I am interested in the role of neutrino and nuclear physics in core-collapse supernovae. I have extensive experience in the development and application of general relativistic numerical hydrodynamic supernova models, including detailed neutrino transport.
NEUTRINO FLAVOR MIXING IN CCSNE
It is well understood that core-collapse supernovae (CCSNe) result from the deaths of stars with masses M>8M⊙. Yet the explosion mechanism of CCSNe has remained one of the biggest open questions in astrophysics. With increasing computational power, simulations of the CCSN mechanism have increased in physical fidelity, now including realistic equations of state, general relativity, and neutrino transport, but also increased in computational precision with 3D simulations and increasing resolution. However, there is a fundamental piece of physics that remains missing from most supernova codes: neutrino flavor mixing. I am including the effects of neutrino flavor mixing in the FLASH supernova code. Neutrino flavor mixing may drastically change predictions of the supernova neutrino spectrum and thus the observable outcomes of CCSNe. I will produce the first simulations of CCSNe including neutrino oscillations and generate predictions of the impact of neutrino mixing on explodability, neutrino signal, and nucleosynthesis.
MULTIMESSENGER SIGNALS FROM CCSNE
Using the STIR model (described below), we now have the capability to run thousands of 1D supernova models that explode in a physically realistic way. We have used this to explore sensitivities of multimessenger signals - gravitational wave, neutrino, and electromagnetic - to the progenitor star and fundamental supernova physics. Our initial work has focused on relationships between observable signals and properties of the progenitor star, such as zero-age main sequence mass, core compactness at collapse, etc. In a follow up work, we have tested the sensitivities of the observable signals to the nuclear equation of state and explored correlations of the signals with fundamental nuclear physics quantities, such as the symmetry energy and effective nucleon mass.
MODELING SUPERNOVA TURBULENCE IN SPHERICAL SYMMETRY
Working with Professor Sean Couch, I have aided in the development of a new method for artificially driving core-collapse supernova explosions in 1D simulations, Supernova Turbulence in Reduced Dimensions (STIR). Turbulence is important for understanding the CCSN explosion mechanism, since turbulence may add a >20% correction to the total pressure behind the shock and thus aid in the explosion. We have implemented mixing length theory (MLT) and included a model of the turbulent pressure in the FLASH supernova code for spherically symmetric simulations. Including MLT and corrections for the turbulent pressure may result in successful explosions in spherical symmetry without altering the neutrino luminosities or interactions, as is commonly done to produce explosions in spherical symmetry. This better replicates the physical explosion mechanism and more reliably produces the thermodynamics and composition, which is vital for accurately predicting the nucleosynthesis that occurs in the supernova environment.
STERILE NEUTRINOS IN CCSNE
Sterile neutrinos are of interest in astrophysics both as dark matter candidates and for their potential impact on core-collapse supernovae. In supernovae, they may serve as an efficient mechanism to transport energy in the protoneutron star and are thus of interest in investigating supernova explosion energies. I have found that the early time explosion energy can be significantly enhanced when oscillations between a sterile neutrino and electron neutrino are included. The enhancement is sufficient to lead to a successful explosion even in a simulation that would not otherwise explode.
NUCLEAR EQUATION OF STATE
I have contributed to the development of the Notre Dame-Livermore Equation of State (NDL EoS), a nuclear equation of state intended for use in core-collapse supernova and neutron star simulations. A complete understanding of the equation of state of nuclear matter will provide us with a vital link between laboratory measurements and astrophysical phenomena. The NDL EoS meets all modern laboratory and astrophysical constraints and includes 3-body interactions and the possibility of a transition to quark gluon plasma. Ultimately, we plan to make this equation of state publicly available for use in core-collapse supernova and neutron star simulations.
EQUATION OF STATE DEPENDENCE OF THE OBSERVABLE PROPERTIES OF TURBULENCE-AIDED NEUTRINO-DRIVEN CORE-COLLAPSE SUPERNOVAE
In prep (2019)
M. L. Warren, B. Barker, T. Cooper, S. M. Couch, J. Ranter, M. Pajkos, and E. P. O'Connor.
MULTIMESSENGER SIGNALS FROM THE LANDSCAPE OF CORE-COLLAPSE SUPERNOVAE
In prep (2019)
M. L. Warren, S. M. Couch, and E. P. O'Connor.
SIMULATING TURBULENCE-AIDED NEUTRINO DRIVEN CORE-COLLAPSE SUPERNOVA EXPLOSIONS IN SPHERICAL SYMMETRY.
In prep (2019)
S. M. Couch, M. L. Warren, and E. P. O'Connor.
A DENSITY FUNCTIONAL EQUATION OF STATE FOR SUPERNOVA SIMULATIONS WITH 3-BODY FORCES AND QUARK GLUON PLASMA.
Phys.Rev.C, Submitted (2018)
J. P. Olson, M. L. Warren, M. Meixner, G. J. Mathews, N. Q. Lan, and H. E. Dalhed.