Physics of Formation of FeII Lines Outside LTE

Proceedings of the 94th Colloquium of the International Astronomical Union Held in Anacapri, Capri Island, Italy, 4–8 July 1986

  • Roberto Viotti
  • Alberto Vittone
  • Michael Friedjung

Part of the Astrophysics and Space Science Library book series (ASSL, volume 138)

Table of contents

  1. Front Matter
    Pages i-xiii
  2. General Introduction to the “Fe II Problem”

  3. FeII Reference Catalogue

    1. G. B. Baratta, R. Viotti
      Pages 9-10
  4. Basic Atomic Data

    1. Front Matter
      Pages 11-11
    2. Bodo Baschek, Sveneric Johansson
      Pages 35-39
    3. T. Brage, A. E. Nilsson, S. Johansson, B. Baschek, J. Adams
      Pages 63-65
    4. U. Pauls, N. Grevesse, M. C. E. Huber
      Pages 79-82
    5. Robert J. Rutten, Roman I. Kostik
      Pages 83-92
  5. Observation of FeII Lines in Different Astrophysical Objects

    1. Front Matter
      Pages 93-93
    2. R. Viotti, M. Friedjung
      Pages 107-113
    3. A. Cassatella, R. Gonzalez Riestra
      Pages 115-124
    4. F.-J. Zickgraf
      Pages 125-133
    5. A. Talavera
      Pages 135-142
    6. E. Covino, L. Terranegra, A. Vittone, F. Giovannelli, C. Rossi
      Pages 143-148

About these proceedings

Introduction

The same kind of physics is frequently common to very different fields of Astrophysics, so experts in each of these fields have often much to learn from each others. It was therefore logical that the International Astronomical Union should sponsor a colloquium about an ion which pro­ duces many spectral lines that can be used as a diagnostic for many sorts of objects, and which may sometimes have a major influence on physical processes occurring in astro­ physical sources. The lines of singly ionized iron (FeII) are present in absorption and emission in the spectra of objects such as the Sun, cool stars, circumstellar envelopes of hot stars, novae, diffuse nebulae including the supernova remnants, and active galactic nuclei. These lines are very often formed far from LTE, and their interpretation is not easy in view of the complex Grotrian diagram for FeII, and the gaps in the knowledge of various physical parameters. In addition, the density of very strong FeII lines becomes very large in the ultraviolet, and the lines can play a major role in the line blanketing. They need therefore to be taken into account in any energy balance argument.

Keywords

LOPES Supernova active galactic nuclei astrophysics quasar solar physics star stars sun telescope

Editors and affiliations

  • Roberto Viotti
    • 1
  • Alberto Vittone
    • 2
  • Michael Friedjung
    • 3
  1. 1.Istituto di Astrofisica Spaziale (CNR)FrascatiItaly
  2. 2.Osservatorio Astronomico di CapodimonteNapoliItaly
  3. 3.Institut d’Astrophysique (CNRS)ParisFrance

Bibliographic information

  • DOI https://doi.org/10.1007/978-94-009-4023-9
  • Copyright Information Springer Science+Business Media B.V. 1988
  • Publisher Name Springer, Dordrecht
  • eBook Packages Springer Book Archive
  • Print ISBN 978-94-010-8285-3
  • Online ISBN 978-94-009-4023-9
  • Series Print ISSN 0067-0057
  • About this book
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