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Show that the relativistic expression for kinetic energy \(\left(\gamma_{u}-1\right) m c^{2}\) is equivalent to the classical \(\frac{1}{2} m u^{2}\) when \(u \ll c\)

Short Answer

Expert verified
The relativistic kinetic energy formula is equivalent to the classical kinetic energy formula when the speed (u) is much less than the speed of light (c). This is confirmed by using a Taylor expansion to approximate the relativistic kinetic energy formula for \( u << c \).

Step by step solution

01

Write down the formulas

Starting with the relativistic formula for kinetic energy:\[K = (\gamma_{u}-1)mc^2\]where \( \gamma_u = \frac {1}{\sqrt {1-u^2/c^2}} \), m is the mass and c is the speed of light. The classical expression for kinetic energy is given by\[K_{classical} = \frac {1}{2}mu^2\]
02

Express \( \gamma_{u} \) in terms of \( u/c \)

Rewrite \( \gamma_u \) as\[\gamma_u = \frac {1}{\sqrt {1-(u/c)^2}}\]This will make the approximation step easier.
03

Approximate \( \gamma_{u} \) for \( u

For the case where \( u << c \), you can use a Taylor expansion of \( \gamma_u \) around \( u/c = 0 \) to approximate \( \gamma_u \). The first two terms of this expansion are\[\gamma_u \approx 1 + \frac {1}{2} (u/c)^2\]This approximation assumes that higher-order terms starting from the third are negligible.
04

Substitute the approximation back into the relativistic kinetic energy expression

Substitute the approximation from Step 3 into the kinetic energy formula \[ K = [1 + \frac {1}{2}(u/c)^2 - 1]mc^2 \] which simplifies to \[ K = \frac {1}{2}mu^2 \] which is the classical expression for kinetic energy.

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Key Concepts

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

Classical Kinetic Energy
Imagine pushing a playground swing: the harder you push, the faster it goes, and the more energy it has in motion. This is the essence of kinetic energy, which in classical mechanics is the energy an object possesses due to its motion. It is calculated using the formula \( K_{classical} = \frac{1}{2}mv^2 \), where \(m\) represents the mass of the object and \(v\) the velocity.

Think of \(m\) as how much stuff is being moved and \(v\) as how fast that stuff is moving. The factor of \(\frac{1}{2}\) is just a constant that comes from the work done to accelerate the object from rest to its current speed.

For example, if you throw a baseball, the kinetic energy would be half its mass times the square of its speed. It's important in classical mechanics to understand this concept because it's a foundational principle that explains how objects behave when they are in motion, such as how much work is needed to stop a moving car or the force of a ball hitting a window.
Taylor Expansion Approximation
The Taylor expansion is like a mathematical Swiss Army knife—it has a tool for approximating almost any function. At the heart of this method, is the idea that you can take a complicated function and approximate it by a polynomial, which is much simpler to work with.

To understand the Taylor expansion, imagine you're trying to describe the shape of a hilly landscape to a friend over the phone. Rather than detailing every rise and dip, you might describe it as generally 'uphill' or 'downhill' with a few 'bumps'—in essence, approximating the actual complex shape with a simpler, easy-to-communicate idea.

In mathematics, we start the approximation at a specific point—usually where we're most interested in the function's behavior—and use derivatives at that point to find the polynomial. The formula for a Taylor series expansion of a function \( f \) around \( a \) is: \[ f(x) = f(a) + f'(a)(x-a) + \frac{f''(a)}{2!}(x-a)^2 + \cdots \]

This series can go on indefinitely, but often, especially when \(x\) is very close to \(a\), only the first few terms are needed to get a good approximation. In physics, we use Taylor expansion to simplify complex relations under 'normal' conditions, such as approximating relativistic formulas where velocity is much less than the speed of light.
Special Relativity
Developed by Albert Einstein, special relativity revolutionized our understanding of space, time, and energy. Among its many profound insights is the realization that the laws of physics are the same for all non-accelerating observers, and that the speed of light in a vacuum is the same no matter the speed at which an observer travels.

One of the critical consequences of special relativity is that mass and energy are equivalent and can be converted into each other, a relationship expressed by Einstein's famous equation \( E=mc^2 \). Additionally, as an object moves faster, its mass increases, and it requires more energy to accelerate - a radical departure from Newtonian mechanics.

In the context of kinetic energy, special relativity modifies the classical expression to account for the increased mass. Instead of \(\frac{1}{2}mu^2\), it uses the more complex form \( (\gamma_{u}-1)mc^2 \), with the Lorentz factor \( \gamma_{u} = \frac {1}{\sqrt {1-u^2/c^2}} \). This accounts for the effects of relativity at high speeds close to the speed of light. However, when the velocity \(u\) is much less than \(c\), the classic expression is a very close approximation to the relativistic formula - this demonstrates the consistency between the principles of Newtonian mechanics and those of special relativity at everyday speeds.

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Most popular questions from this chapter

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