Speaker
Description
Magnetic fields play a crucial role in the process of star formation and the evolution of collapsing dense cores. However, direct measurements of magnetic field strength from observations remain challenging. The polarization–intensity gradient method is a new approach to estimate the magnetic field strength using polarization angle and intensity gradient, which can provide the map of position-dependent magnetic field strength estimates. In this project, we evaluate the applicability and robustness of this method when applied to realistic observational conditions. We perform synthetic Atacama Large Millimeter/submillimeter Array (ALMA) and James Clerk Maxwell Telescope (JCMT) observations based on RAMSES simulations, and apply the polarization–intensity gradient method to estimate the magnetic field strength. We then compare the derived field strengths with the intrinsic values from the simulation to quantify the associated uncertainties. Furthermore, we discuss the physical conditions and environments of dense cores under which the polarization–intensity gradient method provides reliable estimates. Our results aim to clarify the limitations and applicability of this method in interpreting observations of star-forming regions.
| Participate the oral/poster presentation award competition | Yes |
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