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.
