The Origin of the Moon
The leading theory for the formation of the Moon suggests that a Mars-sized impactor struck the proto-Earth in a violent collision shortly after the formation of the solar system. The impact produces vapor, liquid, and solid debris. The debris either escapes the system, falls back to the Earth, or enters circumterrestrial orbits forming a “protolunar disk“. It is from this disk that the Moon is thought to have formed.
Planetary Scale Giant Impacts
We cannot simply go into a laboratory and smash two planets together. To study the evolution of a planetary scale giant impact, we must apply numerical simulations. These simulations are complicated; they evolve the collision of bodies subject to self-gravity, a non-trivial equation of state, and potentially even magnetic fields — all in 3D.
On a day-to-day basis, I crash planets into one another using the astrophysical magnetohydrodynamics framework Athena++. I specialize in investigating the role of magnetic fields in the Moon-forming giant impact. Magnetic fields are amplified as they are stretched and wound by turbulence generated by the planetary collision.
The Evolution of the Protolunar Disk
The birthplace of our Moon was a complex environment. Following the Moon-forming giant impact, a debris disk settled into orbit about the Earth. This protolunar disk was comprised of liquid and vapor lunar rock. It is likely that hot vapor in the protolunar disk interacted with a magnetic field that was amplified by the giant impact. In particular, we anticipate that the protolunar disk was unstable to the magnetorotational instability (MRI). The MRI yields vigorous magnetic turbulence and grows magnetic field strengths exponentially in time. It is possible that the protolunar disk could have exhibited magnetic field strengths comparable to those inside a medical magnetic resonance imaging machine! The MRI enables angular momentum transport. The protolunar disk is forced to spread and material is accreted onto the proto-Earth making Moon formation less efficient. Material accreted onto the proto-Earth must pass through the boundary layer, i.e., the transition layer between the proto-Earth and the innermost regions of the protolunar disk. This boundary layer may be unstable to supersonic shear instabilities that source spiral waves which propagate into the protolunar disk, hence mixing material between the molten Earth and debris disk. Understanding the dynamics of the protolunar disk is essential to understand when, where, and how our Moon formed. Furthermore, numerical simulations of the early evolution of protolunar disk may help reconcile the anomalous similarities between the isotopic ratios of lunar and terrestrial samples.
I am interested in the development and implementation of numerical algorithms for computational magnetohydrodynamics. I am a contributor to the Athena++ magnetohydrodynamics framework.
In collaboration with Dr. Joshua Dolence from Los Alamos National Lab, I have developed a super-time-stepping module in Athena++ for the integration of diffusive physics including Ohmic resistivity, ambipolar diffusion, viscosity, and thermal conduction. I have implemented the first and second-order temporally accurate RKL1 and RKL2 STS algorithms in the Athena++ framework.
In collaboration with Prof. Tomoyuki Hanawa from Chiba University, I have developed and implemented a fully conservative algorithm for self-gravitating hydrodynamics in the Athena++ framework . The scheme is capable of conserving total linear momentum and total energy to numerical round-off error for self-gravitating flows.