Astrophysical media are turbulent and therefore reconnection should be treated in the presence of pre-existing turbulence. We consider the model of fast magnetic reconnection in Lazarian and Vishniac (Astrophys J 517:700-718, 1999) which predicts that the rate of reconnection is controlled by the intensity and the injection scale of turbulent motions. We provide new evidence of successful testing of the model and argue that the model presents a generic set up for astrophysical reconnection events. We study particle acceleration that takes place in volumes of driven turbulence as well turbulent volumes in the presence of large scale reconnection. We show that in the latter case the acceleration is of the first order Fermi type thus supporting the model of acceleration proposed in Gouveia dal Pino and Lazarian .
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机译：天体物理介质是湍流的，因此应在预先存在的湍流存在下进行重新连接。我们考虑Lazarian和Vishniac的快速磁重新连接模型（Astrophys J 517：700-718,1999），其预测重新连接的速率由湍流运动的强度和喷射量表控制。我们提供了对模型的成功测试的新证据，并认为该模型提出了一种用于天体物理重新连接事件的通用设置。我们在存在大规模重新连接的情况下，研究以驱动的湍流的体积发生在驱动湍流中进行的颗粒加速度。我们表明，在后一种情况下，加速度是一阶Fermi类型，从而支持Gouveia Dal Pino和Lazarian中提出的加速模型。
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