Skip to main content Accessibility help

We use cookies to distinguish you from other users and to provide you with a better experience on our websites. Close this message to accept cookies or find out how to manage your cookie settings.

Close cookie message
×
  1. Home
  2. Search

Refine search

Refine search

Access:
Content type:
Publication date:
Apply   From and To filters
Subject: Show more
Journals Show more
Publishers: Show more
Societies Show more
Series: Show more
Collections: Show more

Actions for selected content:

Select all | Deselect all
  • View selected items
  • Export citations
  • Download PDF (zip)
  • Save to Kindle
  • Save to Dropbox
  • Save to Google Drive

Save Search

You can save your searches here and later view and run them again in "My saved searches".

Please provide a title, maximum of 40 characters.
Cancel
×

3 results

  • Chapter 9 - The Geometry Outside a Spherical Star

  • from Part II - The Curved Spacetimes of General Relativity
  • James B. Hartle, University of California, Santa Barbara
  • Book:
    Gravity
    Published online:
    03 September 2021
    Print publication:
    24 June 2021, pp 186-218

  • Summary

    The simplest curved spacetimes of general relativity are the ones with the most symmetry, and the most useful of these is the geometry of empty space outside a spherically symmetric source of curvature – for example, a spherical star. This is called the Schwarzschild geometry. To an excellent approximation, this is the curved spacetime outside the Sun and therefore leads to the predictions of Einstein’s theory most accessible to experimental test. In this chapter, we explore the geometry of Schwarzschild’s solution, assuming it’s given. We will concentrate on predicting the orbits of test particles and light rays in the curved spacetime of a spherical star that exhibit some of the famous effects of general relativity – the gravitational redshift, the precession of the perihelion of a planet, the gravitational bending of light, and the time delay of light.

  • 6 - Equations of Motion in the PPN Formalism

  • Clifford M. Will, University of Florida
  • Book:
    Theory and Experiment in Gravitational Physics
    Published online:
    07 September 2018
    Print publication:
    27 September 2018, pp 129-155

  • Summary

    We derive the equations of motion for a variety of physical systems in the PPN formalism, including photons, fluid systems, and N-body systems consisting of well-separated self-gravitating objects. We also specialize to two-body systems and describe the framework for calculating perturbations of Keplerian orbit elements induced by post-Newtonian corrections in the equations of motion. For a class of theories based on an invariant action, we obtain the Lagrangian that describes the dynamics of an N-body system. We derive the locally-measured, or effective gravitational constant, as measured by a Cavendish experiment, within the PPN formalism. For spinning bodies, we obtain the equations of motion and the equations of spin precession.

  • 7 - The Classical Tests

  • Clifford M. Will, University of Florida
  • Book:
    Theory and Experiment in Gravitational Physics
    Published online:
    07 September 2018
    Print publication:
    27 September 2018, pp 156-169

  • Summary

    We describe three central tests of general relativity, sometimes call the "classical" tests: the deflection of light, the Shapiro time delay and the perihelion advance of Mercury. After deriving each effect in detail within the PPN formalism, we describe the various measurements that lead to tight bounds on the relevant PPN parameters.