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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Strong magnetic field generated by the extreme oxygen-rich red supergiant VY Canis Majoris
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Strong magnetic field generated by the extreme oxygen-rich red supergiant VY Canis Majoris

机译：由极端氧气丰富的红色超巨型VY Canis Mairis产生的强磁场

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Evolved stars experience high mass-loss rates forming thick circumstellar envelopes (CSEs). The circumstellar material is made of the result of stellar nucleosynthesis and, as such, plays a crucial role in the chemical evolution of galaxies and the universe. Since asymmetric geometries of CSEs are common, and with very complex structures for some cases, radiative pressure from the stars can explain only a small portion of the mass-loss processes; thus the essential driving mechanism is still unknown, particularly for high-mass stars. Here we report on magnetic field measurements associated with the well-known extreme red supergiant (RSG) VY Canis Majoris (VY CMa). We measured the linear polarization and the Zeeman splitting of the SiO v = 0, J = 1-0 transition using a sensitive radio interferometer. The measured magnetic field strengths are surprisingly high; their upper limits range between 150 and 650 G within 530 au (similar to 80 R-*) of the star. The lower limit of the field strength is expected to be at least similar to 10 G based on the high degree of linear polarization. Since the field strengths are very high, the magnetic field must be a key element in understanding the stellar evolution of VY CMa, as well as the dynamical and chemical evolution of the complex CSE of the star. M-type RSGs, with large stellar surface, were thought to be very slow rotators. This would seem to make a dynamo in operation difficult, and would also dilute any fossil magnetic field. At least for VY CMa, we expect that powerful dynamo processes must still be active to generate the intense magnetic field.
机译：进化的恒星体验高质量损失率，形成厚的周围的信封（CSE）。外观材料是由恒星核酸的结果制成，因此，在星系和宇宙的化学演变中起着至关重要的作用。由于CSE的不对称几何形状是常见的，并且对于某些情况非常复杂的结构，来自恒星的辐射压力可以仅解释一小部分质量损耗过程;因此，基本的驱动机制仍然是未知的，特别是对于高质量恒星。在这里，我们报告与众所周知的极端红色超巨头（RSG）VY Canis Formis（VY CMA）相关的磁场测量。我们使用敏感的无线电干涉仪测量了SiO V = 0，J = 1-0转换的线性极化和塞曼分离。测量的磁场强度令人惊讶地高;它们的上限范围在530和650克之间的530和650克之间（类似于星形的80 R-*）。基于高度的线性极化，预计场强的下限预计至少与10g相似。由于场强度非常高，因此磁场必须是了解VY CMA的恒星演化的关键因素，以及恒星的复杂CSE的动态和化学演化。 M型RSGS，具有大型恒星表面，被认为是非常缓慢的旋转器。这似乎在运行中使动力难以稀释，并且还将淡化任何化石磁场。至少对于VY CMA，我们预计强大的发电机进程仍然必须是活动的，以产生强烈的磁场。

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