About the project
This project investigates thermonuclear (Type I) X-ray bursts on neutron stars through numerical simulations of flame spreading and ignition. You'll model burst dynamics, compare results with observations, and explore broader applications of the code to stellar flame propagation and exoplanetary atmospheres, developing strong computational and programming expertise.
Type I X-ray bursts, also known as thermonuclear bursts, occur on the surfaces of neutron stars in low-mass X-ray binary systems. Gas from a companion star accretes onto the neutron star, spreading across its surface to form a fresh layer of material. Under extreme gravity, this layer becomes compressed and heated until it reaches the critical temperature and density for thermonuclear ignition.
Nuclear fusion of hydrogen then begins, rapidly converting hydrogen into helium and then heavier elements. The resulting runaway burning releases enormous energy in X-rays—an outburst lasting seconds to minutes yet radiating more energy than the Sun emits in a week. These bursts provide a unique window into the extreme physical conditions on neutron star surfaces.
In this project, you'll develop and run simulations to model how the burning front spreads once ignition occurs. The results will be compared with observational data and theoretical predictions to improve our understanding of thermonuclear processes in compact stars. Beyond neutron stars, you'll explore how the computational methods developed here can be applied to other research areas, such as flame propagation in other stellar environments and atmospheric dynamics on exoplanets. You'll join the High-Energy Astrophysics Group and collaborate with leading researchers worldwide.
