论文标题
恒星形成区域观测中的B场（Bistro）：Serpens Main的丝状结构中的磁场
B-fields in Star-Forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main
论文作者
论文摘要
我们将850 $ $ M $ m的极化观测值对詹姆斯·麦克斯韦望远镜（JCMT）上的POL-2极化计（JCMT）在星形地区观测（BISTRO）调查中作为B场的一部分获得的Pol-2极化计（JCMT）的一部分。这些观察结果探测了大约6000个AU量表上蛇蛇主分子云的磁场形态，该量子由核心和六个具有不同物理特性的细丝，例如密度和恒星形成活性。 Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less dense filamentary structures where $N_{H_2} < 0.93\times 10^{22}$ cm$^{-2}$ (magnetic fields perpendicular to density gradients), while being perpendicular to filaments (magnetic fields parallel to density gradients) in dense丝状结构具有恒星形成活性。此外，将HRO技术应用于密集的核心区域，我们发现磁场取向变化以再次垂直于密度梯度，在$ n_ {h_2} \ y 4.6 \ times 10^{22} $ cm $ $^{ - 2} $。这可以解释为核心形成的签名。在$ n_ {h_2} \大约16 \ times 10^{22} $ cm $^{ - 2} $磁场再次变为平行于密度梯度，这可以理解是由于磁场被插入材料拖入。此外，我们使用davis-chandrasekhar-fermi方法估算了细丝（$ b_ {pos} = 60-300〜μ $ g）的磁场强度，并讨论了细丝是否基于磁场和湍流能量密度的重力不稳定。
We present 850 $μ$m polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope (JCMT) as part of the B-fields In STar-forming Region Observations (BISTRO) survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less dense filamentary structures where $N_{H_2} < 0.93\times 10^{22}$ cm$^{-2}$ (magnetic fields perpendicular to density gradients), while being perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at $N_{H_2} \approx 4.6 \times 10^{22}$ cm$^{-2}$. This can be interpreted as a signature of core formation. At $N_{H_2} \approx 16 \times 10^{22}$ cm$^{-2}$ magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments ($B_{POS} = 60-300~μ$G)) using the Davis-Chandrasekhar-Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.
