Authors: Meiqi Wang(NJIT), Matsumoto Keitarou(NJIT), Sijie Yu(NJIT), Bin Chen(NJIT), and Wickline, Mallory(NJIT)

The acceleration and transport of flare-related solar energetic electrons (SEEs) remain unresolved problems in heliophysics. We present a comprehensive multi-instrument analysis of a solar eruptive event associated with a GOES M-class flare on 5 February 2026, observed continuously from the low corona to interplanetary space. The event was accompanied by an impulsive SEE event detected in situ by Solar Orbiter/EPD. During the flare, multiple successive burst episodes were observed in the low corona through microwave and hard X-ray emissions recorded by EOVSA and Solar Orbiter/STIX, respectively. The same episodes manifested as intense type III radio bursts (>1000 sfu) imaged by OVRO-LWA in the mid-corona over a frequency range of ~10–80 MHz, and as interplanetary type III radio bursts detected by Wind, STEREO, and Solar Orbiter/RPW over frequencies from ~0.1–10 MHz. By tracing the type III radio bursts continuously from the low corona into interplanetary space, we investigate the magnetic connectivity, transport pathways, and directivity of escaping energetic electrons. Combining data-driven MHD simulations with imaging spectroscopy observations from EOVSA, STIX, and OVRO-LWA, we connect the burst-to-burst changes in acceleration and transport with the magnetic environment near the acceleration and escape sites. We discuss the origins, acceleration, and escape processes of energetic electrons near the Sun. Our analysis provides new insights into both the acceleration of solar energetic electrons and their subsequent transport from the low corona into interplanetary space.