The Magnetic Field in the Milky Way Filamentary Bone G47
The Magnetic Field in the Milky Way Filamentary Bone G47
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DOI：
10.3847/2041-8213/ac4d8f
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发表时间：
2022-01
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通讯作者：
I. Stephens;P. Myers;C. Zucker;J. Jackson;B. Andersson;Rowan J. Smith;A. Soam;C. Battersby;P. Sanhueza;T. Hogge;H. Smith;G. Novak;S. Sadavoy;T. Pillai;Zhi-Yun Li;L. Looney;K. Sugitani;S. Coudé;Andrés E. Guzmán;A. Goodman;Takayoshi Kusune;F. Santos;L. Zuckerman;Frankie J. Encalada
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作者：
I. Stephens;P. Myers;C. Zucker;J. Jackson;B. Andersson;Rowan J. Smith;A. Soam;C. Battersby;P. Sanhueza;T. Hogge;H. Smith;G. Novak;S. Sadavoy;T. Pillai;Zhi-Yun Li;L. Looney;K. Sugitani;S. Coudé;Andrés E. Guzmán;A. Goodman;Takayoshi Kusune;F. Santos;L. Zuckerman;Frankie J. Encalada
星星的形成主要发生在磁场被认为是动力学重要的细丝中。最大和密集的丝状物追踪星系内的螺旋结构。在银河系中已经发现了超过12个这样的密集（约104 cm−3）和长（>10 pc）的细丝，它们通常被称为“骨头”。到目前为止，这些骨骼中没有一个的磁场被完整地解析和绘制出来。我们介绍索菲亚遗产项目FIELDMAPS，该项目已经开始使用HAWC+仪器以214 μm和18.″2分辨率绘制10个银河系骨骼。在这里，我们提出了第一个结果，从这个调查的1060 pc长骨G47。与一些对银河平面中致密细丝的研究相反，我们发现磁场通常不垂直于脊柱（即，骨头的中心线）。在活跃的星星形成的密集区域，场往往是垂直的，而在其他区域则更平行或随机。平均场既不平行也不垂直于银河平面或骨骼。沿脊柱沿着的磁场强度通常在20 μ G至100 μG之间变化。磁场往往足够强大，可以抑制沿着大部分骨骼的坍缩，但对于在星星形成中最活跃的区域，磁场抵抗引力坍缩的能力明显较弱。
Star formation primarily occurs in filaments where magnetic fields are expected to be dynamically important. The largest and densest filaments trace the spiral structure within galaxies. Over a dozen of these dense (∼104 cm−3) and long (>10 pc) filaments have been found within the Milky Way, and they are often referred to as “bones.” Until now, none of these bones has had its magnetic field resolved and mapped in its entirety. We introduce the SOFIA legacy project FIELDMAPS which has begun mapping ∼10 of these Milky Way bones using the HAWC+ instrument at 214 μm and 18.″2 resolution. Here we present a first result from this survey on the ∼60 pc long bone G47. Contrary to some studies of dense filaments in the Galactic plane, we find that the magnetic field is often not perpendicular to the spine (i.e., the center line of the bone). Fields tend to be perpendicular in the densest areas of active star formation and more parallel or random in other areas. The average field is neither parallel nor perpendicular to the Galactic plane or the bone. The magnetic field strengths along the spine typically vary from ∼20 to ∼100 μG. Magnetic fields tend to be strong enough to suppress collapse along much of the bone, but for areas that are most active in star formation, the fields are notably less able to resist gravitational collapse.