© 1993

Light Curve Modeling of Eclipsing Binary Stars

  • E. F. Milone
Conference proceedings

Table of contents

  1. Front Matter
    Pages i-vi
  2. Dirk Terrell, R. E. Wilson
    Pages 27-37
  3. J. Mukherjee, G. J. Peters, R. E. Wilson
    Pages 69-74
  4. Robert L. Kurucz
    Pages 93-101
  5. Albert P. Linnell
    Pages 103-111
  6. Paul B. Etzel
    Pages 113-124
  7. Graham Hill, Slavek Rucinski
    Pages 135-150
  8. D. S. Zhai, R. X. Zhang, X. B. Zhang
    Pages 175-180
  9. Timothy Banks
    Pages 181-185

About these proceedings


In the two decades since the development of the first eclipsing-binary modeling code, new analytic techniques and the availability of powerful, sometimes dedicated computing facilities have made possible vastly improved determinations of fundamental and even transient stellar parameters. The scale of these developments, of course, raises questions about modeling tools, techniques, and philosophies, such as: Who will maintain and upgrade the codes? Will the codes be open to improvement by outsiders, and if so, how? And, indeed, what should be the goals of a modeling program? Such questions had not been aired for a long time and, for this reason alone, deserved to be discussed in as general a forum as the community provides. This volume contains material presented by Commission 42 (Close Binary Stars) during the International Astronomical Union's XXI General Assembly in Argentina, July 1991, and during IAU Colloquium 151, Cordoba, Argentina, August 1991. The techniques discussed include simulations of stellar bright and dark spots, streams, partial and complete stellar disks, prominences, and other features characterizing active stars; modeling of polarization parameters; models that use radial velocities as well as line profile simulations to model velocity field variation across stellar disks; the weighted effects of brightness asymmetries; and models for translucent eclipsing agents such as stellar winds.


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Editors and affiliations

  • E. F. Milone
    • 1
  1. 1.Department of Physics and AstronomyUniversity of CalgaryCalgaryCanada

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