ISBN: 9780792330448

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 an… Plus…

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. Pulsation, Rotation and Mass Loss in Early-Type Stars International Astronomical Union / Balona, Luis A. / Henrichs, Huib F., Kluwer Academic Publishers<

ISBN: 9780792330448

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 an… Plus…

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. Media > Book, [PU: Kluwer Academic Publishers]<

1993, ISBN: 9780792330448

Kluwer, 1994. *Price HAS BEEN REDUCED by 10% until Monday, April 24 (sale item)* xxii, 550 pp., Hardcover, lacks the dust jacket, ex library else text clean and binding tight. - If you… Plus…

Kluwer, 1994. *Price HAS BEEN REDUCED by 10% until Monday, April 24 (sale item)* xxii, 550 pp., Hardcover, lacks the dust jacket, ex library else text clean and binding tight. - If you are reading this, this item is actually (physically) in our stock and ready for shipment once ordered. We are not bookjackers. Buyer is responsible for any additional duties, taxes, or fees required by recipient's country., Kluwer, 1994, 0<

1994, ISBN: 9780792330448

Hardcover book. 572 pages. Published by Kluwer Academic Publishers (1994) Media > Book, [PU: Kluwer Academic Publishers]