Speaker
Description
Intensity Interferometry (II) has demonstrated significant potential for high-angular-resolution measurements of stellar objects, as the recent one with VERITAS, which resolved non-spherical structure. However, these studies assume simplified stellar models with static surface brightness, which limits our ability to investigate the effects of realistic stellar structure and shape.
There is an exciting possibility for modeling binary star systems using Smoothed Particle Hydrodynamics (SPH), which provides a physically motivated description of the stellar density and brightness distributions. In this talk, I will present an example of a well-known close binary system, previously investigated under the assumption of static distribution of brightness. By incorporating SPH simulations to measure visibility on the UV plane, we can generate more realistic II observables and find their impact on image reconstruction and parameter estimation. These simulations provide an important step toward interpreting future II observations of complex stellar systems with greater physical realism.
