论文标题
对普通脉冲星的巨型脉冲的低频观察
Low-frequency observations of giant pulses from ordinary pulsars
论文作者
论文摘要
我们介绍了从5个无线电脉冲发生器（B0301+19，B0950+08，B1112+50，B1133+16和B1237+25）和来自B0809+74的异常强度脉冲发电率的研究结果。 All data used were obtained with Large Phased Array radio telescope of Pushchino Radio Astronomy Observatory at 111~MHz from 2012 to 2021. In addition to analysis of the rate of generation of bright pulses, we analyze the distribution of bright pulses in the phase of the pulsar period and search for clusters of bright pulses - several bright pulses emit in adjacent pulsar periods.发现Pulsars B0301+19，B1112+50，B1133+16和B1237+25显示出不同的产生速率和簇的产生。脉冲星B1112+50频率比其他研究的脉冲星的频率高。从该脉冲星中检测到包含四个单个脉冲的最长GRP簇。来自研究的脉冲星的GRP沿这些脉冲星平均脉冲的主要成分的纵向分布。该分布比非巨型脉冲的相分布窄1.5-2倍。发现平均GRP曲线的组成部分与平均非巨型曲线的组成部分之间的距离之间的距离在具有多组分平均值的PULSAR方面有很大不同。
We present results of the investigation of the giant radio pulses (GRPs) generation rate from 5 radio pulsars (B0301+19, B0950+08, B1112+50, B1133+16, and B1237+25) and anomalous intensity pulses generation rate from B0809+74. All data used were obtained with Large Phased Array radio telescope of Pushchino Radio Astronomy Observatory at 111~MHz from 2012 to 2021. In addition to analysis of the rate of generation of bright pulses, we analyze the distribution of bright pulses in the phase of the pulsar period and search for clusters of bright pulses - several bright pulses emit in adjacent pulsar periods. It is found that pulsars B0301+19, B1112+50, B1133+16, and B1237+25 demonstrate different generation rates and generation of clusters. Pulsar B1112+50 more often than others studied pulsars generates GRPs cluster. The longest cluster of GRPs containing four single pulses is detected from this pulsar. GRPs from studied pulsars are distributed along the longitudes of the main components of average pulses of these pulsars. This distribution is 1.5-2 times narrower than the phase distribution of non-giant pulses. It is found that the distance between the components of the average GRP profile and the distance between the components of the average non-giant profile differ substantially for pulsars with multicomponent average profiles.
