Magnetic field structure in a high-mass outflow/disk system

TL;DR

This study investigates the magnetic field structure in a high-mass star-forming region using polarized CO(3-2) and submillimeter continuum observations, revealing alignment with outflows and a possible increase in magnetic strength from envelope to core.

Contribution

First polarization measurements of CO(3-2) in a high-mass star-forming region, providing new insights into magnetic field alignment and strength variations.

Findings

Magnetic fields are aligned with outflows from small to large scales.

Turbulent energy exceeds magnetic energy in the region.

Magnetic field strength appears to increase from envelope to core.

Abstract

To characterize the magnetic field structure of the outflow and core region within a prototypical high-mass star-forming region, we analyzed polarized CO(3-2) - for the first time observed with the Submillimeter Array -- as well as 880mum submm continuum emission from the high-mass outflow/disk system IRAS18089-1732. Both emission features with polarization degrees at a few percent level indicate that the magnetic field structure is largely aligned with the outflow/jet orientation from the small core scales to the larger outflow scales. Although quantitative estimates are crude, the analysis indicates that turbulent energy dominates over magnetic energy. The data also suggest a magnetic field strength increase from the lower-density envelope to the higher-density core.