Abstract

Contributed Talk - Splinter MassiveStars   (MW-1050)

Impact of magnetically-driven jets and radiative feedback on the formation of massive stars

Joshua Barquero Alvarado
André Oliva, Rolf Kuiper

Feedback from massive stars is a significant component in the evolution of giant molecular clouds. It combines several physical processes like the formation of magnetically-driven jets, irradiation and photoionization which are capable to restrain its growth and final mass. In this work, we include the MHD jet contribution self-consistently while including radiative forces and photoionization. Our objective is to understand the function that these 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. We ran a set of simulations considering different stellar feedback effects switched on. All simulations start from the gravitational collapse of a molecular cloud of 100 M⊙, followed by the formation of an accretion disk and the self- consistent launch of magnetically-driven outflows. The stellar feedback effects are driven according to the stellar evolution tracks by Hosokawa & Omukai (2009). We stopped our simulations when accretion becomes negligible or the accretion disk is pushed away from the computational domain. At early times, magnetically-driven outflows limit the stellar growth, while radiation and photoionization dominate at later times, after the star has reached the zero-age sequence. Radiation forces restrain the gravitational infall toward the disk, affect its gravito-centrifugal equilibrium, increase the outflow and completely halt accretion, resulting in a approximately 45 M⊙ star after 100 kyr of evolution. While photoionization shapes the bipolar outflow cavity, its addition did not significantly alter the final mass of the star but increases its accretion time by 20 kyr. In contrast, in simulations that do not include irradiation forces, accretion continues until later on and the star reaches a mass of 75 M⊙.