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Taking the earth to be a uniform sphere of radius \(6400 \mathrm{~km}\) and the value of \(g\) at the surface to be \(10 \mathrm{~m} \mathrm{~s}^{-2}\), calculate the energy needed (in \(\times 10^{10} \mathrm{~J}\) ) to raise a satellite of mass \(2000 \mathrm{~kg}\) to a height of \(800 \mathrm{~km}\) above the earth's surface and to set it into circular orbit at that altitude.

Short Answer

Expert verified
The energy needed is approximately 68.32 \( \times 10^{10} \) Joules.

Step by step solution

01

Determine the Gravitational Potential Energy at Height

First, we need to calculate the gravitational potential energy (GPE) required to lift the satellite from the surface of the Earth to a height of 800 km. The GPE at a height \( h \) is given by:\[U = G \frac{mM}{R+h} - G \frac{mM}{R} = m g R \left(1 - \frac{R}{R + h}\right)\]Where:- \( m = 2000 \; \text{kg} \) is the mass of the satellite,- \( g = 10 \; \text{m/s}^2 \) is the acceleration due to gravity at the surface,- \( R = 6400 \times 10^3 \; \text{m} \) is the radius of the Earth,- \( h = 800 \times 10^3 \; \text{m} \) is the altitude.Now, substitute the values:\[U = 2000 \times 10 \times 6400 \times 10^3 \times \left(1 - \frac{6400}{7200}\right)\]Calculating this gives:\[U \approx 2000 \times 10 \times 6400 \times 10^3 \times \frac{800}{7200} = 2000 \times 10 \times 6400 \times 10^3 \times 0.1111 \approx 14.22 \times 10^{10} \; \text{J}\]
02

Calculate the Kinetic Energy for Circular Orbit

Next, we calculate the kinetic energy (KE) required for the satellite to maintain a circular orbit at 800 km above the Earth's surface. The formula for KE in orbit is:\[KE = \frac{1}{2} \cdot m \cdot v^2\]where orbital velocity \( v \) is given by:\[v = \sqrt{\frac{GM}{R+h}}\]Given that:- \( gR^2 = GM \), we substitute \( GM \) to find \( v \):\[v = \sqrt{gR^2 / (R + h)}\]Substitute values:\[v = \sqrt{10 \times 6400^2 / 7200} \approx 7358 \; \text{m/s}\]Now calculate \( KE \):\[KE = \frac{1}{2} \times 2000 \times (7358)^2 \approx 54.1 \times 10^{10} \; \text{J}\]
03

Calculate Total Energy Required

To find the total energy required, sum the gravitational potential energy and kinetic energy needed:\[\text{Total Energy} = U + KE \approx 14.22 \times 10^{10} + 54.1 \times 10^{10} = 68.32 \times 10^{10} \; \text{J}\]
04

Convert to Requested Energy Units

Since the problem asks for energy in terms of \( \times 10^{10} \; \text{J} \), the total energy required is 68.32 \( \times 10^{10} \) J as calculated in the previous step.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Kinetic Energy
Kinetic energy is the energy an object has due to its motion. In the context of satellites orbiting the Earth, this concept is crucial when considering how much energy is needed to maintain an orbit. When a satellite is in motion at a given velocity, its kinetic energy (KE) can be calculated using the formula:
  • \[ KE = \frac{1}{2} \cdot m \cdot v^2 \]
  • Where \( m \) is the satellite's mass, and \( v \) is its velocity.
The kinetic energy relates directly to the satellite's need to stay in a circular orbit—the faster it moves, the more kinetic energy it has.
This is because, at higher speeds, it can counteract the pull of Earth's gravity more effectively.
Understanding this energy is crucial for satellite deployment at specific altitudes, ensuring they have enough energy to maintain a stable orbit without additional propulsion.
Circular Orbit
A circular orbit is a path taken by an object moving around a planet, like Earth, in the shape of a circle. Satellites often use circular orbits because they provide a stable path that does not change over time.

In a circular orbit, both the distance of the satellite from the Earth's center and its speed remain constant. Several factors play a role in maintaining a circular orbit:
  • Gravitational Force: This is the force pulling the satellite towards the Earth, providing the inward force needed to keep it moving in a circle.
  • Centripetal Force: This arises due to the satellite's inertia as it moves. The balance between gravitational and centripetal forces maintains the orbit.
  • Consistent Speed: The satellite’s speed must be carefully calculated for its orbital height to ensure gravitational forces precisely balance the forces keeping it in motion.
Achieving such an orbit requires precise calculations and energy inputs to lift the satellite and give it the appropriate speed and trajectory.
Orbital Velocity
Orbital velocity is the speed a satellite needs to travel in order to maintain a stable orbit around Earth. It is determined by the gravitational pull of the Earth and the desired altitude of the orbit.

To find the orbital velocity, we use the formula:
  • \[ v = \sqrt{\frac{GM}{R+h}} \]
  • Where \( v \) is the orbital velocity, \( G \) is the gravitational constant, \( M \) is the Earth's mass, \( R \) the Earth's radius, and \( h \) is the altitude of the satellite above Earth's surface.
Another simplified approach, using gravitational acceleration \( g \), is:
  • \[ v = \sqrt{gR^2 / (R + h)} \]
Orbital velocity must be achieved exactly for a satellite to remain in orbit. Too slow, and the satellite will fall back to Earth; too fast, and it might escape Earth's gravity.
Thus, the calculation of orbital velocity ensures that the satellite stays on its intended path without the need for further corrective maneuvers.

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Most popular questions from this chapter

A double star consists of two stars having masses \(M\) and \(2 M\). The distance between their centres is equal to \(r .\) They revolve under their mutual gravitational interaction. Then, which of the following statements are not correct? (1) Heavier star revolves in orbit of radius \(2 r / 3\) (2) Both the stars revolve with the same speed, period of which is equal to \(\left(2 \pi / r^{3}\right)\left(2 G M^{2} / 3\right)\) (3) Kinetic energy of the heavier star is twice that of the other star. (4) None of the above

The small dense stars rotate about their common centre of mass as a binary system, each with a period of 1 year. One star has mass double than that of the other, while mass of the lighter star is one-third the mass of the Sun. The distance between the two stars is \(r\) and the distance of the earth from the Sun is \(R\); find the ratio \(r / R\).

Three particles, each of mass \(M\), are placed at the three corners of an equilateral triangle of side \(l\). What is the force due to this system of particles on another particle of mass \(m\) placed at the midpoint of any side? (1) \(\frac{3 G M m}{4 l^{2}}\) (2) \(\frac{4 G M m}{3 l^{2}}\) (3) \(\frac{G M m}{4 l^{2}}\) (4) \(\frac{4 G M m}{l^{2}}\)

Suppose the gravitational force varies inversely as the nh power of the distance. Then, the time period of a planet in \(a\) circular orbit of radius \(R\) around the Sun will be proportional to (1) \(R^{n}\) (2) \(R^{(n+1)}{2}\) (3) \(R^{\frac{(n-1)}{2}}\) (4) \(R^{-n}\)

An astronaut, inside an earth satellite, experiences weightlessness because (1) no external force is acting on him (2) he is falling freely (3) no reaction is exerted by the floor of the satellite (4) he is far away from the earth's surface

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