Non-equilibrium Ionization Chemistry
Collaborators: Professor Brian O’Shea, Professor J. Michael Shull, Dr. Matthew Turk, Dr. Daniel Reynolds, Dr. Britton Smith
One component currently absent from the extensive publicly available feature list of Enzo is a non-equilibrium treatment of the ionization states of metal species. At present, Enzo users seeking to study the ionization structure of gas within their simulations do so by post-processing their data under the assumption that metals species are always in collisional ionization equilibrium. However, for certain temperature and density regimes, the ionization and recombination timescales for such species become comparable to a Hubble time, leading to the possibility that the gas could be significantly out of equilibrium. This presents a clear need for a non-equilibrium ionization calculations.
Motivated by this need, one aspect of my current work is focused on adding this capability to Enzo. Once complete, it will be possible to track any number of atomic species and their ionization states during simulation run time. This capability is being built using the collisional ionization and recombination rates from the CHIANTI atomic database coupled with the ion-by-ion cooling efficiencies computed by Gnat & Ferland (2012) and, more recently, by Oppenheimer & Schaye (2013) to ensure that the radiative cooling is still being handled correctly. I am also working to incorporate the ion-by-ion photoionization and photoheating rates for a uniform ultra-violet radiation background tabulated by Oppenheimer & Schaye (2013).
To ensure that non-equilibrium ionization chemistry is added to Enzo in a computationally efficient way, I have been collaborating with Dr. Matthew Turk (Columbia University; experienced with non-equilibrium primordial chemistry) and Dr. Daniel Reynolds (Southern Methodist University; experienced with numerical methods and implementing radiative transfer solvers in Enzo). Both individuals are long-time contributors to the development of Enzo. We have been working to develop a brand new open source software package for building and solve complex chemical networks called Dengo. Using the code produced by Dengo, I am working to develop a new module in Enzo that simultaneously computes the ion fractions, heating/cooling rates, and photoionization/heating by a uniform UV background. Once this functionality has been completed and thoroughly tested, I plan to add it to the public Enzo repository.
With the aid of this new module, some scientific questions of personal interest are: What is the true ionization structure of the warm-hot intergalactic medium and circumgalactic medium? What fraction of baryons in the universe reside in this gas phase? How can simulations of these environments be used to interpret current observations and predict the finding of future ones?
The above plot shows the results of a cosmological simulation when you calculate the ionization state of the gas by post-processing the density and temperature and assume the gas is in collisional ionization equilibrium (CIE; left panels) versus performing a direct non-equilibrium calculation during simulation runtime (NEQ; right panels).
If you have questions about the state of this work, please send your queries to email@example.com.
Dust Destruction in Supernova Remnants
Collaborators: Professor J. Michael Shull and Dr. Britton Smith
Part of my past research efforts were focused on the interaction between the reverse shock of supernova remnants and the freshly formed supernova ejecta. The ejecta contained within a supernova remnant consists of gas that has been processed by the core of the progenitor star. Within the stellar core, light elements (hydrogen and helium) have been fused into heavier and heavier elements (e.g. carbon, oxygen, silicon, iron) and at the end of the stellar life cycle these heavy elements (commonly referred to simply as “metals”) are released back into the surrounding environment during the supernova explosion. This metal-enriched ejecta gas is ripe for dust grain formation as it is capable of rapidly cooling to low temperatures and collapsing to high densities – requirements for dust nucleation. It has been theorized that the amount of dust that could be formed by supernovae might explain the high dust masses that have been observed in the early universe.
However, as the ejecta expands outward from the point of the supernova explosion, it impacts the reverse shock of the supernova remnant. The reverse shock is a pressure wave that propagates inward from the expanding shell created by the supernova explosion. When the reverse shock impinges upon the ejecta gas, it further compresses the gas while simultaneously shock heating it to extreme temperatures. Such a scenario could result in the destruction of the aforementioned dust grains.
My work involved studying the ejecta-shock interaction via computational hydrodynamic simulations run on supercomputers at national facilities using the community astrophysics code, Enzo. In these simulations, a dust-rich ejecta cloud is impacted by a planar shockwave with properties expected for a supernova remnant reverse shock. The goal for this work was to quantify the survival rate of dust grains embedded in the ejecta cloud. Understanding the amount of dust destruction that could occur during this interaction would aid in answering the question of dust production at early times in the history of the universe.
The results of this work suggested that, in the most energetic scenarios, some dust grains species would be completely destroyed while even the more robust species had survival rates less than fifty percent. Even in less extreme cases, there was a significant degree of dust destruction, leading to the conclusion that supernovae are unlikely to be the sole source of dust in the early universe.
The above image is a volume-rendered snapshot of the gas density from one of my cloud-crushing simulations. It was created using the python-based data analysis package yt.
If you have questions about this project or about the work that has been completed thus far, please send your queries to firstname.lastname@example.org.