The predominant fusion chain in stellar nucleosynthesis produces positron and neutrino byproducts in equal amounts. An extremely high neutrino flux can be directly measured, but the unobservable, yet equally high flux of positrons is traditionally considered to be short-lived antimatter that annihilates upon contact with electrons. The electrons are traditionally assumed to be populated in such excess that their annihilation with positrons could be sustained indefinitely. This paper posits that, considering the extremely high positron and neutrino flux within a stellar core, there is an opportunity for localized positron populations and accumulation. As there are no existing methods to directly observe a positron accumulation within the solar core, evidence must rely largely on observations of the surface and above. The difficulties of direct observation into internal stellar processes introduces a chance to overlook critical components such as a theoretical positron accumulation, thus exacerbating unresolved stellar questions surrounding observed coronal signatures and high-energy emission channels. This investigation examines the potential for stellar positron accumulation, its consequences for core dynamics, and observational signatures that could support the existence of long-lived positrons. The framework is applied to problems in stellar and galactic physics, solar weather forecasting, and high-energy-density plasma systems.