The 13 June 2010 event was chosen as an example to find spots on a CME-related shock where type II radio bursts were generated. We used the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) data to find the shock and calculate the emission measure distribution over the solar limb in order to obtain various plasma characteristics ahead of and behind the shock front. A region was found in the shock where the electron density jump \(X\) on the shock front, the Alfvén Mach number \(M_{a}\) and the shock velocity \(V_{sh}\) reach a maximum simultaneously. Moreover, the calculated value of \(X\) in this region was found to be closest to the value of \(X^{rb}\) based on type II radio burst data, \((X^{rb})=N_{2}/N_{1}=(f_{u}/f_{l})^{2}\), where \(N_{2}\) and \(N_{1}\) are the electron densities at the upstream and downstream shock regions, \(f_{u}\) and \(f_{l}\) are the radio emission frequencies at the upper and lower band of the dynamic spectrum, in the second harmonic region. Based on these findings, we hypothesized that it is this shock region that is the source of type II radio bursts (type II RB). This region moves at an angle of \(+20^{\circ }\) from the center of the circle approximating the shock, relative to the direction through the shock middle. The type II radio burst source velocity is shown to be close to the CME-related shock velocity. This can be regarded as indirect evidence of the shocks being the source of type II radio bursts. A dependence, \(N_{1}(R_{sh})\), has been obtained in the \(+20^{\circ }\) direction, where \(R_{sh}\) is the shock front location. This dependence is shown to differ noticeably from the coronal background electron densities obtained by Newkirk (Astrophys. J. 133, 983, 1961) and Saito et al. (Ann. Tokyo Astron. Obs. 12, 53, 1970) density models.

以2010年6月13日的事件为例，以查找与CME有关的电击中产生II型无线电脉冲串的点。我们使用了太阳动力学天文台（SDO）数据上的大气成像组件（AIA）来查找冲击，并计算了太阳肢体上的发射量分布，以便获得冲击前和冲击后的各种等离子体特征。在冲击中发现了一个区域，在该区域中，电子密度在冲击前沿跃迁\（X \），Alfvén马赫数\（M_ {a} \）和冲击速度\（V_ {sh} \）同时达到最大值。此外，发现该区域中\（X \）的计算值最接近\（X ^ {rb} \）的值基于II型无线电突发数据\（（X ^ {rb}）= N_ {2} / N_ {1} = {f_ {u} / f_ {l}）^ {2} \），其中\（N_ {2} \）和\（N_ {1} \）是在上游和下游激波区的电子密度，\（f_ {u} \）和\（f_ {l} \）是在在二次谐波区域中，动态频谱的上限和下限。基于这些发现，我们假设正是这一冲击区域成为了II型无线电脉冲爆发（II RB型）的来源。该区域以\（+ 20 ^ {\ circ} \）的角度移动从圆心近似于震动中心，相对于穿过震动中心的方向。II型无线电猝发源速度显示出接近CME相关的冲击速度。这可以看作是电击是II型无线电脉冲源的间接证据。已在\（+ 20 ^ {\ circ} \）方向上获得了依赖项\（N_ {1}（R_ {sh}）\），其中\（R_ {sh} \）是激振前部位置。这种依赖关系被示出为从由纽柯克（Astrophys。J.获得冠背景电子密度显着不同133，983，1961）和Saito等。（安。东京天文学。OB的。12，53，1970）密度的模型。