Past studies have demonstrated that the interplanetary magnetic field (IMF) B_y component introduces asymmetries in the magnetosphere‐ionosphere (M‐I) system, though the exact timings involved are still unclear with two distinct mechanisms proposed. In this study, we statistically analyze convective flows from three regions of the M‐I system: the magnetospheric lobes, the plasma sheet, and the ionosphere. We perform superposed epoch analyses on the convective flows in response to reversals in the IMF B_y orientation, to determine the flow response timescales of these regions. We find that the lobes respond quickly and reconfigure to the new IMF B_y state within 30–40 min. The plasma sheet flows, however, do not show a clear response to the IMF B_y reversal, at least within 4 hr postreversal. The ionospheric data, measured by the Super Dual Auroral Radar Network (SuperDARN), match their counterpart magnetospheric flows, with clear and prompt responses at ≥75° magnetic latitude (MLAT) but a less pronounced response at 60–70 MLAT. We discuss the potential implication of these results on the mechanisms for introducing the IMF B_y component into the M‐I system.

中文翻译：

---

磁层-电离层系统中的对流：通过逆转对IMF的多任务调查

过去的研究表明，行星际磁场（IMF）B _y分量会在磁层-电离层（M-1）系统中引入不对称性，尽管所提出的确切时机尚不清楚，但提出了两种不同的机制。在这项研究中，我们对M-1系统三个区域的对流进行了统计分析：磁层瓣，等离子层和电离层。我们响应IMF B _y方向的逆转，对流进行叠加的历时分析，以确定这些区域的流动响应时间尺度。我们发现，波瓣响应迅速，并重新配置为新的IMF B _y状态在30-40分钟内。但是，血浆片流至少在反转后4小时内没有显示出对IMF B _y反转的明确响应。由超级双极光雷达网络（SuperDARN）测量的电离层数据与对应的电离层流相匹配，在≥75 °磁纬度（MLAT）时具有清晰而迅速的响应，但在60-70 MLAT时响应较不明显。我们讨论了这些结果对将IMF B _y组件引入M-I系统的机制的潜在影响。