To explain the observed phenomenon of 11-year sunspot cycle with two peaks, we draw attention to the possible role of the turbulent magnetic pumping effects in the solar convection zone (SCZ) at the reconstructing of the toroidal magnetic field that generates the sunspots. Turbulent radial pumping of magnetic field has both kinetic (diamagnetism) and magnetic (vertical advection) contributions. We take into account five physical processes for the combined magnetic reconstructing in deep layers of the SCZ. They are the Ω effect near the tachocline, magnetic buoyancy of the smoothed field, macroscopic diamagnetism, rotational magnetic advection, and deep equatorward meridional circulation. It is the effect of advection with taking into account Sun's rotation that plays a key role in the proposed scenario of magnetic reconstructing. We found that reconstructing of deep toroidal field develops differently in the near-polar and equatorial domains of the SCZ. In the lower half of the near-polar domain, two downward pumping effects (diamagnetism and advection) act against magnetic buoyancy and, as a result, they neutralize magnetic buoyancy and thereby block the toroidal field near the tachocline. At the same time, in the deep layers of the equatorial domain, the rotational advection due to the latitudinal convection anisotropy changes its direction to the opposite (from downward to upward), thereby helping magnetic buoyancy. As a result, this upward magnetic pumping here contributes to the transport of the toroidal field to the solar surface. We call this transport as first upward magnetic advection surge. It ensures a transfer of the deep strong fields to the surface in the latitudes belt of sunspots. Meanwhile, a deep equatorward meridional flow transports the blocked near pole toroidal field in the tachocline from high latitudes to low ones where are favourable conditions for floating up of the magnetic field. Here this belated field is transported upward to the solar surface (the second upward magnetic advection surge). Ultimately, two time-delayed upward magnetic surges may cause on the surface in the “royal zone” the first and second peaks of the sunspots cycle.

为了解释观测到的具有两个峰值的 11 年太阳黑子周期现象，我们提请注意太阳对流区 (SCZ) 中湍流磁泵效应在重建产生太阳黑子的环形磁场中的可能作用。磁场的湍流径向泵送具有动能（抗磁性）和磁力（垂直平流）贡献。我们考虑了 SCZ 深层中组合磁重建的五个物理过程。它们是 Ω 效应靠近转速线、平滑场的磁浮力、宏观抗磁性、旋转磁平流和深赤道经向环流。考虑到太阳自转的平流效应在提出的磁重建方案中起着关键作用。我们发现深环场的重建在 SCZ 的近极区和赤道区发展不同。在近极域的下半部分，两种向下的泵送效应（抗磁性和平流）对抗磁浮力，因此，它们抵消了磁浮力，从而阻止了流线附近的环形场。同时，在赤道域的深层，由于纬度对流各向异性引起的旋转平流向相反方向改变（从下到上），从而帮助磁浮力。因此，这种向上的磁泵浦有助于将环形场传输到太阳表面。我们称这种传输为第一次向上的磁平流浪涌。它确保将深层强场转移到太阳黑子纬度带的地表。同时，深赤道经向流将被阻塞的近极环形场从高纬度输送到低纬度，这是磁场上浮的有利条件。在这里，这个迟来的磁场向上传输到太阳表面（第二次向上的磁平流浪涌）。最终，两次延迟的向上磁涌可能会在“皇家区”的地表上引起太阳黑子周期的第一个和第二个峰值。