| Project Detail |
The merging of binary neutron stars produces an explosive kilonova transient, recently confirmed by the first ever detection of a kilonova, AT2017gfo, coincident with a gravitational wave signal, GW170817. The wealth of observations provided by AT2017gfo offers the opportunity to probe the fundamental physics of binary neutron star mergers, including the incompletely known Equation of State of dense nuclear matter and rapid neutron capture nucleosynthesis (the r-process), which produces half of all elements heavier than iron in the Universe. With the detection of AT2017gfo and the new gravitational wave observing run of LIGO, VIRGO and KAGRA (O4) the demand for kilonova simulations has never been so great.
The aim of this research is to produce sophisticated, three-dimensional kilonova radiative transfer simulations from binary neutron star merger ejecta with detailed r-process calculations, allowing simulations to be directly compared to observations. I am uniquely placed to combine these complex simulations to self-consistently model kilonovae, enabling powerful constraints to be placed on the underlying physics through interpreting kilonova observations. I will carry out the first three-dimensional kilonova parameter space study based on realistic hydrodynamical neutron star merger simulations with a range of neutron star masses and Equations of State. The simulations will predict spectra using a state of the art line-by-line opacity treatment for millions of line transitions of r-process elements, which allows spectral features to be directly associated with the ions responsible for forming the features.
This multi-disciplinary approach will constrain and improve hydrodynamical neutron star merger modelling, kilonova radiative transfer simulations, the high density Equation of State and r-process nucleosynthesis, which are critical to move our knowledge of kilonovae and their role in producing heavy elements in the Universe beyond the state of the art. |
