Physics of Thermal Gaseous Nebulae

Physical Processes in Gaseous Nebulae

  • Lawrence H. Aller

Part of the Astrophysics and Space Science Library book series (ASSL, volume 112)

Table of contents

  1. Front Matter
    Pages i-x
  2. Lawrence H. Aller
    Pages 1-17
  3. Lawrence H. Aller
    Pages 18-38
  4. Lawrence H. Aller
    Pages 115-152
  5. Lawrence H. Aller
    Pages 153-166
  6. Lawrence H. Aller
    Pages 167-186
  7. Lawrence H. Aller
    Pages 187-206
  8. Lawrence H. Aller
    Pages 207-221
  9. Lawrence H. Aller
    Pages 222-254
  10. Lawrence H. Aller
    Pages 255-290
  11. Back Matter
    Pages 315-350

About this book

Introduction

Gaseous nebulae offer outstanding opportunities to atomic physicists, spectroscopists, plasma experts, and to observers and theoreticians alike for the study of attenuated ionized gases. These nebulae are often dusty, heated by radiation fields and by shocks. They are short-lived phenomena on the scale of a stellar lifetime, but their chemical compositions and internal kinematics may give important clues to advanced stages of stellar evolution. The material herein presented is based on lectures given at the University of Michigan, University of Queensland, University of California, Los Angeles, and in more abbreviated form at the Raman Institute, at the Scuola Internazionale di Trieste, and elsewhere. Much of it is derived origionally from the series "Physical Processes in Gaseous Nebulae" initiated at the Harvard College Observatory in the late 1930s. I have tried to emphasize the basic physics of the mechanisms involved and mention some of the uncertainties that underlie calculations of many basic parameters. Emphasis is placed on ionized plasmas with electron temperatures typically in the neighborhood of 10,OOOoK. Dust and other ingredients of the cold component of the interstellar medium are treated briefly from the point of view of their relation to hot plasmas of H II regions and planetaries. Chemical composition determinations for nebulae are discussed in some detail while the last section deals with interpretations of elemental abundances in the framework of stellar evolution and nucleogenesis. Gaseous nebulae offer some particularly engaging opportunities for studies of stellar evolution.

Keywords

Supernova Variation galaxy hydrogen line interstellar matter nebula observatory planet stars stellar stellar evolution

Authors and affiliations

  • Lawrence H. Aller
    • 1
  1. 1.University of CaliforniaLos AngelesUSA

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-010-9639-3
  • Copyright Information Springer Science+Business Media B.V. 1984
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-90-277-2546-2
  • Online ISBN 978-94-010-9639-3
  • Series Print ISSN 0067-0057
  • About this book
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