Subfield: Electromagnetism

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Figure 1

The following questions are designed to guide you to find the answer one step by one step.

Background information of the interaction between the solar wind and the Earth's magnetic field

It is well known that the Earth has a substantial magnetic field. The field lines defining the structure of the Earth's magnetic field is similar to that of a simple bar magnet, as shown in Figure 2. The Earth's magnetic field is disturbed by the solar wind, whichis a high-speed stream of hot plasma. (The plasma is the quasi-neutralionized gas.)The plasma blows outward from the Sun and varies in intensity with the amount of surface activity on the Sun. The solar wind compresses the Earth's magnetic field. On the other hand, the Earth's magnetic field shields the Earth from much of the solar wind. When the solar wind encounters the Earth's magnetic field, it is deflected like water around the bow of a ship, as illustrated in Figure 3.

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Figure 2



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Figure 3

The curved surface at which the solar wind is first deflected is called the bow shock. The corresponding region behind the bow shock andfront of the Earth's magnetic field is called themagnetosheath. The region surroundedby the solar wind is called the magnetosphere.The Earth's magnetic field largely prevents the solar wind from enteringthe magnetosphere. The contact region between the solar wind and the Earth's magnetic field is named the magnetopause. The location of the magnetopause is mainly determined by the intensity and the magnetic field direction of the solar wind. When the magnetic field in the solar wind is antiparallel to the Earth's magnetic field, magnetic reconnection as shown in Figure 4 takes place at the dayside magnetopause, which allows some charged particles ofthe solar wind in the region "A" to move into the magnetotail "P" on the night side as illustrated in Figure 5. A powerful solar wind can push the dayside magnetopause tovery close to the Earth, which could cause a high-orbit satellite (such as a geosynchronous satellite) to be fully exposed to the solar wind. The energetic particles in the solar wind could damage high-tech electronic components in a satellite.Therefore, it isimportant to study the motion of charged particles in magnetic fields, which will give an answer of the aurora generation and could help us to understand the mechanism of the interaction between the solar wind and the Earth's magnetic field.
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Figure 4






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Figure 5

Numerical values of physical constants and the Earth's dipole magnetic field:

Speed of light in vacuum: $c=2.998 \times 10^{8} \mathrm{~m} / \mathrm{s}$;

Permittivity in vacuum: $\varepsilon_{0}=8.9 \times 10^{-12} \mathrm{C}^{2} /\left(\mathrm{N} \cdot \mathrm{m}^{2}\right)$;

Permeability in vacuum: $\mu_{0}=4 \pi \times 10^{-7} \mathrm{~N} / \mathrm{A}^{2}$;

Charge of a proton: $e=1.6 \times 10^{-19} \mathrm{C}$;

Mass of an electron: $m=9.1 \times 10^{-31} \mathrm{~kg}$;

Mass of a proton: $m_{p}=1.67 \times 10^{-27} \mathrm{~kg}$;

Boltzmann's constant: $k=1.38 \times 10^{-23} \mathrm{~J} / \mathrm{K}$;

Gravitational acceleration: $g=9.8 \mathrm{~m} / \mathrm{s}^{2}$;

Planck's constant: $h=6.626 \times 10^{-34} \mathrm{~J} \cdot \mathrm{s}$

Earth's radius $R_{E}=6.4 \times 10^{6} \mathrm{~m}$.

The Earth's dipole magnetic field can be expressed as

$$
\vec{B}_{d}=\frac{B_{0} R_{E}^{3}}{r^{5}}\left[3 x z \hat{x}-3 y z \hat{y}+\left(x^{2}+y^{2}-2 z^{2}\right) \hat{z}\right] \quad,\left(r \geq R_{E}\right)
\tag{1}
$$

where $r=\sqrt{x^{2}+y^{2}+z^{2}}, B_{0}=3.1 \times 10^{-5} \mathrm{~T}$, and $\hat{x}, \hat{y}, \hat{z}$ are the unit vectors in the $x, y, z$ directions, respectively.

Questions:

(a)
Context question:
(i)  Before we study the motion of a charged particle in the Earth's dipole magnetic field, we first consider the motion of an electron in a uniform magnetic field $\vec{B}$. When the initial electron velocity $\vec{v}$ is perpendicular to the uniform magnetic field as shown in Figure 6, please calculate the electron trajectory. The electron is initially located at $(\mathrm{x}, \mathrm{y}, \mathrm{z})=(0,0,0)$.

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Figure 6
Context answer:
$$
\left\{\begin{array}{l}
x^{2}+y^{2}=r_{c}^{2} \\
z=0
\end{array}\right.
$$

where $\left|r_{c}\right|=\frac{v_{\perp}}{\left|\omega_{c}\right|}=\frac{m v_{\perp}}{e B}$ is the gyro radius.


Context question:
(ii)  Please determine the electric current of the electron motion and calculate the magnetic moment $\vec{\mu}=I \vec{A}$, where $\stackrel{\mathrm{I}}{A}$ is the area of the electron circular orbit and the direction of $\vec{A}$ is determined by the right-hand rule of theelectric current.
Context answer:
\boxed{$I=\frac{e^{2} B}{2 \pi m}$ , $\vec{\mu}=-\frac{m v_{\perp}^{2}}{2 B^{2}} \vec{B}$}


Context question:
(iii)  If the initial electron velocity $\vec{v}$ is not perpendicular to the uniform magnetic field, i.e, the angle $\theta$ between $\vec{B}$ and $\vec{v}$ is $0^{0}<\theta<90^{\circ}$, please give the screw pitch (the distance along the z-axis between successive orbits) of the electron trajectory.
Context answer:
\boxed{$2 \pi \frac{m v}{e B} \cos \theta$}


Extra Supplementary Reading Materials:

(b)  In the uniform background magnetic field as shown in Figure 6, theplasma density isnonuniform in $x$. For simplicity, we assume that the temperature and the distribution of the ions andelectrons are the same. Thus, the plasma pressure can be expressed as

$$
p(x)=k T\left[n_{i}(x)+n_{e}(x)\right]=2 k T n(x)=2 k T\left(n_{0}+\alpha x\right),
$$

Where $B, T, k, n_{0}$, and $\alpha$ are positive constants, $n_{i}(x)$ and $n_{e}(x)$ are the number densities of the ions and electrons.
Context question:
(i)  Please explain the generation mechanism of the electric current by a schematic drawing.
Context answer:
开放性回答


Context question:
(ii)  If both the ions and electrons have a Maxwellian distribution, the ion distribution is

$f_{i}\left(x, v_{\perp}, v_{\|}\right)=n_{i}(x)\left(\frac{m_{i}}{2 \pi k T}\right)^{3 / 2} e^{-m_{i}\left(v_{\perp}^{2}+v_{\|}^{2}\right) / 2 k T}$,

please calculate the constant $\beta$ in the magnetization $M=\beta n(x) \frac{k T}{B}$, where the magnetization M is the magnetic moment per unit volume. (Hint: We have $\int_{0}^{\infty} x \exp (-x) d x=1$ and

$\left.\int_{-\infty}^{\infty} \exp \left(-x^{2}\right) d x=\sqrt{\pi} \cdot\right)$
Context answer:
\boxed{$\beta=-2$}


Question: (c) Now let's go back to the Earth's dipole magnetic field. Please apply the result from Question(b) to calculate the ratio of the diamagnetic field and the Earth's dipole magnetic field in Equation (1) at the position $\left(x=10 \mathrm{R}_{\mathrm{E}}, y=0, z=1 \mathrm{R}_{\mathrm{E}}\right)$. The plasma pressure is assumed to be $p(z)=p_{0} e^{-(z / a)^{2}}$, where $p_{0}=3 \times 10^{-10} \mathrm{pa}$ and $a=2 R_{E}$. The magnetic field around this position is also assumed to be uniform. Be aware of the difference in the coordinate systemsin Questions (b) and (c). (Hint: The diamagnetic field is given by $B_{m x}=\mu_{o} M$.)

Solution:
Using the equation for the magnetization field $B_{m x}=\mu_{o} M$ and the $\mathrm{x}$ component of the Earth's dipole magnetic field at $\left(x=10 R_{E}, y=0, z=1 R_{E}\right)$, we have

$$
\left|B_{m x} / B_{d}\right|=\left.\mu_{0} \frac{p(z)}{B_{d}^{2}\left(10 R_{E}, 0, z\right)}\right|_{z=R_{E}}=\frac{\mu_{0} e^{-0.25} P_{0}}{28.5 \times 10^{-8} B_{0}^{2}} \approx 1.0
$$

Final answer: 1.0