Astrophysics and Space Science Library – serie
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Recombination lines at radio wavelengths have been - and still are - a p- erful tool for modern astronomy. For more than 30years, 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 in?uences their spectral pro?les, and a description of their many astronomical contributions todate.Theappendixincludessupplementarycalculationsthatmaybeuseful to some astronomers. This material also includes tables of line frequencies from 12MHz to 30THz (?=10?m) as well as FORTRAN computer code to calculate the ?ne-structure components of the lines, to evaluate radial matrix integrals, and to calculate the departure coe?cients of hydrogen in a cosmic environment. It also describes how to convert observational to astrophysical units.The textincludes extensive referencestothe literature toassistreaders who want more details.We appreciate the help of L.W. Avery, D.S. Balser, T.M. Bania, T. Bastian, J.H. Bieging, H.J.J. Blom, N.G. Bochkarev, R.L. Brown, L.A. Bureeva (Minaeva), W.B. Burton, T. Alan Clark, Z.F. Dravskikh, W.C.
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It was with pleasure that CAUP became for three days the core to the cloud of star formation experts all over the world. Close to the celebration of its 15th anniversary – therefore still in the early stages of institutional evolution – we are proud of our multiple activities in Astronomy: a productive research centre, classi?ed as “Institution of excellence” within the Portuguese research units, but also an “Institution of Public Utility” as recognised by the Government. Fifteen years ago we choose to play a role not only in research, as expected from any research centre but also in the training of the future astronomers and the promotion of science and scienti?c culture. This choice is clearly stated in our by-laws and also in the multiple activities we have carried out since. Along the years we have organized on a regular basis international Workshops similar to “Cores to Clusters”. Sometimes we have chosen to organize int- national conferences of a larger size. On other occasions the choice has been for smaller and more informal discussion meetings. Or even doctoral schools with very different objectives. In common all those meetings have always had, besides the formal registered participants, a group of informal participants, our undergraduate students of Astronomy, so eager to be in touch with the real world.
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Neutron stars play a unique role in physics and astrophysics. On the one hand, they contain matter under extreme physical conditions, and their theories are based on risky and far extrapolations of what we consider reliable physical theories of the structure of matter tested in laboratory. On the other hand, their observationsoffertheuniqueopportunitytotestthesetheories. Moreover, n- tronstarsareimportantdramaticpersonaeonthestageofmodernastrophysics; they participate in many astronomical phenomena. ?3 Neutronstarscontainthematterofdensityrangingfromafew g cm attheir 15 ?3 surface, where the pressure is small, to more than 10 gcm at the center, 36 ?2 wherethepressureexceeds10 dyncm . Tocalculateneutronstarstructure, one needs the dependence of the pressure on density, the so called equation of state (EOS), in this huge density range, taking due account of temperature, 9 more than10 K in young neutron stars, and magnetic ?elds, sometimes above 15 10 G. The present book is mainly devoted to the theory of the EOS of neutron star matter and its consequences for neutron star structure. As one moves from the neutron star surface to the center, the methods to calculate the EOS change. Atomic structure and plasma theories are used for the surface stellar layers. Deeper layers of the neutron star crust require nuclear theory combined with plasma physics, both in very exotic density-temperature regimes. Finally, the neutron star core necessitates many-body theory of dense strongly interacting systems,togetherwiththephysicsofstronginteractionsofelementaryparticles.
Del 342 - Astrophysics and Space Science Library
Astrophysics of Emission-Line Stars
Inbunden, Engelska, 2007
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Many types of stars show conspicuous emission lines in their optical spectra. These stars are broadly referred to as emission line stars. Emission line stars are attractive to many people because of their spectacular phenomena and their amazing varieties and variability. This book offers general information on emission line stars, starting from a brief introduction to stellar astrophysics, and then moving to a broad overview of emission line stars including early and late type stars as well as pre-main sequence stars. Detailed references and index are prepared for further reading. Tomokazu Kogure's email address: tkogure@pa2.so-net.ne.jp
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The book is written mainly to advanced graduate and post-graduate students following courses in Perturbation Theory and Celestial Mechanics. It is also intended to serve as a guide in research work and is written in a very explicit way: all perturbation theories are given with details allowing its immediate application to real problems. In addition, they are followed by examples showing all steps of their application.
Del 346 - Astrophysics and Space Science Library
Exploring the Secrets of the Aurora
Häftad, Engelska, 2007
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Prominent progress in science is inevitably associated with controversies. Thus, young researchers, in particular, have to learn how to persevere during the period of controversy and struggle for acceptance. Unfortunately, the skills needed are not taught in textbooks or monographs, which mostly describe the consensus of contemporary experts.This book, which is based on my own experiences as a scientist, describes the history of the progress made in auroral science and magnetospheric physics by providing examples of ideas, controversies, struggles, acceptance, and success in some instances.Although no general methodology (if any exists) is mentioned, I hope that the reader will learn about the history of progress in auroral science and examples (right or wrong) of dealing with the controversies.
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The book should be of use to all who are involved in the design and calibration of large antennas, like ground station managers and engineers, practicing radio astronomers and graduate students in radio astronomy and communication technology.
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This book presents a complete summary of the author's twenty five years of experience in telescope design. It provides a general introduction to every aspect of telescope design. It also discusses the theory behind telescope design in depth, which makes it a good reference book for professionals.
Del 361 - Astrophysics and Space Science Library
Sun Recorded Through History
Inbunden, Engelska, 2009
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The Sun is nowadays observed using di?erent techniques that provide an almost instantaneous 3-D map of its structure. Of particular interest is the studyofthevariabilityinthesolaroutputproducedbythedissipationofm- netic energy on di?erent spatial and temporal scales – the so-called magnetic activity. The 11-year cycle is the main feature describing this phenomenon. Apart from its intrinsic scienti?c interest, this topic is worth studying because of the interaction of such processes with the terrestrial environment. A ?eet of space and ground-based observatories are currently monitoring the behaviour of our star on a daily basis. However, solar activity varies not only on this decadal time-scale, as has been attested mainly through two methods: (a) records of the number of sunspots observed on the solar surface from 1610, and (b) the records of 14 10 cosmogenic isotopes, such as Cand Be, measured in tree-rings and i- cores, respectively. The study of the long-term behaviour of solar activity may be comp- mented by the study of historical accounts describing phenomena directly or indirectly related to solar activity. Numerous scienti?c and non-scienti?c d- uments have reported these events and we can make use of them as a proxy of solar activity in past times.
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The words of this preface were written when the book was ready to go to the press; and are limited to only a few points which are best made in this place. As is intimated by the sub-title, the whole volume was written with appli cations in mind to double-star astronomy. The latter is, however, not the only branch of our science which could benefit from its contents. The same is true of certain aspects of the dynamics of stellar systems or galaxies (the stellar popula tions of which are also characterized by the fact that the mean-free-path of their constituent stars are long in comparison with the dimensions of the respective systems); the central condensations of which are high enough to approximate the gravitational action of a "mass-point". This fact did not, to be sure, escape the attention of previous investigators (in the case of globular clusters, in particular, the Roche model was introduced in their studies under the guise of polytropic models characterized by the index n = 5); though no particular attention will be paid to these in this book. But possible applications of the Roche model are not limited to problems arising in stellar astrophysics. With Coulomb forces replacing gravitation, the equilibrium model finds a close analogy in the field of electrostatics-as was pointed out already at the beginning of this century by (then young) J. H. Jeans (cf.
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This publication is a result of three meetings, each 5 days long, held at the Goddard Space Flight Center on January 24-28, 1983, June 8-14, 1983, and February 13-17, 1984. The meetings were held in the interim between the full operations of the Solar Maximum Mission (SMM) in 1980, and the renewed operations after its repair in orbit in April 1984. Their general objectives were as follows: o Synthesize flare studies after three years of SMM data analysis. Many analyses of individual flares and individual phenomena, often jointly across many data sources had been published, but a need existed for a broader synthesis and updating of our understanding of solar flares since the Skylab Flare Workshops held several years earlier. o Encourage a broader participation in the SMM data anlysis and combine this more fully with theory and other data sources--data obtained with other spacecraft such as the HINOTORI, P78-1, and ISEE-3 spacecrafts, and with the Very Large Array (VLA) and many other ground-based instruments. Many coordinated data sets, unprecedented in their breadth of coverage and multiplicity of sources, had been obtained within the structure of the Solar Maximum Year (SMY). o Stimulate joint studies, and publication in the general scientific literature. The intended primary benefit was for informal collaborations to be started or broadened at the Workshops with subsequent publications. o Provide a special publication resulting from this Workshop. o Provide a starting point of understanding for planning renewed full observations with the repaired SMM.
Accretion Disks and Magnetic Fields in Astrophysics
Proceedings of the European Physical Society Study Conference, Held in Noto (Sicily), Italy, June 16–21, 1988
Inbunden, Engelska, 1989
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The present volume colleets the review and contributed papers presented at the Europhysics Study Conferenee "Acere- tion Disks and Magnetie Fields in Astrophysies" held in Noto, Sicily, Italy, from 16 to 21 June 1988, under the High Patronage of the President of the Italian Republie and the 10ea1 patronage of the Cent ro di Studi Superiori e di Rieer- ehe (Center for Advaneed Study and Research), a seientific institution supported by the City of Nota and the Oniversity of Catania. The attendanee to the Conferenee was limited to about fifty seleeted partieipants from Canada, China, Denmark, Franee, Germany F.R., Italy, Japan, the Netherlands, Spain, Sl~itzerland. Onited Kingdom and Onited States, in order to give the meeting the character and appearance of areal lolorkshop, whose main aim was to highl ight a varied but same wh at uni fied picture of the interact ion, in di fferent astrophysical systems, of rotation, turbulenee and magnetism, with speeifie referenee to aeeretion disks.
Submillimetre Astronomy
Proceedings of the Kona Symposium on Millimeter and Submillimetre Astronomy, Held at Kona, Hawaii, October 3–6, 1988
Inbunden, Engelska, 1990
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G. M. Bernstein, M. L. Fischer, and P. L. Richards Department of Physics, University of California Berkeley, California 94720, U. S. A. J. B. Peterson Department of Physics, Princeton University Princeton, New Jersey 08540, U. S. A. T. Timusk Department of Physics, McMaster University Hamilton, Ontario L8S 4M1 , Canada ABSTRACT. Recent measurements of the diffuse background at millimeter wavelengths indicate no departure from a Planck spectrum near the peak of the blackbody curve. Anisotropy measurements indicate no structure, at the 2% level, in the recently detected submillimeter excess. We report here the results of an April 1987 balloon flight of an instrument designed to measure the spectrum of the cosmic background radiation from 1 mm to 3 mm. A description of the instrument can be found in Peterson, Richards, and Timusk (1985). Modifications were made to the apparatus and experimental procedure in order to identify and reduce systematic errors. Results from the latest flight indicate that two effects hamper the interpretation of the data. These systematic effects will be described in detail in a forthcoming publications; they are probably responsible for the non-Planckian spectrum measured by Woody and Richards (1981). Attempts to remove the systematic effects from our data yield the upper limits to the CBR brightness temperature in 4 bands from 1 mm to 3 mm. There is no evidence for an excess of radiation near the 2. 8 K blackbody peak.
Del 161 - Astrophysics and Space Science Library
Interstellar Medium in Galaxies
Häftad, Engelska, 1990
537 kr
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This book contains the proceedings of the sixth Eurographics Workshop on Vir tual Environments. The event took place from June 1 to June 2, 2000, in Am sterdam. We hope that readers will find these proceedings to be valuable, not only for virtual environment researchers, but also for practitioners developing or using virtual environment applications. We are glad to report that visibility of the workshop continues to expand and that virtual environment researchers and practitioners from allover the world are submitting papers. This year, 40 papers and case studies were submitted of which 20 were accepted. In addition, we are glad to see that the focus of the workshop is also expanding. We accepted 6 research papers on evaluation of virtual environments and there was a broad sampling of other topics. We would like to thank all those involved in organizing the symposium. In particular, thanks go to Mieke Brune who was in charge of the local organization. In addition, we want to thank the international program committee for their excellent, yet laborious, job in reviewing all submitted papers. The quality of the workshop is a reflection of the quality of the submitted papers and the quality of the reviewing process.
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Comets in the Post-Halley Era
In Part Based on Reviews Presented at the 121st Colloquium of the International Astronomical Union, Held in Bamberg, Germany, April 24–28, 1989
Inbunden, Engelska, 1991
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Comets are always very impressive phenomena. Their appearances at regular, but mostly irregular, times excite people who see them. Astronomers have the obvious advantage of being able to see more of comets, and to study them. Their enthusiasm is reflected in the 50 papers in this book, written by more than 90 experts. The reviews in this book clearly describe a landmark in the history of cometary studies. Knowledge gathered up to and including Comet Halley are presented in two volumes. The first volume is about general aspects of observing and studying comets, where they originate and how their evolution develops. The second volume goes into the details of what a comet is: the nucleus, the coma, cometary dust, plasmas and magnetic fields. The book ends with a reflection by Fred Whipple about Comets in the Post-Halley Era. The book discusses all aspects of comets and is therefore suitable for use in graduate level courses. All astronomers and geophysicists interested in comets will find very useful and well-presented information in this book.
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Comets are always very impressive phenomena. Their appearances at regular, but mostly irregular, times excite people who see them. Astronomers have the obvious advantage of being able to see more of comets, and to study them. Their enthusiasm is reflected in the 50 papers in this book, written by more than 90 experts. The reviews in this book clearly describe a landmark in the history of cometary studies. Knowledge gathered up to and including Comet Halley are presented in two volumes. The first volume is about general aspects of observing and studying comets, where they originate and how their evolution develops. The second volume goes into the details of what a comet is: the nucleus, the coma, cometary dust, plasmas and magnetic fields. The book ends with a reflection by Fred Whipple about Comets in the Post-Halley Era. The book discusses all aspects of comets and is therefore suitable for use in graduate level courses. All astronomers and geophysicists interested in comets will find very useful and well-presented information in this book.
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Light scattering and absorption by small homogeneous particles can be worked-out exactly for spheres and infinite cylinders. Homogeneous particles of irregular shapes, when averaged with respect to rotation, have effects that can in general be well-approximated by reference to results for these two idealised cases. Likewise, small inhomogeneous particles have effects similar to homogeneous particles of the same average refractive index. Thus most problems can be solved to a satisfactory approximation by reference to the exact solutions for spheres and cylinders, which are fully stated here in the early part of the book. The sum of scattering and absorption, the extinction, is too large to be explained by inorganic materials, provided element abundances in the interstellar medium are not appreciably greater than solar, H 0 and NH3 being essentially excluded in the 2 general medium, otherwise very strong absorptions near 3p,m would be observed which they are not. A well-marked extinction maximum in the ultraviolet near 2200A has also not been explained satisfactorily by inorganic materials. Accurately formed graphite spheres with radii close to O.02p,m could conceivably provide an explanation of this ultraviolet feature but no convincing laboratory preparation of such spheres has ever been achieved.
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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 enveloped 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. This book provides an extensive coverage of the interstellar maser phenomenon. A precondition for maser action is departure from thermal equilibrium. The book therefore starts with a detailed coverage of the basic background concepts required for an understanding of line formation and radiative transfer. It goes on to describe the theoretical and phenomenological aspects of interstellar masers, their formation sites and the inversion mechanisms. The book should interest active researchers in astronomy and astrophysics as well as other areas of physics.It is designed to be suitable as a textbook in a graduate course and aims to enable a graduate student to embark on research projects in this area in particular, and molecular radio astronomy in general. Basic background concepts; astronomical maser radiation; maser theory; effects of geometry; polarization; pumping; the environments of astronomical masers; OH masers; H2O masers; SiO masers; other masers; extragalactic masers; masers as astronomical tools.
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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 enveloped 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. This book provides an extensive coverage of the interstellar maser phenomenon. A precondition for maser action is departure from thermal equilibrium. The book therefore starts with a detailed coverage of the basic background concepts required for an understanding of line formation and radiative transfer. It goes on to describe the theoretical and phenomenological aspects of interstellar masers, their formation sites and the inversion mechanisms. The book should interest active researchers in astronomy and astrophysics as well as other areas of physics.It is designed to be suitable as a textbook in a graduate course and aims to enable a graduate student to embark on research projects in this area in particular, and molecular radio astronomy in general.
854 kr
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Del 172 - Astrophysics and Space Science Library
Physical Processes in Solar Flares
Inbunden, Engelska, 1991
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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 1 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.
Del 173 - Astrophysics and Space Science Library
Origin and Evolution of Interplanetary Dust
Colloquium Proceedings
Inbunden, Engelska, 1992
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The origin and evolution of interplanetary dust have been extensively discussed ever since the 1960s when a series of meetings began which brought together the interplanetary dust community. More recently, during the 1980s, new knowledge has emerged from comprehensive studies of cometary flybys and from infrared space observations. At present new, in-situ explorations of interplanetary dust are providing some promising results. This work begins with investigations of interplanetary dust by space and Earth environment studies, by physics and chemical analysis, and by zodiacal light and optical studies. Topics related to cometary dust, meteoroids and meteor streams, and circumplanetary dust, which are indeed linked to the evolution of interplanetary dust, are then presented. Finally, the origin of interplanetary dust is tracked back to comets or asteroids and to interstellar or circumstellar dust. A summary demonstrates that interplanetary dust studies are thriving and may provide a clearer understadnign of the formation of the solar system.
Digitised Optical Sky Surveys
Proceedings of the Conference on "Digitised Optical Sky Surveys", Held in Edinburgh, Scotland, June 18-21, 1991
Inbunden, Engelska, 1992
854 kr
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Astronomical photographs contain an enormous amount of information. This presents extremely interesting problems when one wishes to produce digitized sky atlases, to archive the digitized material, to develop sophisticated devices to do the digitizing, and to create software to process the vast amounts of data. All these activities are necessary to be able to carry out astronomy work. One such activity is the important, large-scale optical identification of objects which also emit radiation at other wavelengths. Other activities of the past decade include a multiplicity of surveys that have been made on galaxies and clusters of galaxies. This book treats, in five sections, the existing and future surveys, their digitization and their impact on astronomy. It is designed to serve as a reference for people in the field and for those who wish to engage in using or producing sky surveys.
Del 175 - Astrophysics and Space Science Library
Astronomical Photometry
A Guide
Inbunden, Engelska, 1992
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Small and large telescopes are being installed around the world. Astronomers have thus acquired better access to more modern equipment; not in the least to photometers, which are important tools for the contemporary obsserver. This development of higher quality and more sensitive equipment makes it necessary to improve the accuracy of the measurements. This guide aims to help the astronomer and astronomy student to improve the quality of their photometric measurements and to extract a maximum of information from their observations. The book is based on the authors' observing experience, spending time behind various instruments at different observatories.
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The Andromeda galaxy, or M31, is an attractive galaxy for astronomers. It is close to us, it is of about the size of our galaxy, it provides some intriguing observational puzzles because the galaxy us nearly edge-on, and many objects can be studied in detail because they are still sufficiently bright. With the current developments in instrumentation with which increasingly detailed studies of the Andromeda galaxy can be made, this book provides a foundation for the start of new observations. The work is a source of information on M31, and can be used by both insiders and newcomers to the field.
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More than two centuries have elapsed since the story of interacting binary stars began with the rediscovery of the variability of Algol by John Goodricke and the interpretation he proposed for explaining the regular periodic brightness variations which he found. Over this long span of time our knowledge about these systems has been growing, and we have now reached a fairly good understanding of the structure and behaviour of this interesting group of objects. This book contains a timely summary of our present knowledge of interacting binary stars. The chapters have been written by distinguished scientists who have done relevant research in the field of interacting binary stars.
Del 178 - Astrophysics and Space Science Library
Morphological and Physical Classification of Galaxies
Proceedings of the Fifth International Workshop of the Osservatorio Astronomico di Capodimonte Held in Sant’Agata Sui Due Golfi, Italy, September 3–7, 1990
Inbunden, Engelska, 1992
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The morphological scheme devised by Hubble and followers to classify galaxies has, over many decades, proved to be quite effective in directing the quest for the fundamental parameters describing the extragalactic manifold. This statement, however, is far more true for spirals than for ellipticals. In the last few years efforts have been made to search for a more meaningful classification of ellipticals, at the same time the classical question of whether E galaxies form a physically homogenous family has been brushed up once more. This book pictures the transition process from the morphological to the physical "era' in the classification of galaxies.
Del 179 - Astrophysics and Space Science Library
Structure and Evolution of Single and Binary Stars
Inbunden, Engelska, 1992
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Classical stellar evolution theories have undergone some drastic changes in recent decades. New insights into the development of stellar interiors were obtained from studying stars in various stages of thei lives, as well as with the help of fast computers, which gave the boost to the branch of numerical modelling of stellar structure and evolution. This book is divided into two parts. The first part deals with the general aspects of stellar structure and evolution including information on numerical modelling. The second part deals with specific evolutionary aspects of single and binary stars with a variety of masses. The last chapter gives several models of stars with specific masses. The text is intended as an introduction to students as well as a reference to researchers.