College Physics
11th Edition
ISBN: 9781305952300
Author: Raymond A. Serway, Chris Vuille
Publisher: Cengage Learning
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- A non-rotating black hole has an ‘edge’ at what’s called it’s Schwartzschildradius. For a black hole of mass M, the Schwartzschild radius isRSch = 2GM/(c^2) where G is the gravitational constant and c is the speed of light. Close to black holes, we really should use Einstein’s theory of gravity (General Relativity) instead of Newton’s, but Newton’s is still a good approximation.Using Newtonian Gravity, find the gravitational force on a mass m at theSchwartzschild radius of a black hole. (Your answer for this should look likeFgrav = an expression in terms of G, M, m, c and numbers.) Is the forcesmaller or larger for a more massive black hole?arrow_forwardAs a star ages, it is believed to undergo a variety of changes. One of the last phases of a star's life is to gravitationally collapse into a black hole. If suppose our Sun would end up a Black hole, what will happen to the orbit of the planets of the solar system? (Assuming that the planets are not affected by the evolving stages of the Sun prior to becoming a black hole and noting that for calculation of gravitational force of attraction, the distance being considered is from center to center of the two bodies). Justify your answer.arrow_forwardNeptune has a mass of 1.0 × 1026 kg and is 4.5 × 10⁹ km from the Sun with an orbital period of 177.5 years. Planetesimals in the outer primordial solar system 4.5 billion years ago coalesced into Neptune over hundreds of millions of years. If the primordial disk that evolved into our present day solar system had a radius of 10¹1 km and if the matter that made up these planetesimals that later became Neptune was spread out evenly on the edges of it, what was the orbital period of the outer edges of the primordial disk? Express your answer rounded to the nearest year, and be sure not to do any rounding before expressing your final answer. P = yearsarrow_forward
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