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In 1783, an amateur astronomer named John Michell theorized that if an object had a radius that was five hundred times larger than the sun, but with the approximate average density of the sun, the velocity that would be required to escape the object’s gravitational pull would be faster than the speed of light (Temming). Simon Pierre Laplace, a French astronomer and mathematician, came to a similar conclusion a few years later (Temming). However, their findings were largely discredited since Michell believed that light particles had mass, when in fact, light has a wave nature, proven by Thomas Young’s double slit experiment in 1803 (Temming). Michell and Laplace’s discoveries were found to have a kernel of validity however, when in 1915,*…show more content…*

The very first object to be considered a black hole is Cygnus X-1, discovered in 1971 when radio emissions were detected from the area (Redd, “Black Holes: Facts”). Scientists explored the area further, eventually finding a hidden companion, which was identified as a black hole (Redd, “Black Holes: Facts”). A black hole displays many rather unique characteristics. First and foremost, there are only three externally measurable properties of a black hole; Mass, electric charge, and, if applicable, rate of rotation (Freudenrich). This is referred to as the no-hair theorem (“Fuzzy Wuzzy”). These three elements form a stable black hole. If these elements are synonymous with any other black hole, the region is not identifiable or distinguishable from a separate entity. The mass of a black hole can be calculated by using a modified version of Kepler’s Third Law of Planetary Motion (Freudenrich). Secondly, black holes follow their own specific rules, called the Four Laws of Black Hole Mechanics (“Properties of Black Holes”). These rules coincide with the rules of thermodynamics, though they are specific to black holes (“Black Hole Thermodynamics”). The Zeroth Law is, “The surface gravity k at the event horizon is constant: it has the same value everywhere on the event horizon (“Properties of Black Holes”).” This means that the event horizon has the same surface gravity across its entire area. The First Law is, “The change in

The very first object to be considered a black hole is Cygnus X-1, discovered in 1971 when radio emissions were detected from the area (Redd, “Black Holes: Facts”). Scientists explored the area further, eventually finding a hidden companion, which was identified as a black hole (Redd, “Black Holes: Facts”). A black hole displays many rather unique characteristics. First and foremost, there are only three externally measurable properties of a black hole; Mass, electric charge, and, if applicable, rate of rotation (Freudenrich). This is referred to as the no-hair theorem (“Fuzzy Wuzzy”). These three elements form a stable black hole. If these elements are synonymous with any other black hole, the region is not identifiable or distinguishable from a separate entity. The mass of a black hole can be calculated by using a modified version of Kepler’s Third Law of Planetary Motion (Freudenrich). Secondly, black holes follow their own specific rules, called the Four Laws of Black Hole Mechanics (“Properties of Black Holes”). These rules coincide with the rules of thermodynamics, though they are specific to black holes (“Black Hole Thermodynamics”). The Zeroth Law is, “The surface gravity k at the event horizon is constant: it has the same value everywhere on the event horizon (“Properties of Black Holes”).” This means that the event horizon has the same surface gravity across its entire area. The First Law is, “The change in

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