Author: Walter F. Huebner Publisher: Springer Science & Business Media ISBN: 1461487978 Category : Science Languages : en Pages : 582
Book Description
This book covers all aspects of opacity and equations of state for gases, plasmas, and dust. The discussion emphasizes the continuous transformation of the equilibrium compositions of these phases as a function of temperature and density.
Author: Opacity Project Team Publisher: CRC Press ISBN: 9780750301749 Category : Science Languages : en Pages : 456
Book Description
Opacity is a quantity that determines the transport of radiation through matter and is important in many problems in physics and astrophysics. To calculate opacities, one requires atomic data for a large number of processes involving the absorption and scattering of radiation. Stellar opacities are of particular interest in astrophysics because of their importance for theories of stellar structure and stellar pulsations. Taking advantage of advances in computational atomic and plasma physics and of the availability of powerful supercomputers, The Opacity Project, Volume 2: Selected Research Papers-Atomic Data Tables for S to Fe presents accurate atomic data required for opacity calculations. The work includes computation of energy levels, oscillator strengths, photoionization cross sections, and parameters for pressure broadening of spectral lines. The book uses several different methods of computation to calculate the same data, thereby providing a check on the validity of the data. Divided into two parts, the first presents seven key research papers that review available data and detail the relevant atomic data calculations while the second part provides tables of energy levels and oscillator strengths for the elements S, Ar, Ca and Fe. The Opacity Project Team is comprised of 30 experts from 13 leading international laboratories and observatories in atomic physics and astrophysics.
Author: Publisher: ISBN: Category : Languages : en Pages :
Book Description
We turn to the effects on opacities of atomic lines and molecular bands. It was the realization that these atomic lines were important for the opacity and the radiation flow in stars that allowed the field of stellar evolution to greatly flower in the 1960's and 1970's. Our understanding of stellar structure and evolution is now very deep.
Author: Maurizio Salaris Publisher: John Wiley & Sons ISBN: 9780470092224 Category : Science Languages : en Pages : 386
Book Description
Evolution of Stars and Stellar Populations is a comprehensive presentation of the theory of stellar evolution and its application to the study of stellar populations in galaxies. Taking a unique approach to the subject, this self-contained text introduces first the theory of stellar evolution in a clear and accessible manner, with particular emphasis placed on explaining the evolution with time of observable stellar properties, such as luminosities and surface chemical abundances. This is followed by a detailed presentation and discussion of a broad range of related techniques, that are widely applied by researchers in the field to investigate the formation and evolution of galaxies. This book will be invaluable for undergraduates and graduate students in astronomy and astrophysics, and will also be of interest to researchers working in the field of Galactic, extragalactic astronomy and cosmology. comprehensive presentation of stellar evolution theory introduces the concept of stellar population and describes "stellar population synthesis" methods to study ages and star formation histories of star clusters and galaxies presents stellar evolution as a tool for investigating the evolution of galaxies and of the universe in general
Author: Carl J. Hansen Publisher: Springer Science & Business Media ISBN: 9780387200897 Category : Science Languages : en Pages : 554
Book Description
The?rsteditionofthistextappearedin1994.Shortlyafterthethirdprinting, our editor suggested that we attempt a second edition because new devel- mentsinstellarstructureandevolutionhadmadeouroriginalworkoutdated. We (the original authors, CJH and SDK) reluctantly agreed but with res- vations due to the e?ort involved. Our initial reluctance disappeared when we were able to convince (cajole, twist the arm of, etc.) our new coauth- colleague Virginia Trimble to join us. (Welcome Virginia!) We (i.e., all three of us) hope that you agree that the present edition is a great improvement compared to the 1994 e?ort. Our objectives in this edition are the same ones we set forth in 1994: Whatyouwill?ndisatextdesignedforourtargetaudience:thety- cal senior undergraduate or beginning graduate student in astronomy or astrophysics who wishes an overview of stellar structure and e- lution with just enough detail to understand the general picture. She or he can go on from there to more specialized texts or directly to the research literature depending on talent and interests. To this end, this text presents the basic physical principles without chasing all the (interesting!) details. For those of you familiar with the ?rst edition, you will ?nd that some things have not been changed substantially (F = ma is still F = ma), while othersde?nitelyhave.Forexample,Chapter2hasbeencompletelyrewritten.
Author: Jordi Jose Publisher: CRC Press ISBN: 1439853088 Category : Science Languages : en Pages : 467
Book Description
Stars are the main factories of element production in the universe through a suite of complex and intertwined physical processes. Such stellar alchemy is driven by multiple nuclear interactions that through eons have transformed the pristine, metal-poor ashes leftover by the Big Bang into a cosmos with 100 distinct chemical species. The products of
Author: Martin Harwit Publisher: Springer Science & Business Media ISBN: 147572019X Category : Science Languages : en Pages : 642
Book Description
My principal aim in writing this book was to present a wide range of astrophysical topics in sufficient depth to give the reader a general quantitative understanding of the subject. The book outlines cosmic events but does not portray them in detail-it provides aseries of astrophysical sketches. I think this approach befits the present uncertainties and changing views in astrophysics. The material is based on notes I prepared for a course aimed at seniors and beginning graduate students in physics and astronomy at Cornell. This course defined the level at which the book is written. For readers who are versed in physics but are unfamiliar with astronomical terminology, Appendix A is included. It gives a brief background of astronomical concepts and should be read before starting the main text. The first few chapters outline the scope of modern astrophysics and deal with elementary problems concerning the size and mass of cosmic objects. However, it soon becomes apparent that a broad foundation in physics is needed to proceed. This base is developed in Chapters 4 to 7 by using, as ex am pIes, specific astronomi cal situations. Chapters 8 to 10 enlarge on the topics first outlined in Chapter I and show how we can obtain quantitative insights into the structure and evolution of stars, the dynamics of co~mic gases, and the large-scale behavior of the universe.
Author: Opacity Project Team Publisher: CRC Press ISBN: 9780750302883 Category : Science Languages : en Pages : 834
Book Description
Opacity is a quantity which determines the transport of radiation through matter, and is important in many problems in physics and astronomy. To calculate opacities one requires atomic data for a large number of processes involving the absorption and scattering of radiation. Stellar opacities are of particular interest in astrophysics because of their importance for theories of stellar structure and stellar pulsations. Taking advantage of advances in computational atomic and plasma physics and of the availability of powerful supercomputers, a collaborative effort - the international Opacity Project - has been made to compute accurate atomic data required for opacity calculations. The work includes computation of energy levels, oscillator strengths, photoionisation cross sections and parameters for pressure broadening of spectral lines. Several different methods of computation have been used to calculate the same data thereby providing a check on the validity of the data. The Opacity Project Team is made up of 30 experts drawn from 13 leading laboratories and observatories in atomic physics and astrophysics in the USA, Europe and South America. The Project has been running since 1986. ^IThe Opacity Project Volume 1 is the first of a two-volume reference work produced by the international Opacity Project. It is divided into two parts: * Reprints of 31 key research papers elaborating the theoretical physical basis and computational methods used to produce the data. These papers provide essential background for researchers to understand how the data are produced. * Tables of energy levels and oscillator strengths for atoms and ions of the elements He to Si. Volume 2 contains tables of energy levels and oscillator strengths for the elements P to Fe. The amount of data will be similar to that of Volume 1.
Author: D. Vanbeveren Publisher: Springer Science & Business Media ISBN: 9781402003769 Category : Science Languages : en Pages : 360
Book Description
The evolution of galaxies is governed mainly by the evolution of massive stars whereas the evolution of a massive star depends primarily on its mass, chemical composition and on whether or not the star is a Single object or a binary component. To study the evolution of galaxies, it is therefore essential to know how stellar masses are distributed at birth, how many stars are formed in binaries, and what the mass ratio and orbital period distribution of binaries look like. Massive stars are intrinsically the brightest stars, so that it may be possible to discover their properties in distant groups prOvided that large telescopes can be used for basic stellar observations. However, until now the observations of massive stars have been reasonably complete only for a small region of our own Galaxy (~ 3 kpc from the Sun). One hopes that the conclusions resulting from these observations hold for the whole Galaxy, for the whole cosmos. With 'The Brightest Stars' of De Jager (1980) in mind, the present monograph is an addendum and an update in which we discuss the observations of 'The Brightest Binaries' in the framework of stellar evolution. A small or intermediate mass star close to the Sun may look brighter than a massive one far away. However, within volume limited star samples, the massive stars are on average also the brightest ones. In the present monograph (similarly as in the work of De Jager), bright means massive. The book consists of four main chapters.
Author: Walter F. Huebner
Author: Opacity Project Team
Author: 
Author: Su-Shu Huang
Author: Maurizio Salaris
Author: Carl J. Hansen
Author: Jordi Jose
Author: Martin Harwit
Author: Opacity Project Team
Author: D. Vanbeveren