Welcome to my website! Here you can find some general information about my research and movies of my simulations.

High-redshift analogue Evolution of 1, 0.1, 0.01, and 0.001 micron radius dust grains (from left to right) under sputtering in a multi-phase galactic outflow. The galaxy has a star formation rat...

This post is a summary of Richie et al. 2024, my first paper on dust evolution in galactic outflows. In this paper, we used idealized simulations of individual dusty clouds in hot galactic winds to...

When simulating dust, a major simplification in modeling can be made through assumptions about dust dynamics. Dust dynamics (which aren’t straightforward to calculate in Eulerian hydrodynamics simu...

Overview To understand how dust is transported in galactic winds, I’ve been thinking about the primary mechanism that destroys dust at high gas temperatures in galaxies, sputtering. In very simpl...

The cloud crushing time is given by: $t_{cc}=\frac{\chi^{1/2}a_0}{v_b}.$ So, for a cloud of radius $a_0=0.1~\text{kpc}$, the cloud crushing times are: $\chi$ Physical Scenario...

Gas Temp $n=0.001~\text{cm}^{-3}$ $n=0.01~\text{cm}^{-3}$ $n=0.1~\text{cm}^{-3}$ $n=1~\text{cm}^{-3}$ $10^1~\text{K}$ $1.8\times10...

Simulating Dusty Clouds With Cholla Cloud-Wind Dynamics The dynamics of an interaction between a cool, dense, spherical cloud and a warmer or hot planar shock is a well-studied problem. The semina...

Visualizing Photometric Data As an assignment in my graduate galaxies course this spring, I was tasked with making a visualization of some sort of astronomical data or concept using an interactive ...

Background I am working on adding a dust model to the grid-based Cholla hydrodynamics code. Cholla currently uses its hydro capabilities to model gas, which is the primary fluid component of galaxi...