Characterizing Magnetic Properties of Young Protostars in Orion
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| Main Authors: | , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| author | Huang, Bo Girart, Josep M. Stephens, Ian W. Myers, Philip C. Zhang, Qizhou Cortés, Paulo Sánchez-Monge, Álvaro Fernández-López, Manuel Gouellec, Valentine J. M. Le Megeath, Tom Murillo, Nadia M. Carpenter, John M. Li, Zhi-Yun Liu, Junhao Looney, Leslie W. Sadavoy, Sarah Karnath, Nicole Kwon, Woojin |
| author_facet | Huang, Bo Girart, Josep M. Stephens, Ian W. Myers, Philip C. Zhang, Qizhou Cortés, Paulo Sánchez-Monge, Álvaro Fernández-López, Manuel Gouellec, Valentine J. M. Le Megeath, Tom Murillo, Nadia M. Carpenter, John M. Li, Zhi-Yun Liu, Junhao Looney, Leslie W. Sadavoy, Sarah Karnath, Nicole Kwon, Woojin |
| contents | The {\em B}-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 ${\rm μm}$ towards 61 protostars in the Orion molecular clouds with $\sim 1^{\prime\prime}$ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of $\sim 6^{\prime\prime}$ (2400~au) around the protostar. This allows to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis-Chandrasekhar-Fermi method. The underlying magnetic field strengths are approximately 2.0~mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations ($\lesssim1.0$~mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of $\gtrsim2.0$ mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios $\lesssim3.0$. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_14726 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Characterizing Magnetic Properties of Young Protostars in Orion Huang, Bo Girart, Josep M. Stephens, Ian W. Myers, Philip C. Zhang, Qizhou Cortés, Paulo Sánchez-Monge, Álvaro Fernández-López, Manuel Gouellec, Valentine J. M. Le Megeath, Tom Murillo, Nadia M. Carpenter, John M. Li, Zhi-Yun Liu, Junhao Looney, Leslie W. Sadavoy, Sarah Karnath, Nicole Kwon, Woojin Astrophysics of Galaxies The {\em B}-field Orion Protostellar Survey (BOPS) recently obtained polarimetric observations at 870 ${\rm μm}$ towards 61 protostars in the Orion molecular clouds with $\sim 1^{\prime\prime}$ spatial resolution using the Atacama Large Millimeter/submillimeter Array. From the BOPS sample, we selected the 26 protostars with extended polarized emission within a radius of $\sim 6^{\prime\prime}$ (2400~au) around the protostar. This allows to have sufficient statistical polarization data to infer the magnetic field strength. The magnetic field strength is derived using the Davis-Chandrasekhar-Fermi method. The underlying magnetic field strengths are approximately 2.0~mG for protostars with a standard hourglass magnetic field morphology, which is higher than the values derived for protostars with rotated hourglass, spiral, and complex magnetic field configurations ($\lesssim1.0$~mG). This suggests that the magnetic field plays a more significant role in envelopes exhibiting a standard hourglass field morphology, and a value of $\gtrsim2.0$ mG would be required to maintain such a structure at these scales. Furthermore, most protostars in the sample are slightly supercritical, with mass-to-flux ratios $\lesssim3.0$. In particular, the mass-to-flux ratios for all protostars with a standard hourglass magnetic field morphology are lower than 3.0. However, these ratios do not account for the contribution of the protostellar mass, which means they are likely significantly underestimated. |
| title | Characterizing Magnetic Properties of Young Protostars in Orion |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2503.14726 |