晚M多重系统LHS 1070三个分量中的谱型相关旋转制动和强磁通量
Spectral type dependent rotational braking and strong magnetic flux in three components of the late-M multiple system LHS 1070
摘要：
我们显示了附近晚M型多重系统LHS 1070的A、B和C分量的高分辨率光谱。成分A是一颗中等质量的恒星，B和C的质量都在褐矮星的临界值。从我们的光谱，我们测量旋转速度和平均磁场的所有三个组件单独。我们发现，在所有分量中，磁通量的数量级为几千高斯。两个晚M天体B和C的自转速度相似（vsini = 16 km/s），而早M天体A的自转速度只有前者的一半。这表明在晚M光谱类型下的净旋转制动减弱，并且缺乏缓慢旋转的晚M和L矮星是真实的。此外，我们发现，磁通量在B组件中是在组件C在类似的旋转速度的两倍强。这表明在完全对流的物体中，旋转制动与磁场强度不成比例，并且不同的场拓扑是低质量物体中弱制动的原因。
英文摘要：
We show individual high resolution spectra of components A, B, and C of the nearby late-M type multiple system LHS 1070. Component A is a mid-M star, B and C are known to have masses at the threshold to brown dwarfs. From our spectra we measure rotation velocities and the mean magnetic field for all three components individually. We find magnetic flux on the order of several kilo-Gauss in all components. The rotation velocities of the two late-M objects B and C are similar (vsini = 16km/s), the earlier A component is spinning only at about half that rate. This suggests weakening of net rotational braking at late-M spectral type, and that the lack of slowly rotating late-M and L dwarfs is real. Furthermore, we found that magnetic flux in the B component is about twice as strong as in component C at similar rotation rate. This indicates that rotational braking is not proportional to magnetic field strength in fully convective objects, and that a different field topology is the reason for the weak braking in low mass objects.
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