Edward Buie II
I grew up in the Detroit metropolitan area with a love for the universe and everything in it. This love led me to attending Michigan State University where I studied Astronomy and Physics, eventually graduating as the second black astronomy major in their history (I found this funny with me being a second).
Currently, I'm an Astrophysics PhD candidate and NSF fellow in the School of Earth and Space Exploration (SESE) at Arizona State University (ASU) working with Evan Scannapieco. I'm also involved in tons of mentoring roles, have given science talks at K-12 schools, participate in the SESE Prison Education program, and other outreach efforts. Details on all of this (research and outreach) are provided in my CV below.
I enjoy reading, writing, and sitting on random benches reflecting on life and watching birds. I also love traveling, seeing different parts, and interacting with different people. I always come back from my travels with a story or two. Estoy también aprendicando Español (I'm also learning Spanish).
Last Updated: May 2021
I am interested in the diffuse halo of ionized gas surrounding galaxies known as the Circumgalactic Medium (CGM). To study this environment, I conduct 3D galaxy simulations with turbulence using the non-equilibrium chemistry & cooling code MAIHEM (please click on MAIHEM for more details of the code).
When we think of galaxies we often imagine a spinning disk with blue lights throughout and a bright center. But galaxies are more than meets the eye. Astronomers also observe large reservoirs 20 times the size of the host galaxy to exist. These halos of gas are often found to co-rotate with the host galaxy and are important in regulating the host galaxy's growth and evolution from its formation to its current stage. In this talk we will explore the scope of this halo, why it's nearly invisible to us, and see how simulated turbulence of a hot, magnetized plasma compares to real halos. These simulations are unique in that they also consider the non-equilibrium cooling and chemistry that occurs, giving me the ability to capture various observational features common to nearby halos surrounding star-forming galaxies.
The circumgalactic medium (CGM) of nearby star-forming galaxies shows clear indications of O VI absorption accompanied by little to no N V absorption. This unusual spectral signature, accompanied by absorption from lower ionization state species whose columns vary by orders of magnitude along different sight lines, indicates that the CGM must be viewed as a dynamic, multiphase medium, such as occurs in the presence of turbulence. Motivated by previous isotropic turbulent simulations, I conduct chemodynamical simulations of an anisotropic turbulent media in a Navarro-Frenk-White (NFW) density gradient, using the MAIHEM package. Simulations are ran until 3 Gyr and assume a metallicity of 30% solar with a redshift zero metagalatic UV background, and track ionizations, recombinations, and species-by-species radiative cooling for a wide range of elements. I also incorporate adaptive mesh refinement such that I am able to capture detailed features within the simulated CGM. This is done with the purpose of matching ionic column densities seen in low redshift observations around actively star-forming galaxies.