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Resonance bands and binary-star formation.

Norman R Lebovitz1

  • 1Mathematics Department, University of Chicago, 5734 S. University Avenue, Chicago, Illinois 60637, USA. norman@math.uchicago.edu

Annals of the New York Academy of Sciences
|June 28, 2005
PubMed
Summary

Numerical simulations of self-gravitating masses suggest instability, potentially leading to binary star formation. Idealized models reveal resonance bands as key to understanding stellar evolution and instability.

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Area of Science:

  • Astrophysics
  • Computational physics
  • Stellar dynamics

Background:

  • Self-gravitating masses are fundamental in astrophysics.
  • Previous studies used idealized models (uniform-density ellipsoids) to approximate realistic stratified figures.
  • Numerical computations have explored the evolution of stratified, asymmetric, self-gravitating masses.

Purpose of the Study:

  • To isolate qualitative features common to both idealized and realistic self-gravitating figures.
  • To guide numerical computations and interpret their outcomes.
  • To identify instabilities relevant to binary star formation.

Main Methods:

  • Numerical computations of realistically stratified, asymmetric, self-gravitating masses.
  • Analysis of the evolution and stability of idealized uniform-density ellipsoids.
  • Reconsideration of idealized theory to find common qualitative features.

Main Results:

  • Instability onset was observed in numerical computations of realistic masses, hinting at binary star formation.
  • Idealized models accurately predicted some behaviors of realistic figures.
  • The study identified resonance bands of instability in evolutionary trajectories as a significant feature.

Conclusions:

  • Resonance bands represent a crucial factor in the instability of self-gravitating masses.
  • Idealized models, when analyzed for common features, can effectively guide and interpret complex numerical simulations.
  • Further investigation into resonance bands is warranted for a comprehensive understanding of binary star formation.

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