论文标题
Beta Lyrae System II中磁化空间结构的形成。可见光谱中磁控制结构的反射
Formation of magnetized spatial structures in the Beta Lyrae system II. Reflection of magnetically controlled structures in the visible spectrum
论文作者
论文摘要
本文提出了在Beta Lyre系统中传质中形成的磁化积聚结构的图片。结果表明，供体和增益之间气态流的结构是由于供体磁场的空间构型。其偶极轴与连接组件中心的线大大偏离，并倾向于二元系统的轨道平面。磁性偶极子的中心从供体中心向上移动。供体磁极周围的表面靠近增益器，是供体表面额外物质损失的区域。通过快速反转该磁盘，尤其是在次级正交阶段的快速反转来增强磁化等离子体与积聚盘的有效碰撞，其中观察到高温培养基和形成的积聚流的系统。主要在供体磁场的相位变异性与各种复合线的动态和能量特性的相应变异性之间的明显相关性中证明了这一概念。这是指在H $α$，HEI $λ$ 7065的气态结构中形成的发射速度曲线的行为，或它们等效宽度和强度的可变性，以及捐助者气氛的常规吸收线的变化。对于H $α$发射线中的绝对通量的相位变异性以及H $α$区域中连续体的快速变化是正确的，这是某些参数，这反映了供体磁场的相位变异性。这种方法使确定形成物质流出的供体表面上磁性区域位置的相位边界。
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.
