Photoevaporation is one of the disk dispersal mechanisms. The gas is heated by the radiation from the central star. The gas is typically heated up to several hundreds K on the disk surface. The heated gas escapes from the gravitational potential by the central star.

Photoevaporation simulations have been done in several ways. Previous works show that it is necessary to solve radiative trasfer and hydrodynamics in a combined way.

I performed a series of photoevaporation simulations varying stellar mass, luminosity and dust-to-gas ratio.

disk evolution

Recent researches suggest that accretion, disk wind and photoevaporation are the main disk dispersal processes. It is computationally expensive to run 2D long-term disk evolution simulations with several physical processes. I developed simulation codes which calculate evolution of disk surface density.

molecular line analysis

I analysed ALMA data.