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In 1963 Yu. G. Klimov, S. Liebes, and Sjur Refsdal recognized independently that quasars are an ideal light source for the gravitational lens effect. [23] It was not until 1979 that the first gravitational lens would be discovered. It became known as the "Twin QSO" since it initially looked like two identical quasistellar objects.
The alternating pressure build up and escape causes a pulsing effect, hence the name: pulser pump. The maximum air pressure that can accumulate depends on the height of the water column between the air chamber and the lower reservoir. The deeper the air chamber is positioned, the higher the elevation to which the water can be pumped.
In weak gravitational lensing, the Jacobian is mapped out by observing the effect of the shear on the ellipticities of background galaxies. This effect is purely statistical; the shape of any galaxy will be dominated by its random, unlensed shape, but lensing will produce a spatially coherent distortion of these shapes.
Gravitational lensing is an effect of gravitation, most commonly associated with General relativity. Subcategories. This category has the following 2 subcategories ...
The Oppenheimer–Snyder model of continued gravitational collapse is described by the line element [13] = + (+ +) The quantities appearing in this expression are as follows: The coordinates are ( τ , R , θ , ϕ ) {\displaystyle (\tau ,R,\theta ,\phi )} where θ , ϕ {\displaystyle \theta ,\phi } are coordinates for the 2-sphere.
The key difference between an embedded lens and a traditional lens is that the mass of a standard lens contributes to the mean of the cosmological density, whereas that of an embedded lens does not. Consequently, the gravitational potential of an embedded lens has a finite range, i.e., there is no lensing effect outside of the void.
Strong gravitational lensing is a gravitational lensing effect that is strong enough to produce multiple images, arcs, or Einstein rings. Generally, for strong lensing to occur, the projected lens mass density must be greater than the critical density , that is Σ c r {\displaystyle \Sigma _{cr}} .
The difference between de Sitter precession and the Lense–Thirring effect is that the de Sitter effect is due simply to the presence of a central mass, whereas the Lense–Thirring effect is due to the rotation of the central mass. The total precession is calculated by combining the de Sitter precession with the Lense–Thirring precession.