LaTeX Exercise 1

The images of the equations on this page were taken from the Wikipedia pages referenced for each equation.

Imports


In [2]:
from IPython.display import Image

Typesetting equations

In the following cell, use Markdown and LaTeX to typeset the equation for the probability density of the normal distribution $f(x, \mu, \sigma)$, which can be found here. Following the main equation, write a sentence that defines all of the variable in the equation.


In [3]:
Image(filename='normaldist.png')


Out[3]:
\begin{equation*} f(x,\mu,\sigma) = \frac{1}{\sigma\sqrt{2\pi}}e^{-\frac{(x-\mu)^2}{2\sigma^2}} \end{equation*}

Where $\mu$ is the mean or expectaion of the distribution and $\sigma$ is the standard deviation.

In the following cell, use Markdown and LaTeX to typeset the equation for the time-dependent Schrodinger equation for non-relativistic particles shown here (use the version that includes the Laplacian and potential energy). Following the main equation, write a sentence that defines all of the variable in the equation.


In [4]:
Image(filename='tdseqn.png')


Out[4]:
\begin{equation*} i\hbar\frac{\partial}{\partial t}\Psi(r,t) = \left[\frac{-\hbar^2}{2\mu}\nabla^2+V(r,t)\right]\Psi(r,t) \end{equation*}

where $r$ is radius, $t$ is time, $\hbar$ is plank's constant divided by 2$\pi$, $\mu$ is the particle's reduced mass, $V(r,t)$ is the particle's potential energy, $\nabla^2$ is the Laplacian (differential opperator), and $\Psi(r,t)$ is the wave function.

In the following cell, use Markdown and LaTeX to typeset the equation for the Laplacian squared ($\Delta=\nabla^2$) acting on a scalar field $f(r,\theta,\phi)$ in spherical polar coordinates found here. Following the main equation, write a sentence that defines all of the variable in the equation.


In [5]:
Image(filename='delsquared.png')


Out[5]:
\begin{equation*} \Delta f= \frac{1}{r^2}\frac{\partial}{\partial r} \left(r^2\frac{\partial f}{\partial r} \right)+ \frac{1}{r^2sin\theta}\frac{\partial}{\partial \theta} \left(sin\theta\frac{\partial f}{\partial \theta} \right) + \frac{1}{r^2sin^2\theta} \frac{\partial^2 f}{\partial \psi^2} \end{equation*}

Where $\Delta = \nabla^2$ acting on a scalar field in spherical cooridnates, $r$ represents the radius, $\psi$ is the azimuthal angle and $\theta$ is the zenith angle/co-latitude.