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Find the quadrupole moment of a distribution of charge on the surface of a sphere of radius \(a\) with surface charge density \(\sigma=\sigma_{0}\left(\frac{3}{2} \cos ^{2} \theta-\frac{1}{2}\right)\). Find the total energy stored in this distribution.

Short Answer

Expert verified
Answer: The total energy stored in the distribution of charge due to the quadrupole moment for the given charge distribution on a sphere is 0.

Step by step solution

01

Calculate the charge distribution on the sphere's surface

To find the charge distribution on the sphere's surface, we multiply the surface charge density formula by the surface area element \(dS\) which is given by \(a^2 \sin \theta d\theta d\phi\). This gives: $$d Q = \sigma dS = \sigma_0 \left(\frac{3}{2}\cos^2\theta - \frac{1}{2}\right) a^2 \sin \theta d\theta d\phi$$
02

Compute the quadrupole moment tensor components

The components of the quadrupole moment tensor are given by the following integral: $$ Q_{lm} = \frac{1}{2}\int \rho(\vec{r}) (3x_l x_m - r^2 \delta_{lm}) d^3 r$$ In spherical coordinates, the tensor components are given by: $$ Q_{\theta\theta}=\frac{1}{2}\int dQ(3a^2 \cos^2\theta - a^2)$$ $$ Q_{\phi\phi}=\frac{1}{2}\int dQ a^2(3 \cos^2\theta \sin^2\theta - \sin^2\theta)$$ $$ Q_{\theta\phi}=\frac{1}{2}\int dQ(3a^2 \cos\theta \sin\theta \cos\phi \sin\theta \sin\phi)$$
03

Compute the quadrupole moment tensor

Now, let's compute each component of the quadrupole moment tensor. First, we calculate \(Q_{\theta \theta}\): $$ Q_{\theta\theta}=\frac{1}{2}\int_{0}^{\pi}\int_{0}^{2\pi} dQ (3a^2 \cos^2\theta - a^2) =\frac{3}{2} a^2 \sigma_0 \int_{0}^{\pi}\int_{0}^{2\pi} (\cos^2\theta\sin\theta-\frac{1}{3}\sin\theta)d\theta d\phi = 0$$ Next, let's compute \(Q_{\phi\phi}\): $$ Q_{\phi\phi}=\frac{1}{2}\int_{0}^{\pi}\int_{0}^{2\pi} dQ a^2(3 \cos^2\theta \sin^2\theta - \sin^2\theta) = a^2 \sigma_0\int_{0}^{\pi}\int_{0}^{2\pi} (\frac{3}{2}\cos^2\theta\sin^3\theta-\frac{1}{2}\sin^3\theta)d\theta d\phi = 0$$ Lastly, we compute \(Q_{\theta\phi}\): $$ Q_{\theta\phi}=\frac{1}{2}\int_{0}^{\pi}\int_{0}^{2\pi} dQ(3a^2 \cos\theta \sin\theta \cos\phi \sin\theta \sin\phi) = 0$$ Since all components of the quadrupole moment tensor are zero, the quadrupole moment is also zero.
04

The Total Energy Stored

Now that we have found the quadrupole moment tensor, we can find the total energy stored in the distribution of charge. To find the total stored energy, we can use the following formula: $$ W = \frac{1}{2}\frac{1}{4\pi\epsilon_0}\int d^3 r \rho(\vec{r}) V(\vec{r})$$ However, since the quadrupole moment tensor is zero, the potential \(V(\vec{r})\) due to the quadrupole moment is also zero. Therefore, there is no energy stored in the distribution of charge due to the quadrupole moment.$$ W = 0$$.

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Key Concepts

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

Electrostatics
Electrostatics is the branch of physics that deals with the study of forces, fields, and potentials arising from static charges. It involves understanding how charged particles like protons and electrons interact with one another when they are not in motion.

In this particular problem, we are analyzing a distribution of charge on a sphere, which is a typical electrostatic system. The sphere has a set radius denoted by \(a\), and the charges are distributed across its surface according to a specific formula for surface charge density.

This formula determines how charges are spaced around the sphere and ultimately influences the electrostatic potential and field around it.
  • The concepts of potential energy and electric fields are central to electrostatics.
  • Understanding electrostatics is vital for fields such as electronics, electromagnetism, and many engineering applications.
Charge Distribution
Charge distribution refers to how electric charge is spread over an object or within a space. In this exercise, the charge distribution is specified on the surface of a sphere, characterized by a function of the angle \(\theta\).

The charge on the surface changes depending on the angle, with a density given by \(\sigma = \sigma_{0}\left(\frac{3}{2} \cos^2 \theta - \frac{1}{2}\right)\). This non-uniform distribution affects the resulting electrostatic properties of the sphere.

Understanding charge distribution is crucial:
  • It dictates how electric fields and potentials are structured around an object.
  • Affects the calculations of forces and energy in a system.
  • Plays a significant role in the design and functioning of capacitors and other devices.
Surface Charge Density
Surface charge density \(\sigma\) is the amount of electric charge per unit area on the surface of an object. In our scenario, we have a non-uniform surface charge density described by the formula \(\sigma = \sigma_{0}\left(\frac{3}{2} \cos^2 \theta - \frac{1}{2}\right)\).

This function indicates how the charge density varies with the polar angle \(\theta\), causing some areas on the sphere to have higher or lower charge concentration.
  • The concept of surface charge density is essential for understanding and calculating the effects of electrostatic forces and fields.
  • It can influence physical phenomena such as electrical conductivity and capacitance.
  • Surface charge density distributions are crucial in designing and analyzing electronic components like sensors and semiconductors.
Energy Calculation
Energy calculation in electrostatics often involves determining the energy stored in an electric field or charge distribution. Here, the problem involves calculating the energy stored due to the charges distributed over the sphere's surface.

Typically, the formula \( W = \frac{1}{2}\frac{1}{4\pi\epsilon_0}\int d^3 r \rho(\vec{r}) V(\vec{r})\) would be used to calculate the energy stored. However, since the quadrupole moment tensor was found to be zero in this problem, the potential and thus stored energy are also zero.
  • Energy calculations help assess the stability and reactivity of a system.
  • Accurate energy estimates are critical in fields like power electronics and nuclear physics.
  • Understanding potential energy in charge distributions aids in developing efficient electrical systems and devices.

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Most popular questions from this chapter

Assume that the pressure \(p\) in a star with spherical symmetry is related to the density \(\rho\) by the (distinctly unrealistic) equation of state \(p=\frac{1}{2} k \rho^{2}\), where \(k\) is a constant. Use the fluid equilibrium equation obtained in Problem 23 to find a relation between \(\rho\) and \(\Phi .\) Hence show that Poisson's equation yields $$ \frac{\mathrm{d}^{2}[r \rho(r)]}{\mathrm{d} r^{2}}=-\frac{4 \pi G}{k} r \rho(r) $$ Solve this equation with the boundary conditions that \(\rho\) is finite at \(r=0\) and vanishes at the surface of the star. Hence show that the radius \(a\) of the star is determined solely by \(k\) and is independent of its mass \(M\). Show also that \(M=(4 / \pi) a^{3} \rho(0)\).

Two equal charges \(q\) are located at the points \((\pm a, 0,0)\), and two charges \(-q\) at \((0, \pm a, 0)\). Find the leading term in the potential at large distances, and the corresponding electric field.

A diffuse spherical cloud of gas of density \(\rho\) is initially at rest, and starts to collapse under its own gravitational attraction. Find the radial velocity of a particle which starts at a distance \(a\) from the centre when it reaches the distance \(r\). Hence, neglecting other forces, show that every particle will reach the centre at the same instant, and that the time taken is \(\sqrt{3 \pi / 32 \rho G}\). Evaluate this time in years if \(\rho=10^{-19} \mathrm{~kg} \mathrm{~m}^{-3}\). (Hint: Assume that particles do not overtake those that start nearer the centre. Verify that your solution is consistent with this assumption. The substitution \(r=a \sin ^{2} \theta\) may be used to perform the integration.) Estimate the collapse time for the Earth and for the Sun, taking a suitable value of \(\rho\) in each case

Find the gravitational potential at large distances of a thin circular loop of radius \(a\) and mass \(m\), up to terms of order \(r^{-3}\). Find also the potential, and the leading term in the gravitational field near the origin, at distances \(r \ll a\).

Suppose that at some time the Moon had been ocean-covered and rotating relative to the Earth. Find the ratio between the heights of the tides raised on the Moon by the Earth and on the Earth by the Moon. (The Moon's radius is \(R_{\mathrm{M}}=0.27 R_{\mathrm{E}}\).) Estimate how high the tides on the Moon would have been when the Earth-Moon distance was \(10 R_{\mathrm{E}}\).

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