Mass Loss from Red Giants - Proceedings of a Conference held at the University of California at Los Angeles, U.S.A., June 20-21, 1984 (Hardcover, 1985 ed.)

Red giant and supergiant stars have long been favorites of professional 6 and amateur astronomers. These enormous stars emit up to 10 times more energy than the Sun and, so, are easy to study. Some of them, specifically the pulsating long-period variables, significantly change their size, brightness, and color within about a year, a time scale of interest to a single human being. Some aspects of the study of red giant stars are similar to the study of pre-main-sequence stars. For example, optical astronomy gives us a tantalizing glimpse of star forming regions but to really investi gate young stars and protostars requires infrared and radio astronomy. The same is true of post-main-sequence stars that are losing mass. Optical astronomers can measure the atomic component of winds from red giant stars that are undergoing mass loss at modest rates 6 (M $ 10- M9/yr.). But to see dust grains and molecules properly, 5 especially in stars with truly large mass loss rates, ~ 10- M9/yr, one requires IR and radio astronomy. As this stage of copious mass loss only lasts for ~105 years one might be tempted to ask, "who cares?".

General

Imprint:	Kluwer Academic Publishers
Country of origin:	Netherlands
Series:	Astrophysics and Space Science Library, 117
Release date:	August 1985
First published:	1985
Editors:	Mark Morris • Arie J. Zuckerman
Dimensions:	297 x 210 x 20mm (L x W x T)
Format:	Hardcover
Pages:	320
Edition:	1985 ed.
ISBN-13:	978-90-277-2075-7
Categories:	Books > Science & Mathematics > Astronomy, space & time > Galaxies, clusters, intergalactic matter > General
LSN:	90-277-2075-4
Barcode:	9789027720757

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