In this paper, we study the self-gravitating accretion disks by considering the toroidal component of magnetic field, [Formula: see text] and wind/outflow in the flow and also investigate the effect of two parameters, [Formula: see text] and [Formula: see text] corresponding to magnetic field on the latitudinal structure of such accretion disks. The cooling of the disk is parameterized simply as, [Formula: see text] (where [Formula: see text] is the internal energy and [Formula: see text] is the cooling timescale and [Formula: see text] is a free constant) and the heating rate is decomposed into two components, magnetic field and viscosity dissipations. We have shown that when the toroidal magnetic field becomes stronger, the heating process (viscous and resistivity) and the radiative cooling rate increase. Ohmic heating is much bigger than viscous heating and cooling, so we must consider the role of the magnetic field in the energy equation. Our numerical solutions show that the thickness of the disk decreases with strong toroidal component of magnetic field. The magnetic field leads to production of the outflow in the low latitude. So, by increasing the toroidal component of the magnetic field, the regions which belong to inflow decrease and the disk is cooled.

中文翻译：

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自引力原行星盘上环形磁场的数值研究

在本文中，我们通过考虑磁场的环形分量[公式：见文本]和流动中的风/流出来研究自引力吸积盘，并研究两个参数的影响，[公式：见文本]和[公式：见正文] 对应于此类吸积盘纬向结构上的磁场。磁盘的冷却被简单地参数化为，[公式：见文本]（其中 [公式：见文本] 是内部能量，[公式：见文本] 是冷却时间尺度，[公式：见文本] 是自由常数) 并且加热速率分解为两个分量，磁场和粘度耗散。我们已经表明，当环形磁场变强时，加热过程（粘性和电阻率）和辐射冷却速率会增加。欧姆加热比粘性加热和冷却要大得多，所以我们必须考虑磁场在能量方程中的作用。我们的数值解表明，圆盘的厚度随着磁场的强环形分量而减小。磁场导致在低纬度产生外流。因此，通过增加磁场的环形分量，属于流入的区域减少并且磁盘被冷却。