Universe
Universe
11th Edition
ISBN: 9781319039448
Author: Robert Geller, Roger Freedman, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 5, Problem 1Q
To determine

To explain: Whether the eclipse of Jupiter will appear earlier, later, or neither, if it goes under retrograde motion, as seen from Earth.

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The path of a total solar eclipse is modeled by f(t)=0.00387t^2−0.481t+26.103​, where​ f(t) is the latitude in degrees south of the equator at t minutes after the start of the total eclipse. What is the latitude closest to the​ equator, in​ degrees, at which the total eclipse will be visible.
In addition to the formation of shadows and eclipses,  what other phenomena prove the rectilinear propagation of light?
Lunar eclipses are always eclipses of a full Moon. That is, the Moon is always seen full just before and after Earth’s shadow passes over it. Why is this? Why can we never have a lunar eclipse when the Moon is in its crescent or half-moon phase?
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General Relativity: The Curvature of Spacetime; Author: Professor Dave Explains;https://www.youtube.com/watch?v=R7V3koyL7Mc;License: Standard YouTube License, CC-BY