Relativistic plasma dynamics originating from solar magnetic reconnection events constitute one of the most intricateastrophysical phenomena, encompassing particle acceleration to near-light velocities and subsequent interactions with gravitational fields and space-time curvature. This investigation presents comprehensive theoretical frameworks for understanding plasma property evolution from ejection during coronal energy releasethrough propagation to Earth’s magnetosphere, where these processes manifest as auroral phenomena. We derive fundamental equations governing relativistic plasma behavior, incorporating Einstein’s field equations, Riemann curvature tensorformulations, and four-velocity descriptions in curved space-time geometries. The analysis integrates Eugene Parker’s groundbreaking solar wind acceleration theory with Subrahmanyan Chandrasekhar’s magnetohydrodynamic equations to explain plasma acceleration to relativistic velocities (v ≈ 0.1c to 0.3c) during magnetic reconnection events and subsequent deceleration to subsonic velocities (v ≈ 400-800 km/s) through gravitational and space-time curvature effects. We examine transitions from relativistic regimes near the Sun, where Lorentz factors γ =(1 − v2/c2) −1/2 approach 1.15, to non-relativistic conditions in Earth’s vicinity. The mathematical framework demonstrates Schwarzschild metric governance of plasma motion within solar gravitational fields, while plasma β parameter transitions from 1 near corona to 1 in solar wind. Our analysis reveals spacetime curvature effects, quantified through Riemann tensor R µ νρσ components, play crucial roles in plasma deceleration, with gravitational redshift and temporal dilation affecting particle energy distributions. The study provides novel insights intofundamental physics connecting solar energy release mechanisms, relativistic plasma propagation, and terrestrial space weatherphenomena.
Prasad et al. (2025) studied this question.