The meteoroid stream of long-period comet C/1861 G1 (Thatcher) is modeled in course to reveal the details of its structure. Specifically, we modeled several parts of the comet's theoretical stream, which were characterized by various values of evolutionary times and various strengths of the Poynting-Robertson effect. The dynamical behaviour of 10 ​000 test particles in each model from the time of their ejection up to the present was followed via a numerical integration of their orbits. The characteristics of the particles that moved on orbits approaching the Earth's orbit were used to predict a shower. Primarily, we wanted to find whether C/1861 G1 is the parent body of other meteor showers than the April Lyrids. However, we confirm that the orbit of this parent and its meteoroid stream is relatively stable during a long time and the meteoroids can collide with our planet only in the pre-perihelion orbital arc corresponding to the April Lyrids, No. 6, code LYR. Our modeling did not show any clustering of the meteoroids in the stream due to the gravitational perturbations that could explain the observed outbursts. The observed semi-major axes are, in general, smaller than those of the modeled particles and the parent comet because of a selection effect. Namely, the meteoroids in orbits with smaller semi-major axes pass the Earth's orbit more frequently. They are then observed and recorded in the data more often than the meteors with the larger axes.

长周期彗星C / 1861 G1（撒切尔）的流星流经过建模，可以揭示其结构的细节。具体来说，我们对彗星的理论流的几个部分进行了建模，这些部分的特征是演化时间的各种值和Poynting-Robertson效应的各种强度。从它们的射出之时到现在，每个模型中有10 000个测试粒子的动力学行为是通过对其轨道的数值积分来跟踪的。在接近地球轨道的轨道上移动的粒子的特征被用来预测一次阵雨。首先，我们想确定C / 1861 G1是否是4月天琴座以外的其他流星雨的母体。然而，我们确认该母体及其流星体流的轨道在很长一段时间内相对稳定，流星体只能在对应于4月Lyrids，编号6 LYR的近日点前轨道弧中与我们的行星碰撞。由于重力扰动可以解释观测到的爆发，因此我们的模型未显示流中的任何类星体聚集。通常，由于选择效应，观察到的半长轴小于建模粒子和母彗星的半长轴。即，具有较小半长轴的轨道中的流星体更频繁地通过地球的轨道。与具有较大轴的流星相比，它们被观测和记录在数据中的频率更高。代码LYR。由于重力扰动可以解释观测到的爆发，因此我们的模型未显示流中的任何类星体聚集。通常，由于选择效应，观察到的半长轴小于建模粒子和母彗星的半长轴。即，具有较小半长轴的轨道中的流星体更频繁地通过地球的轨道。与具有较大轴的流星相比，它们被观测和记录在数据中的频率更高。代码LYR。由于重力扰动可以解释观测到的爆发，因此我们的模型未显示流中的任何类星体聚集。通常，由于选择效应，观察到的半长轴小于建模粒子和母彗星的半长轴。即，具有较小半长轴的轨道中的流星体更频繁地通过地球的轨道。与具有较大轴的流星相比，它们被观测和记录在数据中的频率更高。半长轴较小的轨道上的流星体更频繁地通过地球的轨道。与具有较大轴的流星相比，它们被观测和记录在数据中的频率更高。半长轴较小的轨道上的流星体更频繁地通过地球的轨道。与具有较大轴的流星相比，它们被观测和记录在数据中的频率更高。