活動星系核 (AGN) 內的中微子，由於能直接穿透吸積盤及星系核周圍的複雜環境，成為探測黑洞周圍環境與星系演化過程的重要信觀測對象。釋放中微子的活動星系核，同時也是極高能加速粒子的所在之處。長久以來天文學家認為中微子源自於帶有噴流的活動星系核。這類天體噴流所產生的電磁輻射，在觀測中表現出明顯的時變特性。雖然學界已經有很好的模型去解釋這些噴流的光譜和亮度變化，但強子過程在射電偏振觀測中的作用仍待深入探究。本研究旨在建立噴流射電偏振觀測與中微子產生機制之間的聯繫，重點探討 AGN 噴流中瞬態強子事件引發的偏振特徵時變性。假設瞬變現象源自環繞黑洞運行的恆星與噴流物質的相互作用, 噴流內的質子與恆星風中的重子發生碰撞並產生次級輕子, 進而與磁場發生作用而產生同步輻射。同步輻射的偏振特性不僅受到噴流內螺旋狀磁場結構的影響，噴流以接近光速運動時，也會改變電場偏振向量的方向。除此之外，觀測角度、質子能譜分佈、恆星參數（質量損失率、軌道週期等）也都會影響輻射偏振隨時間的變化。在眾多恆星參數中，恆星質量損失率最顯著影響強子碰撞導致的亮度的增強。透過「雙競爭區模型」，持續數月的時變特徵被模擬出來的同時，偏振變化與同步輻射總通量變化也呈現強相關性。這類事件具有隨機爆發特性，且其互動所產生的輻射很難和噴流本身的光區分開來。因此由強子碰撞過程中產生的射電輻射，在噴流活動較弱且時變性較高的 AGN 中比較有可能被探測到。

Neutrino Active Galactic Nuclei (AGNs) are some of the most fascinating astrophysical objects, as they contain information about the origin of the most energetic cosmic rays, activity of supermassive black holes, and the growth of galaxies. Among various classes of AGNs, jetted AGNs have long been proposed as prominent sources of astrophysical neutrinos. On the other hand, electromagnetic emission from jetted AGNs are often characterized by substantial variability. Although significant progress has been made in modeling the spectral and temporal characteristics of AGN jet emission, the role of hadronic processes in shaping the radio polarization remains less explored. This work aims to bridge the gap between radio polarisation observation and neutrino production in AGN jets. I investigate the spectral and temporal variability of the polarization signatures arising from transient hadronic events in AGN jets. It is assumed that the transient phenomenon results from stars interacting with the jet as they orbit a supermassive black hole. In this jet-star model, the polarized synchrotron radiation is determined by the jet's magnetic field structure, the jet's Lorentz factor, the viewing angle, the proton energy distribution and various stellar parameters. We find that the mass loss rate is the most important stellar parameter to account for strong hadronic flares. By using a numerical approach, we demonstrate that a two-zone model gives rise to substantial variability spanning monthlong timescale. The polarization evolution strongly correlates with the changes in the total synchrotron flux. These events are sporadic in nature and difficult to distinguish from jet emission. As a result, hadronic signatures in the radio regime are more likely to be detected in AGNs with weak, variable jet activity, where a jet's contribution is less dominant.