# Massive Outflows Driven by Magnetic Effects in Star Forming Clouds with High Mass Accretion Rates

## TL;DR

This study uses 3D magnetohydrodynamics simulations to explore how magnetic effects influence massive outflows in star-forming clouds with high mass accretion rates, revealing the importance of magnetic strength.

## Contribution

It demonstrates that strong magnetic fields are essential for launching massive outflows in high accretion rate environments, extending understanding of star formation mechanisms.

## Key findings

- Massive outflows are driven by magnetic effects in high accretion rate clouds.
- Strong magnetic energy leads to comparable mass ejection and accretion rates.
- Simulation results align with observed properties of massive star outflows.

## Abstract

The relation between the mass accretion rate onto the circumstellar disc and the rate of mass ejection by magnetically driven winds is investigated using three-dimensional magnetohydrodynamics simulations. Using a spherical cloud core with a varying ratio of thermal to gravitational energy, which determines the mass accretion rate onto the disc, to define the initial conditions, the outflow propagation for approximately 10^4 yr after protostar formation is then calculated for several cloud cores. The mass ejection rate and accretion rate are comparable only when the magnetic energy of the initial cloud core is comparable to the gravitational energy. Consequently, in strongly magnetised clouds a higher mass accretion rate naturally produces both massive protostars and massive outflows. The simulated outflow mass, momentum, kinetic energy and momentum flux agree well with observations, indicating that massive stars form through the same mechanism as low-mass stars but require a significantly strong magnetic field to launch massive outflows.