The Spectra of the Heavy Elements


Book Description

This paper lists the most prominent spectrum lines of the elements from protactinium to americium. In most cases, the spectra were made available because of the necessity of conducting spectrochemical analyses on a number of samples for impurities. Because of limitations of sample size, it was not feasible to perform the analyses with the aid of chemical or physical separations, and so the spectrum of the major constituent was always present. It would be of considerable interest to provide descriptions of the spectra which would be adequate for term analyses leading to energy levels and electron configurations, not only for the spectroscopic interest but also for the assistance they might provide in the correlation of chemical properties of these elements. However, the amounts of labor and sample required for such descriptions are quite formidable, as is evidenced by the fact that the spectra of thorium and uranium are still incompletely analyzed in spite of their having been available in unlimited quantities for many years. To be adequate for a term analysis, the wavelengths must be measured to the third decimal place for as many lines as can be observed over the most extensive wavelength range accessible; Zeeman patterns must be provided; and a temperature or excitation variation must be provided in order to distinguish the various stages of ionization and low levels from high levels. On the other hand, for purposes of identification, it is sufficient to have measurements of the strongest lines of each element, accurate to the first decimal place, covering a representative wavelength region that is convenient for analysis. Since it will probably be some time before data of much value for term analyses are accumulated, the following information was collected for whatever usefulness it might have in spectrochemical analyses.




Stellar Interiors


Book Description

That trees should have been cut down to provide paper for this book was an ecological afIront. From a book review. - Anthony Blond (in the Spectator, 1983) The first modern text on our subject, Structure and Evolution of the Stars, was published over thirty years ago. In it, Martin Schwarzschild described numerical experiments that successfully reproduced most of the observed properties of the majority of stars seen in the sky. He also set the standard for a lucid description of the physics of stellar interiors. Ten years later, in 1968, John P. Cox's tw~volume monograph Principles of Stellar Structure appeared, as did the more specialized text Principles of Stellar Evolution and Nuc1eosynthesis by Donald D. Clayton-and what a difference ten years had made. The field had matured into the basic form that it remains today. The past twenty-plus years have seen this branch of astrophysics flourish and develop into a fundamental pillar of modern astrophysics that addresses an enormous variety of phenomena. In view of this it might seem foolish to offer another text of finite length and expect it to cover any more than a fraction of what should be discussed to make it a thorough and self-contained reference. Well, it doesn't. Our specific aim is to introduce only the fundamentals of stellar astrophysics. You will find little reference here to black holes, millisecond pulsars, and other "sexy" objects.




Nuclei in the Cosmos


Book Description

Nuclear astrophysics as it stands today is a fascinating science. Even though, compared to other scientific fields, it is a young discipline which has developed only in this century, it has answered many questions concerning the under standing of our cosmos. One of these great achievements was the concept of nucleosynthesis, the creation of the elements in the early universe in interstellar matter and in stars. Nuclear astrophysics has continued, to solve many riddles of the evolution of the myriads of stars in our cosmos. This review volume attempts to provide an overview of the current status of nuclear astrophysics. Special emphasis is given to the interdisciplinary nature of the field: astronomy, nuclear physics, astrophysics and particle physics are equally involved. One basic effort of nuclear astrophysics is the collection of ob servational facts with astronomical methods. Laboratory studies of the nuclear processes involved in various astrophysical scenarios have provided fundamen tal information serving both as input for and test of astrophysical models. The theoretical understanding of nuclear reaction mechanisms is necessary, for example, to extrapolate the experimentally determined reaction rates to the thermonuclear energy range, which is relevant for the nuclear processes in our cosmos. Astrophysical models and calculations allow us to simulate how nuclear processes contribute to driving the evolution of stars, interstellar matter and the whole universe. Finally, elementary particle physics also plays an important role in the field of nuclear astrophysics, for instance through weak interaction processes involving neutrinos.




Observational Astrophysics


Book Description

For the last twenty years astronomy has been developing dramatically. Until the nineteen-fifties, telescopes, spectrometers, and photographic plates consti tuted a relatively simple set of tools which had been refined to a high degree of perfection by the joint efforts of physicists and astronomers. Indeed these tools helped at the birth of modern astrophysics: the discovery of the expan sion of the Universe. Then came radioastronomy and the advent of electronics; the last thirty years have seen the application to astrophysics of a wealth of new experimental techniques, based on the most advanced fields of physics, and a constant interchange of ideas between physicists and astronomers. Last, but not least, modern computers have sharply reduced the burden of dealing with the information painfully extracted from the skies, whether from ever scarce photons, or from the gigantic data flows provided by satellites and large telescopes. The aim of this book is not to give an extensive overview of all the tech niques currently in use in astronomy, nor to provide detailed instructions for preparing or carrying out an astronomical project. Its purpose is methodologi cal: photons are still the main carriers of information between celestial sources and the observer. How we are to collect, sample, measure, and store this infor mation is the unifying theme of the book. Rather than the diversity of tech niques appropriate for each wavelength range, we emphasize the physical and mathematical bases which are common to all wavelength regimes.




Los Alamos Science


Book Description




Heavy Metals


Book Description

Fundamental societal changes resulted from the necessity of people to get organized in mining, transporting, processing, and circulating the heavy metals and their follow-up products, which in consequence resulted in a differentiation of society into diversified professions and even societal strata. Heavy metals are highly demanded technological materials, which drive welfare and progress of the human society, and often play essential metabolic roles. However, their eminent toxicity challenges the field of chemistry, physics, engineering, cleaner production, electronics, metabolomics, botany, biotechnology, and microbiology in an interdisciplinary and cross-sectorial manner. Today, all these scientific disciplines are called to dedicate their efforts in a synergistic way to avoid exposure of heavy metals into the eco- and biosphere, to reliably monitor and quantify heavy metal contamination, and to foster the development of novel strategies to remediate damage caused by heavy metals.




The Analysis of Starlight


Book Description

This book presents a detailed pedagogical account of the equation of state and its applications in several important and fast growing topics in theoretical physics, chemistry and engineering. This book is the storv of the analysis of starlight by astronomical spectroscopy. It describes the development of the subject from the time of Joseph Fraunhofer, who, in 1814, used a telescope-mounted prism to observe the spectral light emitted from several bright stars. He discovered that light was missing at certain colours (wavelengths) in the starlight, and these so-called spectral lines were subsequently shown to hold clues to the nature of the stars themselves. The book explains how the classification of stars using their line spectra developed into a major branch of astronomy whilst new methods in astrophysics made possible the approximate quantitative analysis of spectral lines in the 1920s and 1930s. After the Second World War these techniques were considerably improved when computers were programmed to model the structure of the outer layers of stars. Basic concepts in spectroscopy and spectral analysis are also covered and. finally. Dr Hearnshaw comments on the stellar spectroscopy of some individual star.







Supernovae - Proceedings Of The 6th Jerusalem Winter School For Theoretical Physics


Book Description

Supernovae are highly energetic phenomena for which it is necessary to use simultaneously particle physics, nuclear physics and hydrodynamics to study the creation of the strong explosions involved. Supernovae synthesize heavy elements and in some cases lead to the formation of neutron stars or black holes. Recent progress has revealed new classes of explosions, and new insights into the evolution and explosion mechanisms including that of the dramatic event SN 1987A in the Large Magellanic Cloud. Major questions still remain, concerning the evolution of massive stars in binary systems, the nature of gravitational collapse, and the physical processes involved in the thermonuclear explosion of degenerate stars. This School explores our current understanding of supernovae, and areas of active study.




Progress in Physics, vol. 1/2007


Book Description

Progress in Physics has been created for publications on advanced studies in theoretical and experimental physics, including related themes from mathematics.