Taking M⊙=2×1030 kg{“version”:”1.1″,”math”:”M⊙=2&#xD7…

Taking M⊙=2×1030 kg{“version”:”1.1″,”math”:”M⊙=2×1030 kg”} and R⊙=7×108 m{“version”:”1.1″,”math”:”R⊙=7×108 m”}, find the maximum deflection angle for light originating behind the sun observed during a solar eclipse. 

Taking M⊙=2×1030 kg{“version”:”1.1″,”math”:”M⊙=2&#xD7…

Taking M⊙=2×1030 kg{“version”:”1.1″,”math”:”M⊙=2×1030 kg”} and R⊙=7×108 m{“version”:”1.1″,”math”:”R⊙=7×108 m”}, find the maximum deflection angle for light originating behind the sun observed during a solar eclipse. 

Usually a source object will not lie on the axis determined…

Usually a source object will not lie on the axis determined by the observer and the deflecting mass. Which of the following are probable consequences of that asymmetric arrangement? I. In a dual-image lens effect, one image will show a time delay from the other. II. The effective index of refraction will differ significantly from its value for on-axis sources. III. An observed radio ring will appear thicker and brighter on one side than the other. 

Usually a source object will not lie on the axis determined…

Usually a source object will not lie on the axis determined by the observer and the deflecting mass. Which of the following are probable consequences of that asymmetric arrangement? I. In a dual-image lens effect, one image will show a time delay from the other. II. The effective index of refraction will differ significantly from its value for on-axis sources. III. An observed radio ring will appear thicker and brighter on one side than the other. 

Determine the effective focal length of a gravitational lens…

Determine the effective focal length of a gravitational lens created by a celestial object of mass M0 and radius r0 assuming both that dS >> dL, so that rays coming from the source are parallel at the lens, and that tanθ≈θ{“version”:”1.1″,”math”:”tanθ≈θ”} (in radians) for small angles.

Determine the effective focal length of a gravitational lens…

Determine the effective focal length of a gravitational lens created by a celestial object of mass M0 and radius r0 assuming both that dS >> dL, so that rays coming from the source are parallel at the lens, and that tanθ≈θ{“version”:”1.1″,”math”:”tanθ≈θ”} (in radians) for small angles.