Balona luis (10 Ergebnisse)

Zustand: New. In English.

Couverture rigide. Zustand: bon. R260269814: 1994. In-8. Relié. Très bon état, Couv. convenable, Dos satisfaisant, Intérieur frais. 550 pages augmentées de quelques figures en noir et blanc dans texte. Avec Jaquette. . . Classification Dewey : 420-Langue anglaise. Anglo-saxon.

Gr.-8°, original hardcover. 1. ed. With numerous images, XVII, 413 p. Shelfmark on spine, stamp on Title, otherwise very fine copy. Sprache: Englisch Gewicht in Gramm: 0.

Zustand: New. In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together in order to broaden our understanding of O and B stars. Editor(s): Balona, Luis A.; Henrichs, Huib F.; Le Contel, Jean Michel. Series: International Astronomical Union Symposia (Closed). Num Pages: 550 pages, biography. BIC Classification: PGM. Category: (P) Professional & Vocational; (UP) Postgraduate, Research & Scholarly; (UU) Undergraduate. Dimension: 240 x 160 x 30. Weight in Grams: 1031. . 1994. Softcover reprint of the original 1st ed. 1994. Paperback. . . . . Books ship from the US and Ireland.…

Paperback. Zustand: Brand New. reprint edition. 572 pages. 9.40x6.20x1.30 inches. In Stock.

Zustand: New. In English.

Taschenbuch. Zustand: Neu. Druck auf Anfrage Neuware - Printed after ordering - In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together for the first time in order to broaden our understanding of O and B stars. Thanks to advances in digital spectroscopy, new types of pulsating B stars have been discovered. The pulsations can be understood in terms of the recent revision of metal opacities, but the effects of rapid rotation and magnetic fields need further study. Observations in the UV and X-ray regions demonstrate that many B and Be stars show other activity, besides pulsation which is not yet understood. The reason for the enhanced mass loss in Be stars is a question which dominates the Symposium and which remains unanswered, although it is surely to be found in activity at or near the photosphere coupled with rotation. It is shown that the geometry of the circumstellar envelopes around Be stars is indeed a flattened disk as they can now be optically resolved. The variability of radiatively-driven winds from O and B stars are likely related to the rotation of the star. This underlines the central theme of the book: that the various phenomena seen in these stars cannot be studied in isolation.…

Gebunden. Zustand: New. In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together for the first time in order to broaden our understanding of O and B stars. Thanks to advances in digital spectroscopy, new types of pu.

Hardcover. Zustand: Brand New. 576 pages. 9.75x6.75x1.25 inches. In Stock.

Buch. Zustand: Neu. Neuware - In this Symposium, researchers specializing in pulsation, rotation, magnetic fields and stellar winds are brought together for the first time in order to broaden our understanding of O and B stars. Thanks to advances in digital spectroscopy, new types of pulsating B stars have been discovered. The pulsations can be understood in terms of the recent revision of metal opacities, but the effects of rapid rotation and magnetic fields need further study. Observations in the UV and X-ray regions demonstrate that many B and Be stars show other activity, besides pulsation which is not yet understood. The reason for the enhanced mass loss in Be stars is a question which dominates the Symposium and which remains unanswered, although it is surely to be found in activity at or near the photosphere coupled with rotation. It is shown that the geometry of the circumstellar envelopes around Be stars is indeed a flattened disk as they can now be optically resolved. The variability of radiatively-driven winds from O and B stars are likely related to the rotation of the star. This underlines the central theme of the book: that the various phenomena seen in these stars cannot be studied in isolation.…