| 書目名稱 | Mass Loss from Red Giants |
| 副標題 | Proceedings of a Con |
| 編輯 | Mark Morris,Ben Zuckerman |
| 視頻video | http://file.papertrans.cn/626/625238/625238.mp4 |
| 叢書名稱 | Astrophysics and Space Science Library |
| 圖書封面 |  |
| 描述 | 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?". |
| 出版日期 | Conference proceedings 1985 |
| 關(guān)鍵詞 | LOPES; Variation; astronomy; gravity; interferometry; optical interferometry; photometry; planet; radio astr |
| 版次 | 1 |
| doi | https://doi.org/10.1007/978-94-009-5428-1 |
| isbn_softcover | 978-94-010-8896-1 |
| isbn_ebook | 978-94-009-5428-1Series ISSN 0067-0057 Series E-ISSN 2214-7985 |
| issn_series | 0067-0057 |
| copyright | D. Reidel Publishing Company, Dordrecht, Holland 1985 |
|Archiver|手機版|小黑屋|
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