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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 5.

(Left) The map of the mass-to-flux ratio in G35. Black contours are the same as shown in Figure 3. The green triangles are the same as shown in Figure 1. (Right) Mean mass-to-flux ratio, ﹩\overline{\lambda }﹩, as a function of number density cut. The mean mass-to-flux ratio is calculated using the mean column density and magnetic field strength within the number density cut. When ﹩\overline{\lambda }﹩ is 1, the number density is 1.2 × 106 cm−3, which is shown as the magenta contour in the left panel.

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