lagrange Points.- Cosmic Rays and the Dynamic Balance in the Large Magellanic Cloud.- Li

Astronomers communicate all the time, with colleagues of course, but also with managers and administrators, with decision makers and takers, with social representatives, with the news media, and with society at large. Education is naturally part of the process. Astronomy communication must take into account several specifics: the astronomy community is rather compact and well organized world-wide; astronomy has penetrated the general public remarkably well with an extensive network of associations and organizations of aficionados all over the world. Also, as a result of the huge amount of data accumulated and by necessity for their extensive international collaborations, astronomers have pioneered the development of distributed resources, electronic communications and networks coupled to advanced methodologies and technologies, often long before they become commonly used world-wide.
This book is filling a gap in the astronomy-related literature by providing a set of chapters not only of direct interest to astronomy communication, but also well beyond it. The experts contributing to this book have done their best to write in a way understandable to readers not necessarily hyperspecialized in astronomy nor in communication techniques while providing specific detailed information, as well as plenty of pointers and bibliographic elements.
This book will be very useful for researchers, teachers, editors, publishers, librarians, computer scientists, sociologists of science, research planners and strategists, project managers, public-relations officers, plus those in charge of astronomy-related organizations, as well as for students aiming at a career in astronomy or related spacescience.

The purpose of this book is to give a detailed description of the planetary nebulae including the relevant astronomical observations and their interpretation. Considerable attention is given to the evolution of these objects as well as to their physical characteristics. I t is hoped that the book be useful to both advanced research workers and to students with some background in astronomy. In this regard, the book should serve as a text as well as a reference work. The many tables included are expected to be useful for both purposes. The references are generally not included in the text except for historical purposes in an effort to improve readability. References are given at the end of each chapter together with sufficient text to describe their content. No attempt has been made to make the list of references complete; on the contrary it has generally been limited to the most recent literature on the subject which in turn refers to earlier research. Again, exceptions have been made for references of historical interest.

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. This book provides three stages in the solution of the solar flare problem. Chapter one describes the connection between observational data and theoretical concepts, where it is stressed that next to investigating flares, the related non-stationary large-scale phenomena must be studied as well. The second chapter deals with secondary physical processes, in particular the study of high-temperature plasma dynamics during impulsive heating. The last chapter presents a model built on the knowledge of the two previous chapters and it constructs a theory of non-neutral turbulent current sheets. The author believes that this model will help to solve the problem of solar flares. For solar physicists, plasma physicists, high-energy particle physicists.

If standard gravitational theory is correct, then most of the matter in the universe is in an unidentified form which does not emit enough light to have been detected by current instrumentation. This proceedings was devoted to a discussion of the so-called "missing matter" problem in the universe. The goal of the School was to make current research work on unseen matter accessible to students of faculties without prior experience in this area. Due to the pedagogical nature of the School and the strong interactions between students and the lectures, the written lectures included in this volume often contain techniques and explanations not found in more formal journal publications.

This thesis presents studies of the starless core populations of three nearby molecular clouds made as part of the James Clerk Maxwell Telescope Gould Belt Survey. These studies combine observations made using the SCUBA-2 submillimetre camera with data from several other instruments, including the Herschel Space Observatory, to identify and characterise starless cores in the Ophiuchus, Taurus and Cepheus molecular clouds. The temperatures, masses and stability against collapse of the starless cores are measured, the latter through detailed virial analysis, including a determination of the external pressure on the cores. The book illustrates core stability on the "virial plane", in which core stability is plotted against core confinement mode, showing that starless cores are typically confined by external pressure rather than self-gravity. It also presents an analytical model of the evolution of starless cores in the "virial plane", demonstrating that a pressure-confined starless core may evolve due to virial stability rather than gravitational collapse, which means that a core can only be definitively considered to be prestellar if it is gravitationally bound.

This work investigates the theoretical and cosmological implications of modifying Einstein's theory of general relativity. It explores two classes of modifications to gravity: those in which the graviton is given a small mass, and those in which Lorentz invariance is spontaneously broken. It elucidates the nature of cosmological perturbations in theories of massive bimetric gravity, including a potentially deadly instability. Theories of gravity beyond general relativity could explain why the expansion of the Universe is accelerating, obviating the need for a dark energy, and can also affect the evolution of the early Universe. Next, it investigates the nature of spacetime in massive gravity theories that contain two different spacetime metrics. Lastly, the strongest constraints to date are placed on the size of Lorentz-violating effects in the gravity sector during inflation.

Our knowledge of the heliosphere in three dimensions near solar minimum has advanced significantly in the last 10 years, largely as a result of the on-going ESAINASA Ulysses mission. Similar advances in our understanding of the global heliosphere near solar maximum are to be expected with the return of Ulysses to high solar latitudes in 2000/200 I. With this in mind, the 34th ESLAB Symposium, held at ESTEC in Noordwijk, The Netherlands, on 3-6 October, 2000, was devoted to 'The 3-D Heliosphere at Solar Maximum'. This was the third ESLAB Sympo sium focusing on the three-dimensional heliosphere (previous symposia being in 1985 and 1994), and the timing was particularly appropriate, marking as it did the 10th anniversary of the launch of the Ulysses spacecraft. Furthermore, Ulysses had just started its third high-latitude pass, the second over the Sun's south polar regions. The symposium addressed a wide range of topics related to the solar-maximum heliosphere, with presentations on many of the latest findings from Ulysses and other space-based missions. Ground-based studies and theoretical modeling were also well represented. Specific questions to which answers were sought included the following.

This volume presents the current knowledge of magnetic fields in diffuse astrophysical media. Starting with an overview of 21st century instrumentation to observe astrophysical magnetic fields, the chapters cover observational techniques, origin of magnetic fields, magnetic turbulence, basic processes in magnetized fluids, the role of magnetic fields for cosmic rays, in the interstellar medium and for star formation. Written by a group of leading experts the book represents an excellent overview of the field. Nonspecialists will find sufficient background to enter the field and be able to appreciate the state of the art.

These proceedings of a workshop held at Isle-aux-Coudres, Quebec, Canada in August 1993, provide an assessment of a fundamental subject in modern stellar astrophysics. Hot, luminous stars play a crucial role in the rapid recycling of matter in dense regions of the Universe. The most luminous objects generate the strongest outflows of material, which in turn have a profound impact on both the interstellar medium and the underlying stars themselves. However, recent observational and theoretical advances have shown that these outflows are highly unstable and inhomogeneous. These characteristics constitute a fundamental property of the outflows that can no longer be disregarded. This text provides an assessment of this important phenomenon from both an observational and a theoretical perspective. It includes up-to- date discussions of the observational diagnostics of time-dependent stellar-wind structure, the theoretical understanding of the origin of such structures, and its consequences for the process of mass loss via stellar winds.