使用GMRT发现八个“主序列射电脉冲发射源”：热磁星相干射电发射开始的线索
Discovery of eight 'Main-sequence Radio Pulse emitters' using the GMRT: clues to the onset of coherent radio emission in hot magnetic stars
摘要：
主序射电脉冲发射源（英语：Main-sequence radio pulse-emitters，缩写：MRP）是由电子回旋脉泽发射（英语：electron cyclotron maser emission，缩写：ECME）产生的周期性射电脉冲。尽管这些恒星可以自然地提供触发ECME的合适条件，但在二十多年的时间里，迄今为止只有七颗这样的恒星被报道。在本文中，我们报告了8个以上的MRP的发现，从而增加了一倍以上的样本量，这样的对象。这些发现是我们在2015-2021年期间使用巨型米波射电望远镜进行sub-GHz观测计划的结果。将这些恒星添加到先前已知的MRPs中，我们推断至少有32%的磁热恒星表现出这种现象，从而表明ECME的观测并不罕见。大得多的MRP样本使我们能够第一次进行统计分析，比较它们的物理特性。我们提出了一个经验关系，可用于预测是否磁热星可能产生ECME。我们的初步分析表明，在该现象的效率中起主要作用的物理参数是最大表面磁场强度和表面温度。此外，我们提出了强有力的证据，等离子体密度分布的ECME脉冲轮廓的影响。这类结果进一步激励搜索MRPs作为一个强大的表征所观察到的ECME属性和恒星物理参数之间的关系，只能实现一个大样本。
英文摘要：
'Main-sequence radio pulse-emitters' (MRPs) are magnetic early-type stars from which periodic radio pulses, produced via electron cyclotron maser emission (ECME), are observed. Despite the fact that these stars can naturally offer suitable conditions for triggering ECME, only seven such stars have been reported so far within a span of more than two decades. In this paper, we report the discovery of eight more MRPs, thus more than doubling the sample size of such objects. These discoveries are the result of our sub-GHz observation program using the Giant Metrewave Radio Telescope over the years 2015-2021. Adding these stars to the previously known MRPs, we infer that at least 32 percent of the magnetic hot stars exhibit this phenomenon, thus suggesting that observation of ECME is not a rare phenomenon. The significantly larger sample of MRPs allows us for the first time to perform a statistical analysis comparing their physical properties. We present an empirical relation that can be used to predict whether a magnetic hot star is likely to produce ECME. Our preliminary analysis suggests that the physical parameters that play the primary role in the efficiency of the phenomenon are the maximum surface magnetic field strength and the surface temperature. In addition, we present strong evidence of the influence of the plasma density distribution on ECME pulse profiles. Results of this kind further motivate the search for MRPs as a robust characterization of the relation between observed ECME properties and stellar physical parameters can only be achieved with a large sample.
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