This article proposes a picture of magnetized accretion structures formed during the mass transfer in the Beta Lyrae system. It is shown that the structure of the gaseous flows between the donor and the gainer is due to the spatial configuration of the donor magnetic field. Its dipole axis is deviated substantially from the line joining the centers of the components and is inclined to the orbital plane of the binary system; the center of the magnetic dipole is displaced from the donor center toward the gainer. The surface around the donor magnetic pole, which is close to the gainer, is a region of an additional matter loss from the donor surface. The effective collision of the magnetized plasma with the accretion disk is enhanced by the fast counter-rotation of this disk, especially in the secondary quadrature phases, in which the high-temperature medium and the system of formed accretion flows are observed. This concept is demonstrated, primarily, in the obvious correlations between the phase variability of the donor magnetic field and the corresponding variability of the dynamic and energy characteristics of the various complex lines. This refers to the behavior of the radial velocity curves of the emission-absorption lines formed in the gaseous structures of type H$α$, HeI $λ$ 7065, or the variability of their equivalent width and intensity, and the variability of conventional absorption lines of the donor atmosphere. This is true for the phase variability of the absolute flux in the H$α$ emission line and the fast varying of the continuum in the H$α$ region as certain parameters, which reflect the phase variability of the donor magnetic field. This approach made it possible to determine the phase boundaries of the location of the magnetic polar region on the donor surface above which the matter outflows are formed.
Formation of magnetized spatial structures in the Beta Lyrae system III. Reflection of magnetically controlled matter in circumbinary structures in helium lines, in particular arising from metastable levels
Is WISEP J060738.65+242953.4 Really A Magnetically Active, Pole-on L Dwarf?
超冷矮星（UCD）的旋转和明显的磁场活动的相互作用对于收集这些物体内发电机运行的线索至关重要。多个磁化的UCD具有KG强度的磁场。最近有报道称，L 8矮星WISEP J060738.65+242953.4是一个无线电发射的UCD，由于其缺乏光度变化和狭窄的谱线，很可能是在极上观察到的。然而，在阿雷西博天文台进行的后续射电观测，以及对先前公布的细节的仔细分析表明，射电和光谱数据的科学和统计意义被夸大了。如果UCD是沿其对齐的自旋/磁轴观察到的，则观察到的H $α$活动的缺失可能会对UCD磁性的极光模型提出挑战，尽管短期或长期的周期性磁性活动可以解释这种行为。蒙特卡罗模拟表明，该源的自转速度可能为vsin i=6-12 km s $^{-1}$，表明它的倾角和自转速度都很正常，并且它的角动量的演化与100万年前观测到的棕矮星一致。最快和最慢旋转棕矮星的发现和验证对这些天体的角动量演化和磁活动历史提出了有价值的约束。
ROME (Radio Observations of Magnetized Exoplanets). II. HD 189733 Does Not Accrete Significant Material from its Exoplanet like a T Tauri Star from A Disk
有人断言，HD 189733系统中的主星稳定地吸积来自其“热彗星”伴星的蒸发的外大气层气体，就像金牛座T星从圆盘吸积一样。我们进行统计和周期图分析的测光时间序列的主要，所获得的自动光电望远镜（APT），恒星的微变和振荡（MOST），和明智的天文台，调查这一索赔的目的是揭示存在的吸积冲击或光球吸积热点被发现在金牛座T系统，如AA头。我们重新分析现有的无线电，光学，紫外线和X射线数据的框架内的吸积金牛座T系统，以确定物理量，如等离子体密度和温度，吸积率和耀斑长度。我们发现，吸积率为$\dot{M}\sim10^{9}$至10 $^{11}$ g s $^{-1}$，恒星更类似于一个系统，间歇性地吸收气体从掠日彗星爆发比经典的金牛座T系统，吸积率至少大两个数量级。如果这种吸积存在，它将导致在所有波长上都无法检测到的低活动。或者，迄今为止观察到的所有发射特性都与来自磁活跃恒星的恒星活动一致。
