Parkes observations for project P1189 semester 2024APRS_12

The study of "space weather" is crucial, given the profound impact of solar wind and Coronal Mass Ejection (CME) phenomena on the solar system, presenting risks to Earth's satellites, the power grid, and civilian infrastructure. Observational studies emphasize the primary influence of magnetic fields on the early eruptive phase of CMEs. Despite advancements, understanding CME magnetic fields, especially at low solar altitudes during initial acceleration, remains limited. Valuable insights can be gained by probing the heliosphere at various distances from the sun through observational methods. In this project, our focus is on establishing baseline measurements for the dispersion measure (DM) and rotation measure (RM) at solar altitudes ($> 20 R_\odot$). We achieve this through regular monitoring of pulsars at larger solar elongations. Challenges arise, such as the varying trend in measured DM for some pulsars due to low-frequency catalog data, impacting the creation of a DM baseline for high-frequency UWL measurements. Preliminary analyses of observed pulsars indicate promising results, prompting further cross-matching with CME events and focused modeling efforts with robust observational coverage.

空间天气研究至关重要，因为太阳风与日冕物质抛射（CME）现象对太阳系具有深远影响，会对地球卫星、电网及民用基础设施构成风险。观测研究强调磁场对日冕物质抛射早期爆发阶段的主导作用。尽管研究取得进展，但对日冕物质抛射磁场的理解——尤其是初始加速阶段低太阳高度处的磁场——仍存在局限。通过观测手段探测太阳不同距离处的日球层，有望获得宝贵见解。本项目旨在建立太阳高度（>20 R⊙）处色散量（DM）与旋转量（RM）的基线测量值，具体通过对较大太阳距角处脉冲星的常规监测实现。研究面临若干挑战，例如部分脉冲星的测量色散量（DM）因低频星表数据存在变化趋势，这会影响高频UWL测量色散量基线的构建。对观测脉冲星的初步分析显示出良好结果，这推动了与日冕物质抛射事件的进一步交叉匹配，以及开展具有全面观测覆盖的针对性建模工作。