Kepler's Second Law, Eccentricity, Questions And Answers

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Contents
Task 1 2
Part A 2
Part B 2
Task 2 4
Part A 4
Part B 4
Task 3 5
Part A 5
Part B 5

Task 1
Part A
The Earth is orbited by 2,271 satellites, 10,000 rocks and debris and over 500,000 pieces of junk and smaller debris. But what forces are causing this to occur? Eccentricity is a measurement of how much the conic section deviates from being circular. This means that it is a measurement of how much the orbit (in this case) deviates from the 0 or the center.
When a satellite orbits the Earth in moves through an atmosphere depending on the satellite, when this occurs it can begin to venture inwards or outwards of the orbit due to Earth`s seasons and direction change creating a fluctuation in the amount eccentricity the
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In other words ellipses can be round or elongated; the degree of stretch is known as eccentricity. Eccentricity is defined as the ratioc/2a. C defined as the distance between the two focuses of the ellipse and a is the semi-major axis. In fact, a circle is an ellipse with an eccentricity of zero. Kepler`s second law is the speed of the planets along their elliptical orbits is such that they sweep out equal areas in equal periods of time. This means that the nearer the planets are to the Sun, the faster they travel along their orbit, so that a line drawn between the planet and the Sun can sweep out the same area. The third of Kepler`s law is the Square of the period of any planet is proportional to the cube of the semi major axis of its orbit. The equation for the law isT^2/(R_av^3 )=k. In the equation k is the constant. This rule is used to describe and calculate the relationship between the distance of planets from the sun and their orbital periods. According to this law the expression P2a−3 has the same value for all the planets in the solar system. In this expression P is the time taken for a planet to complete an entire orbit around the sun. A is the mean value of the maximum and minimum distances between the sun and the planets. The constant in the corresponding formula in Newtonian form is:
P^2/a^3 =(4π^2)/G(M+m) ≈(4π^2)/GM=Constant
In the following equation M is equal to the mass of the sun, m equals the mass of the planet. G is the gravitational constant. Because the sun us much heavier than any planet, Keplers third law correlates to Newtons equations (Laws Of Planetary Motion,

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