Speaker
Description
Stellar feedback shapes its environment from its local cloud to his own hosting galaxy. It combines several physical processes, such as the formation of magnetically-driven jets, irradiation and photoionization which restrain its growth and final mass. In this work, we include the MHD jet contribution self-consistently while adding radiative forces and photoionization. Our goal is to understand the role that different stellar feedback effects have on the outcome of the formation process while observing the physical mechanisms governing the disk and the low-density cavity.
To achieve this, we utilize the state-of-the-art code PLUTO, which solves the equations of non-ideal magnetohydrodynamics, with the addition of specialized modules for self-gravity, radiation transport and photoionization. These simulations start from the gravitational collapse of a molecular cloud of 100 $M_\odot$ and radius of 0.1 pc with different stellar feedback effects switched on, followed by the formation of an accretion disk and the magnetically-driven jets. The radiative feedback effects are driven according to the stellar evolution tracks by Hosokawa & Omukai (2009). These simulations were stopped when accretion becomes negligible or the disk is destroyed by radiative feedback.
Magnetically-driven outflows alone limit the stellar growth at early times, while radiation and photoionization become dominant at later times, when the star has reached the zero-age sequence. We observe that radiation forces restrain gravitational infall toward the disk, affect its gravito-centrifugal equilibrium, increase the outflow and completely halt accretion, resulting in an approximately 45 $M_\odot$ star after around 100 kyr of evolution. While photoionization shapes the bipolar outflow cavity, its addition did not significantly alter the final mass of the star. In contrast, in simulations without irradiation forces, accretion continues and the star reaches a mass of around 75 $M_\odot$.
