L a willson (21 Ergebnisse)

Zustand: Poor. This is an ex-library book and may have the usual library/used-book markings inside.This book has hardback covers. Book contains pencil markings. In poor condition, suitable as a reading copy. Re-bound by library. Please note the Image in this listing is a stock photo and may not match the covers of the actual item,500grams, ISBN.…

Hardcover. Zustand: Very Good. Zustand des Schutzumschlags: Good. 1st Edition. *Veteran-Owned, Family-Run, Small Book Store in the Pacific Northwest* FAST SHIPPING!! Clean text, no markings, tight binding. 292 pp.

Zustand: Good. Volume 99. This is an ex-library book and may have the usual library/used-book markings inside.This book has hardback covers. Clean from markings. In good all round condition. No dust jacket. Please note the Image in this listing is a stock photo and may not match the covers of the actual item,500grams, ISBN:0826407404.…

Hardcover. Zustand: Fine. Zustand des Schutzumschlags: Very Good. 1st Edition. *Veteran-Owned, Family-Run, Small Book Store in the Pacific Northwest* FAST SHIPPING!! Clean text, no markings, tight binding. 292 pp.

Gr.-8°, original hardcover. 1. ed. Numerous fig.,XII, 365 p. Shelfmark on spine, stamp on title, otherwise very fine copy. Sprache: Englisch Gewicht in Gramm: 0.

Zustand: NEW.

Gr.-8°, original hardcover. 1. ed. XII, 336 p. Stamp on preliminary page and title, otherwise very fine copy. Sprache: Englisch Gewicht in Gramm: 0.

Zustand: Good. Former library copy. Pages intact with minimal writing/highlighting. The binding may be loose and creased. Dust jackets/supplements are not included. Includes library markings. Stock photo provided. Product includes identifying sticker. Better World Books: Buy Books. Do Good.

Zustand: New. In.

Zustand: New. In.

Zustand: New. In.

Zustand: New. In.

Paperback. Zustand: Brand New. 352 pages. 9.25x6.10x0.80 inches. In Stock.

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Stellar mass loss is an essential part of the cycling of material from the interstellar medium into stars and back, and must be understood if we are to model processes on galactic to cosmological scales. The study of stellar winds and the effects of stellar mass loss has reached a particularly exciting stage where observational capabilities are increasingly able to provide interesting constraints on models and theories. Recent resu1ts from theoretical and observational work for both hot and cool stars with substantial winds have led to the suggestion that a combination of pulsation with other mechanisms makes for particularly efficient mass loss from stars. This provided the original motivation for the organization of this workshop. The conference was organized along relatively conventional lines according to the types of objects being scrutinized. However the true unity of the proceedings comes from the interplay of the mechanisms involved. For example, for the cool, luminous Mira variables, pulsation leads to shock waves that extend the atmosphere, enhancing dust formation; radiation pressure on dust drives the wind, cooling the atmosphere and in some cases suppressing the shocks. Similarly for the Be stars, both pulsation (in this case, non-radial) and radiation pressure (due to UV resonance lines) are expected to be important, and this expectation is at least qualitatively borne out by the observations.…

Zustand: New. Proceedings of the NATO Advanced Research Workshop, Ames, Iowa, U.S.A., October 23-27, 1989 Fundamental unsolved problems of stellar astrophysics include the effects of angular momentum on stellar structure and evolution, the nature and efficiency of t.

Paperback. Zustand: Brand New. 384 pages. 9.25x6.10x0.87 inches. In Stock.

Zustand: New. Proceedings of the NATO Advanced Research Workshop, Ames, Iowa, U.S.A., October 23-27, 1989 Editor(s): Willson, L. A.; Stalio, R. Series: NATO Science Series C. Num Pages: 365 pages, biography. BIC Classification: PGM; PHVB. Category: (P) Professional & Vocational; (UP) Postgraduate, Research & Scholarly. Dimension: 243 x 167 x 26. Weight in Grams: 678. . 1990. Hardback. . . . . Books ship from the US and Ireland. …

Taschenbuch. Zustand: Neu. Neuware - Fundamental unsolved problems of stellar astrophysics include the effects of angular momentum on stellar structure and evolution, the nature and efficiency of the processes by which angular momentum is redistributed within and lost from stars, and the role that stellar rotation plays in enhancing or driving stellar mass loss. There appears to be a qualitative change in the nature and efficiency of these mechanisms near spectral type FO: hotter (more massive) stars typically retain more angular momentum at least until they reach the main sequence, while cooler stars typically spin down quickly. For the hotter stars, recent work suggests a strong link between the type of pulsation behavior, the mass loss rates, and the rotation velocity. If the same mechanisms are able to drive mass loss from the main sequence A stars, as has recently been proposed, then the current interpretations of a number of observations will be drastically affected: e. g. the ages of clusters may be incorrect by up to a factor of two, and the surface abundances of isotopes of He, Li and Be may no longer give constraints on cosmological nucleosynthesis. There are also effects on the evolution of the abundances of elements in the interstellar medium and on the general evolution of populations of stars. Thus the questions of the mechanisms of angular momentum and mass loss of stars more massive than the sun is important not only for stellar studies but for the foundations of much of modern astrophysics.…

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Fundamental unsolved problems of stellar astrophysics include the effects of angular momentum on stellar structure and evolution, the nature and efficiency of the processes by which angular momentum is redistributed within and lost from stars, and the role that stellar rotation plays in enhancing or driving stellar mass loss. There appears to be a qualitative change in the nature and efficiency of these mechanisms near spectral type FO: hotter (more massive) stars typically retain more angular momentum at least until they reach the main sequence, while cooler stars typically spin down quickly. For the hotter stars, recent work suggests a strong link between the type of pulsation behavior, the mass loss rates, and the rotation velocity. If the same mechanisms are able to drive mass loss from the main sequence A stars, as has recently been proposed, then the current interpretations of a number of observations will be drastically affected: e. g. the ages of clusters may be incorrect by up to a factor of two, and the surface abundances of isotopes of He, Li and Be may no longer give constraints on cosmological nucleosynthesis. There are also effects on the evolution of the abundances of elements in the interstellar medium and on the general evolution of populations of stars. Thus the questions of the mechanisms of angular momentum and mass loss of stars more massive than the sun is important not only for stellar studies but for the foundations of much of modern astrophysics.…

Buch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - Stellar mass loss is an essential part of the cycling of material from the interstellar medium into stars and back, and must be understood if we are to model processes on galactic to cosmological scales. The study of stellar winds and the effects of stellar mass loss has reached a particularly exciting stage where observational capabilities are increasingly able to provide interesting constraints on models and theories. Recent resu1ts from theoretical and observational work for both hot and cool stars with substantial winds have led to the suggestion that a combination of pulsation with other mechanisms makes for particularly efficient mass loss from stars. This provided the original motivation for the organization of this workshop. The conference was organized along relatively conventional lines according to the types of objects being scrutinized. However the true unity of the proceedings comes from the interplay of the mechanisms involved. For example, for the cool, luminous Mira variables, pulsation leads to shock waves that extend the atmosphere, enhancing dust formation; radiation pressure on dust drives the wind, cooling the atmosphere and in some cases suppressing the shocks. Similarly for the Be stars, both pulsation (in this case, non-radial) and radiation pressure (due to UV resonance lines) are expected to be important, and this expectation is at least qualitatively borne out by the observations.…

Hardcover. viii, [2], 28, [4], 26, [4], 28pp, 75 pls, 2 folding genealogies. Original blind-stamped cloth, sps gilt-lettered, t.e.g; sl worn; ex-lib, stamps removed from titles, front free e-ps stuck down (2 torn, exposing library labels). First publ in parts 1830-38.