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Magnetic Fields in Massive Star-forming Regions (MagMaR). VI. Magnetic Field Dragging in the Filamentary High-mass Star-forming Region G35.20–0.74N Due to Gravity

  • Authors: Jihye Hwang, Patricio Sanhueza, Josep Miquel Girart, Ian W. Stephens, Maria T. Beltrán, Chi Yan Law, Qizhou Zhang, Junhao Liu, Paulo Cortés, Fernando A. Olguin, Patrick M. Koch, Fumitaka Nakamura, Piyali Saha, Jia-Wei Wang, Fengwei Xu, Henrik Beuther, Kaho Morii, Manuel Fernández López, Wenyu Jiao, Kee-Tae Kim, Shanghuo Li, Luis A. Zapata, Jongsoo Kim, Spandan Choudhury, Yu Cheng, Kate Pattle, Chakali Eswaraiah, Panigrahy Sandhyarani, L. K. Dewangan, O. R. Jadhav

Jihye Hwang et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 9.

The schematic view of G35. The large-elongated structure and yellow circles indicate the filament and dense cores in G35. The gray lines show magnetic field lines. Magnetic field lines are initially perpendicular to the major axis of the filament (Left). As the density increases, the gas moves and drags the magnetic field lines (Right). Cores are also moved along the filament, making a short separation. The black arrow represents the time evolution of the filament. Colored arrows show gas movement based on velocity gradients.

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