发表机构
Riga Technical University; Ventspils University of Applied Sciences, Engineering Research Institute “Ventspils International Radio Astronomy Center”; Centre for Fusion, Space and Astrophysics, Department of Physics, University of Warwick; Centro de Investigacion en Astronomía, Universidad Bernardo O’Higgins; ASTRON – Netherlands Institute for Radio Astronomy（里加工业大学; 文茨皮尔斯应用科学大学，文茨皮尔斯国际射电天文中心工程研究所; 华威大学物理系聚变、太空与天体物理中心; 贝尔纳多·奥希金斯大学天文学研究中心; 荷兰射电天文研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文编制了LOFAR LV614站在2022-2025年探测的335个太阳射电暴目录，涵盖I-V型，给出了流量、频率、高度及漂移等参数，并分析了事件分布规律。
AI 中文摘要
本文介绍了拉脱维亚Irbene天文台LV614 LOFAR站以独立模式在2022年6月至2025年8月期间于29-60 MHz频率范围内探测到的太阳射电暴目录（见https URL）。观测以每周一次的频率进行，时间分辨率为1秒，频谱分辨率为0.195 MHz。累计观测时长为1125.2小时。对所有分析过的观测数据，均使用仙后座A作为参考源进行了带通校准。该目录共包含335个太阳射电暴，涵盖了I-V型全部五种主要类型的射电暴。具体而言，目录中分别包含23个、8个、293个、6个和5个I型、II型、III型、IV型和V型射电暴的参数。探测到的射电暴峰值流量范围从0.3 SFU到234 SFU。目录提供了峰值流量、峰值频率以及射电源在太阳表面上方的估计高度等信息。对于II型和III型射电暴，我们还给出了频率漂移的估计值，其平均值分别为0.043 MHz s⁻¹和4.383 MHz s⁻¹。我们还拟合了df/dt = Af^a关系，最佳拟合参数为A=0.78，a=0.43。发现I型和III型事件的数量随峰值流量的增加而减少，幂律指数分别约为-0.9和-1.25。对于III型射电暴，我们估计了电子束速度，对于基频，其范围在光速的0.005到0.477之间，对于二次谐波，其范围在光速的0.008到0.794之间。
英文摘要
A catalogue (https://doi.org/10.5281/zenodo.20157853) of solar radio bursts detected with the LV614 LOFAR station at the Irbene Observatory, Latvia, in the stand-alone mode from June 2022 to August 2025 in the 29-60 MHz frequency range is presented. Observations were conducted with the weekly cadence, one-second time resolution, and 0.195 MHz spectral resolution. The cumulative duration of the observation was 1125.2 h. For all analysed observations, bandpass calibration was applied using Cassiopeia A as a reference source. In total, the catalogue includes 335 solar radio bursts. Radio bursts of all five main types, I-V, were detected. Specifically, the catalogue contains parameters of 23, 8, 293, 6, and 5 bursts of Type I, II, III, IV, and V, respectively. The detected burst peak flux ranges from 0.3 SFU to 234 SFU. The catalogue provides information about the peak flux and frequency, and the estimated height of the source above the solar surface. For Type II and III bursts, we also give the estimations of the frequency drifts, with mean values $ 0.043 ~\mathrm{MHz\,s^{-1}}$ and $4.383 ~\mathrm{MHz\,s^{-1}}$, respectively. We also estimated the fit $df/dt = Af^a$, with the best fit parameters $A=0.78$ and $a=0.43$. The numbers of Type I and III events are found to decrease with the peak flux, with the power law indices about $-0.9$ and $-1.25$, respectively. For Type III, we estimated electron beam speed ranging from 0.005 to 0.477 of the speed of light for the fundamental frequency, and 0.008 to 0.794 of the speed of light for its second harmonic.
CommentsAccepted for publication in The Astrophysical Journal Supplement Series
