Commit dd2a12f4 authored by Tianbai Xiao's avatar Tianbai Xiao
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Update physics.rst

Former-commit-id: 3ff149f4
parent f35b90cb
......@@ -56,11 +56,12 @@ where the particles don't interact with one another but scatter with the backgro
For convenience, we reformulate the particle velocity into polar coordinates :math:`\{r, \phi, \theta \}`
.. math::
:label: boltzmann
:label: porbz
&\left[\frac{1}{\mathrm{~V}} \frac{\partial}{\partial t}+\Omega \cdot \nabla+\Sigma(r, E, t)\right] \psi(r, \Omega, E, t) \\
&=\int_{0}^{\infty} d E^{\prime} \int_{\mathcal R^2} d \Omega^{\prime} \Sigma_{s}\left(r, \Omega^{\prime} \bullet \Omega, E^{\prime} \rightarrow E\right) \psi\left(r, \Omega^{\prime}, E^{\prime}, t\right)
\frac{\partial \psi}{\partial t}+\Omega \cdot \nabla_x \psi = Q(\psi)
The particle distribution :math:`\psi(t, x, \Omega, E)` is often called angular flux.
The particle distribution :math:`\psi(t, r, \Omega, E)` here is often named as angular flux.
The continuous slowing down approximation
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