Astrophysics II: Stellar Structure / Astrophysik II: Sternaufbau

  • Authors
  • Marshal H. Wrubel
  • H. C. Arp
  • G. R. Burbidge
  • E. Margaret Burbidge
  • Hans E. Suess
  • Harold C. Urey
  • Lawrence H. Aller
  • P. Ledoux
  • Th. Walraven
  • Armin J. Deutsch
  • E. Schatzman
  • Cecilia Payne-Gaposchkin
  • F. Zwicky

Part of the Encyclopedia of Physics / Handbuch der Physik book series (HDBPHYS, volume 11 / 51)

Table of contents

  1. Front Matter
    Pages II-VIII
  2. Marshal H. Wrubel
    Pages 1-74
  3. H. C. Arp
    Pages 75-133
  4. G. R. Burbidge, E. Margaret Burbidge
    Pages 134-295
  5. Hans E. Suess, Harold C. Urey
    Pages 296-323
  6. Lawrence H. Aller
    Pages 324-352
  7. P. Ledoux, Th. Walraven
    Pages 353-604
  8. P. Ledoux
    Pages 605-688
  9. Armin J. Deutsch
    Pages 689-722
  10. E. Schatzman
    Pages 723-751
  11. Cecilia Payne-Gaposchkin
    Pages 752-765
  12. F. Zwicky
    Pages 766-785
  13. Back Matter
    Pages 786-831

About this book

Introduction

Sects. 12, 13. 89 sequence and that subgiant and fainter stars in globular clusters have ultraviolet excesses. When dealing with stars whose physical properties are imperfectly under­ stood, such as in globular cluster stars, we cannot rely too heavily on the empiri­ cal calibration by the kinds of stars used to define Fig. 5, to determine their true, unreddened U-B, B-V curve. But if by a combination of arguments, principally the reddening in the region of the stars we do known about, we can assign a fairly probable unreddened U-B, B-V curve to a group of stars about which we know little, the argument may be turned around. In this case some information may be gained about the energy envelope of the stars by examining the differences between the normal two-color index curves for the unknown group of stars compared to the known. In general there seem to be two possible causes for different stars defining different normal sequences in the U-B, B-V plane. One, the relative energy distribution in the continuum in the U, B and V photometry bands are different. An example of this is the effect of the Balmer depression in supergiants. This, of course, requires deviation from black body radiation curves for one or both groups of stars. This cause seems to be the dominant effect for very blue, hot stars where the depression of the continuum by absorption lines is at a minimum.

Keywords

Astrophysik Libration Stern Sternaufbau Supernova astrophysics energy fields photometry planet radiation stability star stellar evolution sun

Bibliographic information

  • DOI https://doi.org/10.1007/978-3-642-45908-5
  • Copyright Information Springer-Verlag OHG. Berlin · Göttingen · Heidelberg 1958
  • Publisher Name Springer, Berlin, Heidelberg
  • eBook Packages Springer Book Archive
  • Print ISBN 978-3-642-45910-8
  • Online ISBN 978-3-642-45908-5
  • Series Print ISSN 0085-140X
  • About this book