Fluid Velocity Mapping and Magnetic Reconnection Rates in the Solar Corona via High-Resolution Extreme Ultraviolet Telescopes

International Journal of Physics | Vol. 10, No. 12, December 2019 | pp. 89–96

DOI: 10.46882/2019/IJP/000116

Research Article

Title: Fluid Velocity Mapping and Magnetic Reconnection Rates in the Solar Corona via High-Resolution Extreme Ultraviolet Telescopes

Names of Authors: G. R. Davies¹, M. T. Al-Saeed²

Authors’ Affiliations:
¹ School of Physics and Astronomy, University of St Andrews, St Andrews, UK
² Department of Physics, Faculty of Science, Kuwait University, Safat, Kuwait

Abstract: Magnetic reconnection is the primary physical process driving explosive energy releases in solar atmospheric plasma, heating material to millions of Kelvin and accelerating coronal mass ejections. This paper evaluates fluid velocity mapping and quantifies local magnetic reconnection rates within an X-class solar flare event. We utilized high-resolution spectroscopic data from space-based extreme ultraviolet (EUV) channels tracking highly ionized iron lines (Fe XVI and Fe XXIV). Differential affine velocity estimator algorithms were deployed to construct two-dimensional velocity fields of plasma inflows and outflows surrounding the current sheet. The empirical measurements reveal systematic plasma inflows moving at 18.2 km/s, while directed outflows reach velocities of 285.0 km/s along the coronal loop headers. Based on these transport metrics, the local dimensionless reconnection rate was calculated to range between 0.05 and 0.08. These values closely match fast reconnection regimes predicted by the Petschek theoretical framework modified by localized turbulent transport. Spectroscopic line-broadening analysis indicates localized turbulent temperatures peaking at 9.2 MK within the diffusion region, confirming intense localized viscous dissipation. These imaging diagnostics provide direct observational parameters for refining magnetohydrodynamic models of solar coronal heating loops.

Keywords: Solar corona; magnetic reconnection; extreme ultraviolet; plasma dynamics; solar flares; magnetohydrodynamics

Manuscript Timeline: Received: August 18, 2019; Revised: October 10, 2019; Accepted: November 02, 2019; Published: December 16, 2019

Citation: Davies, G. R., & Al-Saeed, M. T. (2019). Fluid Velocity Mapping and Magnetic Reconnection Rates in the Solar Corona via High-Resolution Extreme Ultraviolet Telescopes. International Journal of Physics, 10(12), 89–96.

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