"Tile; D'apC:Tile; l. DpWTa ()coi 7rpo7rapod)w GBP D'T}K,mi'. "between us and Goodness the gods have placed the sweat of our brows". This quote from Isiodos, the first lyrical poet, is jotted on a sheet of paper found among the papers of Heike Kamerlingh Onnes at the Boerhaave Museum, Leiden. On this same sheet, one can also read quotes from Schiller, Goethe, Shakespeare, Homer, Pindar and Dante. Each quote is for somebody or something. It appears to have been a game played at least by Ehrenfest and Crommelin -an unmistakable sign of these two physicists's deep culture. This particular quote was for the "Werkplaats", the Physical Laboratory of the University of Leiden. Our purpose in putting together the Selected Papers of its first Director, Kamerlingh Onnes (1853-1926), is to try and articulate the dominant trends of a different type of culture at Leiden: its physics culture during the years that established low temperature physics as a distinct branch of physics. Our aims in choosing the particular papers are threefold. First, we wish to present the interconnectedness among the different research programs of Kamerlingh Onnes and to bring out the decisive role of the work initiated by van der Waals in determining the direction of nearly all of these research programs.

High-contrast astronomical imaging has progressed significantly in the past decade. Many of these techniques have been laboratory demonstrated to perform at contrast levels adequate for the detection of Solar System-like planets and dust around nearby stars. None of them, however, have been demonstrated in space. The state of the art in high-contrast imaging systems that have been built for space-based observation, the environment best suited for spectroscopic study of exo-Earths, is the nulling interferometer that was flown on the Planetary Imaging Concept Testbed Using a Rocket Experiment (PICTURE). The PICTURE nulling interferometer, built from multiple optical elements, relies on the incorporation of additional dispersive components in order to deliver the broadband performance preferred for faint object imaging. These elements add to the cost, complexity, and misalignment risk of the instrument.
The Monolithic Achromatic Nulling Interference Coronagraph (MANIC) Brian Hicks describe in this thesis the first optic of its kind. He has taken the multiple optical element concept described in earlier works from theory to a flyable monolithic optic. Brian has advanced the state of the art in nulling interferometers by improving optical stability and robustness. Following application of the fabrication method described in this work, the design of MANIC also allows for broader band performance at higher contrast than that achieved with the PICTURE nulling interferometer.

In the 18th century, purely scientific interests as well as the practical necessities of navigation motivated the development of new theories and techniques to accurately describe celestial and lunar motion.

"Between Theory and Observations" presents a detailed and accurate account, not to be found elsewhere in the literature, of Tobias Mayer's important contributions to the study of lunar motion including the creation of his famous set of lunar tables, which were the most accurate of their time.

When the Apollo astronauts went to the moon, the whole world watched. When the Fly Me to the Moon art quilt challenge went out, it went global. This book showcases the curated results of that call for entries: 179 art quilts by over 130 artists from 8 countries, expressing their interpretation of the space program and all things lunar. Walk down memory lane or discover the story of the missions for the first time, but most importantly, enjoy a trip to the moon and beyond without the time and rigors of space training. As you travel into space, meet the astronauts, hum the tunes, and listen to the artists tell you about their pieces. Find endless inspiration and discover what the moon is really made of: cotton, thread, crystals, paint, ink, tulle, and crocheted lace.

Stellar pulsations provide a complex system in stars. This complexity is studied by analyzing the non-sinusoidal, semi-regular, or irregular light curves. This unique volume summarizes the application of recent theoretical results obtained from stellar pulsation studies. In addition, the latest developments in hydrodynamic simulations are discussed. A historical sketch of the study of beat Cepheids, first known for their variable amplitudes, is given as an introduction to the book. This introduction clearly demonstrates how complicated the study of variable stars can be, and therefore challenges and invites the reader to study the entire book.

One of the questions about which humanity has often wondered is the arrow of time. Why does temporal evolution seem irreversible? That is, we often see objects break into pieces, but we never see them reconstitute spontaneously. This observation was first put into scientific terms by the so-called second law of thermodynamics: entropy never decreases. However, this law does not explain the origin of irreversibly; it only quantifies it. Kinetic theory gives a consistent explanation of irreversibility based on a statistical description of the motion of electrons, atoms, and molecules. The concepts of kinetic theory have been applied to innumerable situations including electronics, the production of particles in the early universe, the dynamics of astrophysical plasmas, quantum gases or the motion of small microorganisms in water, with excellent quantitative agreement. This book presents the fundamentals of kinetic theory, considering classical paradigmatic examples as well as modern applications. It covers the most important systems where kinetic theory is applied, explaining their major features. The text is balanced between exploring the fundamental concepts of kinetic theory (irreversibility, transport processes, separation of time scales, conservations, coarse graining, distribution functions, etc.) and the results and predictions of the theory, where the relevant properties of different systems are computed.

This book presents experiments which will teach physics relevant to astronomy. The astronomer, as instructor, frequently faces this need when his college or university has no astronomy department and any astronomy course is taught in the physics department. The physicist, as instructor, will find this intellectually appealing when faced with teaching an introductory astronomy course. From these experiments, the student will acquire important analytical tools, learn physics appropriate to astronomy, and experience instrument calibration and the direct gathering and analysis of data. Experiments that can be performed in one laboratory session as well as semester-long observation projects are included.

Attilio Ferrari I want to recall here the basic points I raised at the beginning of the Workshop as the main targets of discussion (in the name of the Scientific Committee). I attempted to focus the attention of participants on the fact that, in many instances, we tend to discuss jets in terms of simple physics, more or less as one did at the time extragalactic radio sources were discovered: for instance, we still use equipartition arguments. However, we must realize that processes in jets, leading to their morphologies and energetics clearly depend on complex plasma phenomena. Therefore, the same standard arguments used to derive characteristic parameters should be questioned; some of the speakers were invited to attempt a critical analysis of this point, an~ in fact I believe that this "inquisitive attitude" was actually present all along the Workshop. Observers were asked to choose the parameters to be used in a statistical sample of jets. For this they were urged, first of all, to distinguish between primary and secondary features. For instance, are knots and wiggles common to all jets? Are relativistic flow velocities expected in all active nuclei? Are jets denser or lighter than the external medium? On the theoretical side I asked to discuss whether or not existing models are in accordance with the limited statistical sample that we have today. And which should be the lines of development to be pursued first, and to what extent.

This multiauthor book is a compilation of fourteen papers that result from activities within the scientific programme "Response of the Earth System to Impact Processes" (IMPACT) of the European Science Foundation. The program deals with all aspects of meteorite impact research and operates through workshops, exchange programs and short courses. Most of the papers are initiated from the 4th IMPACT workshop "Meteorite Impacts in Precambrian Shields" that took place in Lappajärvi, Finland, in 2000. The volume begins with a detailed view of thirty confirmed meteorite impact structures found in the Fennoscandian Shield and its nearest surroundings. The following papers describe impact structures in different areas.

In summary, we can conclude that the contributions of the different ionization processes to the total ionization rate for the most abundant interstellar species are basically known. The ionization of the noble gases He and Ne is almost completely dominated by photoionization, whereas for H charge-exchange with the solar wind is most important. For other species, such as 0 and Ar, both processes contribute significantly. Electron impact ionization can typically contribute by '" 10% to the total rate in the inner Solar System. Because direct measurements of the solar EUV flux are not yet continuously available, the variation of the ionization rate over the solar cycle still contains a relatively large uncertainty. The recent measurements of pickup ion distributions and of the neutral helium gas provide an independent tool to determine the total ionization rate that can be used to cross calibrate with the results obtained for the individual ionization processes. Acknowledgements The authors are grateful to M. Allen for supplying us with new data on photoioniza tion cross-sections compiled by him. We thank also M. Gruntman for drawing our attention to and support in collecting the most recent data on charge-exchange cross-sections. D. R. was supported by grant No. 2 P03C. 004. 09 from the Com mittee for Scientific Research (Poland). This work was also supported in part through NASA contract NAS7-918, NSF Grant INT-911637, NASA Grant NAGW- 2579.

Recombination lines at radio wavelengths have been - and still are - a pow erful tool for modern astronomy. For more than thirty years they have allowed astronomers to probe the gases from which stars form. They have even been detected in the Sun. In addition, observations of these spectral lines facilitate basic research into the atom, in forms and environments that can only exist in the huge dimensions and extreme conditions of cosmic laboratories. We intend this book to serve as a tourist's guide to the world of Radio Recombination Lines. It contains three divisions: a history of their discovery, the physics of how they form and how their voyage to us influences their spectral profiles, and a description of their many astronomical contributions to date. The appendix includes supplementary calculations that may be useful to some astronomers. This material also includes tables of line frequencies from 12 MHz to 30THz (AlOJLm) as well as FORTRAN computer code to calculate the fine structure components of the lines, to evaluate radial matrix integrals, and to calculate the departure coefficients of hydrogen in a cosmic environment. It also describes how to convert observational to astrophysical units. The text includes extensive references to the literature to assist readers who want more details."

This book contains lectures presented in the symposium on "wave Instabili ties in S: pace Plasmas" organized wi thin the progrem of .t.y . XIX URSI General Assembly held in Helsinki, Finland, during tJ: l

Three eminent scientists, each well known for the clarity of their writing, present for students and researchers what is known about the internal structure, origin and evolution of White Dwarfs, Neutron Stars and Black Holes, all objects at the final stage of stellar evolution. They cover fascinating topics such as pulsation of white dwarfs, millisecond pulsars or the dynamics around black holes. The book is written for graduate students in astrophysics, but is also of interest to professional astronomers and physicists.

This book tells the story of the evolution of the Satellite Center which started from a small Satellite Systems Division in 1967 with a handful of engineers to a vibrant R&D center which is playing the lead role in the Indian Satellite Program. India's space program is unique as it is driven by societal applications. The Indian Space Research Organisation (ISRO) has centers dedicated to various space applications. The ISRO Satellite Centre, now known as the UR Rao Satellite Centre (URSC), has evolved as lead center for Satellite Technology over five decades and has developed state-of-the-art satellites for applications such as remote sensing, satellite communication and space science. Through the story of URSC, the book describes the challenges of putting together new research and development centers and programs and conveys the importance of leadership and project management skills required to undertake such a task. This book is of interest to researchers, professionals, and administrators involved in the development of new R&D facilities and also to space scientists and space enthusiasts across the world.

How planets form is one of the long-standing questions in astrophysics. In particular, formation scenarios of planetesimals which are kilometer-sized bodies and a precursor of planets are still unclear and under debate although some promising mechanisms have been proposed. This book highlight disk instabilities that have the potential to explain the origin of planetesimals. Using linear analyses and numerical simulations, it addresses how a disk evolves through the development of instabilities, and also presents a new instability driven by dust coagulation. As a result, the simulation demonstrates a scenario of planetesimal formation: A successive development of multiple instabilities triggers planetesimal formation in resulting dusty rings.

The Symposium 'Meteorite Research' was conceived originally at the second meeting of the UNESCO Working Group on Meteorites, held in Paris October 18-20, 1965, under the chairmanship of Professor J. Orce ' In addition to the Chairman the fol lowing were present: Dr. G. Harbottle, Dr. M. H. Hey, Dr. B. H. Mason, Dr. P. M. Millman, Professor K. I. Sztr6kay. Dr. E. M. Fournier d'Albe represented the UNESCO Secretariat. Recommendation No.4 from the minutes of this meeting reads as follows: "The Working Group, in view ofthe need to strengthen international co-operation in meteorite research, asks that the International Atomic Energy Agency be requested to consider the possibility of organizing, in 1968, an interdisciplinary conference on meteorites, in collaboration with UNESCO and the appropriate international scientific organizations." After approval in principle of this recommendation had been secured from various international agencies and unions, plans for the symposium were consolidated at the third and final meeting of the Working Group, held in Paris October 12-14, 1966, the members in attendance being the same as for the second meeting."

This volume gives an overview of knowledge about the light nuclei created in the Hot Early Universe: H, D, 3He, 4He, and 7Li. It combines observational and theoretical results on the early Universe, the distant galaxies, our Milky Way, the local interstellar cloud, and the solar nebula. The implications for cosmology, galactic and stellar evolution, dark matter research etc. are outlined and directions of future research are indicated.

In the last few years great improvements in the study of stellar jets and bipolar outflows have been achieved, both observationally and theoretically. High resolution observations at various frequencies (radio, IR, optical and X-ray) of these features in different types of objects have shown a large variety of morphologies at all scales often revealing contrasting symmetries which do not allow straightforward kinematic interpretations valid for all cases. In particular, at present, it seems very difficult to give a statistical definition of what the "standard properties" of jets and bipolar outflows are. On the theoretical side, the identification of physical processes capable of producing the observed rich morphological variety of jets and bipolar outflows and supporting them over long lifetimes is still controversial. Furthermore several models are actively discussed in an attempt of reaching a complete understanding of the phenomenon. The workshop provided an unique opportunity for both observers and theoreticians to gather together and produce an updated and exhaustive picture of the field. In addition the meeting has been enriched by the presentation of some works on jets in external galaxies. This topic was focused on what people working on stellar jets could learn from colleagues working on extragalactic jets and vice versa. Invited papers were prepared with the aim of giving the state of the art about scientific subjects; contributed papers and some selected poster papers presented, on the contrary, very recent results in the various fields.

This unique , authoritative book introduces and accurately depicts the current state-of-the art in the field of space storms. Professor Koskinen, renowned expert in the field, takes the basic understanding of the system, together with the pyhsics of space plasmas, and produces a treatment of space storms. He combines a solid base describing space physics phenomena with a rigourous theoretical basis. The topics range from the storms in the solar atmosphere through the solar wind, magnetosphere and ionosphere to the production of the storm-related geoelectric field on the ground. The most up-to-date information available ist presented in a clear, analytical and quantitative way. The book is divided into three parts. Part 1 is a phenomenological introduction to space weather from the Sun to the Earth. Part 2 comprehensively presents the fundamental concepts of space plasma physics. It consists of discussions of fundamental concepts of plasma physics, starting from underlying electrodynamics and statistical physics of charged particles and continuing to single particle motion in homogeneous electromagnetic fields, waves in cold plasma approximation, Vlasov theory, magnetohydrodynamics, instabilities in space plasmas, reconnection and dynamo. Part 3 bridges the gap between the fundamental plasma physics and research level physics of space storms. This part discusses radiation and scattering processes, transport and diffiusion, shocks and shock acceleration, storms on the Sun, in the magnetosphere, the coupling to the atmosphere and ground. The book is concluded wtih a brief review of what is known of space stroms on other planets. One tool for building this briege ist extensive cross-referencing between the various chapters. Exercise problems of varying difficulty are embedded within the main body of the text.

I. Initial Angular Momentum Distribution.- Angular Momentum Effects in Star Formation.- Evolutionary Properties of Intermediate-Mass Protostar.- Small-Scale Structure and Angular Momentum Transfer in Protostellar Environments.- Ekman Pumping in a Rotating Protostar.- Rotation in Pre-Main Sequence Stars; Properties and Evolution.- Disks Associated with Intermediate Mass Stars.- Differential Rotation of Fully Convective Pre-Main Sequence Stars.- The X-ray Emission from PMS Stars in Taurus-Auriga, and the Relationship with Other Diagnostics of Activity.- Multifrequency Monitoring of RU Lupi; Observational Results and a Model.- Polarimetry and CCD Imaging of Herbig Ae/Be Stars and Star Forming Regions.- II: Angular Momentum Evolution.- Rotational Velocities of Low Mass Stars in Young Clusters.- Rotation of Young Stars in the Orion Nebula Region.- Rotational Velocities of Stars in Open Clusters; the Time-Dependence Revisited.- Main Sequence Angular Momentum Loss in Low-Mass Stars.- The Angular Momentum Evolution of Young and Old Binary Components.- Ages of Spotted Late-Type Stars.- Rotation of Evolved Stars.- Rotational Discontinuity of Evolved Stars; What Interpretation?.- III: Consequence of Rotation.- Magnetic Activity and Rotation.- Lithium, Rotation and Age.- Rotation, Chromospheric Activity, and Lithium Abundances in G and K Dwarfs of the Pleiades.- Lithium Abundance and Rotation in Southern Chromospherically Active Stars.- Lithium Depletion Induced by Rotation in Young Stars.- Rotational Mixing and Lithium in Young Stars.- IV: Internal Rotation and Models.- Internal Solar Rotation.- Stellar Activity Belts as Potential Indicators of Internal Rotation and Angular Momentum Distribution.- Dynamics of Spot Groups and Rotation of the External Convective Layers in the Sun and Magnetically Active Stars.- Theory of Magnetic Braking of Late-Type Stars.- Pre-Main Sequence and Main Sequence Rotational Evolution; Constraints on Models Derived from Observations.- Evolutionary Models of Rotating Stars.- The Internal Rotation of the Sun; Implications on the History of its Angular Momentum.- Angular Momentum Transport, Rotational Instabilities, Magnetic Fields and Mixing.- The Spin-Down of Main Sequence Stars Based on Observed Magnetic Field Strength.- Session V: Observational Perspectives.- Observational Perspectives.- PRISMA: a Space Facility for Studying Rotation and Activity.- The Spectrum-UV Project.- Summary of the Workshop.- Panel Discussion: Initial Angular Momentum.- Panel Discussion: Dynamos and Internal Rotation.- Author Index.- Object Index.

Habent sua Jata colloquia. The present volume has its ongms in a spring 1984 international workshop held, under the auspices of the Israel Academy of Sciences and Humanities, by The Institute for the History and Philosophy of Science and Ideas of Tel-Aviv University in cooperation with The Van Leer Jerusalem Foundation. It contains twelve of the twenty papers presented at the workshop by the twenty-six participants. As Proceedings of conferences go, it is a good representative of the genre, sharing in the main characteristics of its ilk. It may even be one of the rare instances of a book of Proceed ings whose descriptive title applies equally well to the workshop's topic and to the interrelations between. the various papers it includes. Tension and Accommodation are the key words. Thus, while John Glucker's paper, 'Images of Plato in Late Antiqu ity, ' raises, by means of the Platonic example, the problem of interpreta tion of ancient texts, suggesting the assignment of proper weight to the creator of the tradition and not only to his many later interpreters in assessing the proper relationship between originator and commentators, Abraham Wasserstein's 'Hunches that did not come off: Some Prob lems in Greek Science' illustrates the long-lived Whiggish tradition in the history of science and mathematics. As those familiar with my work will undoubtedly note, Wasserstein's position is far removed from my stance on ancient Greek mathematics."