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Shock-Wave Solutions of the Einstein Equations with Perfect Fluid Sources: Existence and Consistency by a Locally Inertial Glimm Scheme
Jeff Groah, California State University at Monterey Bay, Seaside, CA, and Blake Temple, University of California, Davis, CA
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Memoirs of the American Mathematical Society
2004; 84 pp; softcover
Volume: 172
ISBN-10: 0-8218-3553-X
ISBN-13: 978-0-8218-3553-1
List Price: US$57
Individual Members: US$34.20
Institutional Members: US$45.60
Order Code: MEMO/172/813
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We demonstrate the consistency of the Einstein equations at the level of shock-waves by proving the existence of shock wave solutions of the spherically symmetric Einstein equations for a perfect fluid, starting from initial density and velocity profiles that are only locally of bounded total variation. For these solutions, the components of the gravitational metric tensor are only Lipschitz continuous at shock waves, and so it follows that these solutions satisfy the Einstein equations, as well as the relativistic compressible Euler equations, only in the weak sense of the theory of distributions. The analysis introduces a locally inertial Glimm scheme that exploits the locally flat character of spacetime, and relies on special properties of the relativistic compressible Euler equations when \(p=\sigma^2\rho\), \(\sigma\equiv const\).

We demonstrate the consistency of the Einstein equations at the level of shock-waves by proving the existence of shock wave solutions of the spherically symmetric Einstein equations for a perfect fluid, starting from initial density and velocity profiles that are only locally of bounded total variation. For these solutions, the components of the gravitational metric tensor are only Lipschitz continuous at shock waves, and so it follows that these solutions satisfy the Einstein equations, as well as the relativistic compressible Euler equations, only in the weak sense of the theory of distributions. The analysis introduces a locally inertial Glimm scheme that exploits the locally flat character of spacetime, and relies on special properties of the relativistic compressible Euler equations when \(p=\sigma^2\rho\), \(\sigma\equiv const\).

Readership

Graduate students and research mathematicians interested in partial differential equations, relativity, and gravitational theory.

Table of Contents

  • Introduction
  • Preliminaries
  • The fractional step scheme
  • The Riemann problem step
  • The ODE step
  • Estimates for the ODE step
  • Analysis of the approximate solutions
  • The elimination of assumptions
  • Convergence
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