Magnetic fields play a crucial role in star formation processes across all scales. Accurately determining their properties—including strength and spatial orientation—is essential for understanding the physical characteristics of molecular clouds, star-forming cores, and protoplanetary disks.
Soler and Hennebelle (2017) provided a general framework for understanding the relationship between the density gradient and the relative orientation of the magnetic field in turbulent molecular clouds. Their studies suggest that this relationship is either preferentially parallel or perpendicular, depending on the observed column density range.
This study investigates the connection between the magnetic field and the structural properties of molecular clouds, using Heiles Cloud 1 (LDN 1251) and Heiles Cloud 2 (HCL 2) as case studies. The analysis focuses on how the magnetic field influences the morphology and dynamics of these clouds, particularly in denser regions where it may regulate the formation of gas and dust structures.
The primary method employed is the Histogram of Relative Orientations (HRO) analysis, which quantifies the relative angles between polarization vectors and the column density gradient. This technique provides a statistical assessment of the alignment between the magnetic field and gas structures, offering insights into whether the magnetic field primarily guides gas dynamics in low-density regions or acts to resist gravitational collapse in higher-density areas.
The findings contribute to a deeper understanding of the role of magnetic fields in shaping the structure of molecular clouds, including filament formation and the evolution of star-forming cores. A comparative analysis of the two case studies highlights key similarities and differences in the observed regions.