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Conservation laws and the energy–momentum–stress pseudotensor; the cosmological principle and the structure of the universe at large, the Robertson–Walker metric and the Friedman universe(s), Hubble’s law, the expansion of the universe, and the cosmological constant.
This textbook describes the equipment, observational techniques, and analysis used in the investigation of stellar photospheres. Now in its fourth edition, the text has been thoroughly updated and revised to be more accessible to students. New figures have been added to illustrate key concepts, while diagrams have been redrawn and refreshed throughout. The book starts by developing the tools of analysis, and then demonstrates how they can be applied. Topics covered include radiation transfer, models of stellar photospheres, spectroscopic equipment, how to observe stellar spectra, and techniques for measuring stellar temperatures, radii, surface gravities, chemical composition, velocity fields, and rotation rates. Up-to-date results for real stars are included. Written for starting graduate students or advanced undergraduates, this textbook also includes a wealth of reference material useful to researchers. eBook formats include color imagery while print formats are greyscale only; a wide selection of the color images are available online.
Sidney Coleman (1937–2007) earned his doctorate at Caltech under Murray Gell-Mann. Before completing his thesis, he was hired by Harvard and remained there his entire career. A celebrated particle theorist, he is perhaps best known for his brilliant lectures, given at Harvard and in a series of summer school courses at Erice, Sicily. Three times in the 1960s he taught a graduate course on Special and General Relativity; this book is based on lecture notes taken by three of his students and compiled by the Editors.
Magnetic fields permeate space and affect many major astrophysical phenomena, but they are often ignored due to their perceived complexity. This self-contained introduction to astrophysical magnetic fields provides both a comprehensive review of the current state of the subject and a critical discussion of the latest research. It presents our knowledge of magnetic fields from the Early Universe, their evolution in cosmic time through to their roles in present-day galaxies, galaxy clusters and the wider intergalactic medium, with attention given to both theory and observations. This volume also contains an extensive introduction into magnetohydrodynamics, numerous worked examples, observational and mathematical techniques and interpretations of the observations. Its review of our current knowledge, with an emphasis on results that are likely to form the basis for future progress, benefits a broad audience of advanced students and active researchers, including those from fields such as cosmology and general relativity.
To use spectral lines for stellar analysis, we need to have some basic understanding of how and why they respond to variations in chemical abundances, temperature, and pressure.Here in Chapter 13 these issues are explored and we learn how to select spectral lines suitable for specific tasks.
In this chapter we bring together some of the techniques of observing and calculating stellar spectra with the aim of measuring the sizes and temperatures of stars.Results are summarized.
Surface gravity is one of the basic parameters of a star.The tools we have to measure a star's gravity are reviewed and examples of their application aregiven.A summary of gravity values is given.
Rotation of stars affects stellar spectra and stellar physics.Spectral lines are broadened and imprinted with the characteristic shape of the rotational velocity distribution, and there may be modulation from spots being carried across the visible hemisphere.Methods for extracting rotation rates from line profiles are discussed in detail.Results are summarized.Rotation circulates material inside stars, mixing chemicals and transporting angular momentum.And rotation couples with convection to generate magnetic fields.The magnetic fields produce many types of activity, including spots and flares and energy for coronae, and they hold on to escaping mass, acting as a magnetic brake on the rotation.We look into how rotation changes with time, with evolutionary stage, and for binaries with tidal interaction.