Investigating the role of plasmoid instability in the acceleration of charged particles in the solar coronal plasma

Shahraki Pour, Mahdi; Hosseinpour, Mahboub

doi:10.47176/ijpr.25.2.12053

Investigating the role of plasmoid instability in the acceleration of charged particles in the solar coronal plasma

Document Type : Original Article

Authors

Mahdi Shahraki pour ¹

Mahboub Hosseinpour ²

¹ Department of Physics, Faculty of Science, Shahid Chamran University of Ahvaz

² Faculty of Physics, University of Tabriz

https://doi.org/10.47176/ijpr.25.2.12053

Abstract

Plasmoid instability in the magnetized plasma of the solar corona, caused by the extended process of nonlinear magnetic reconnection, suddenly releases the plasma's stored magnetic energy in the form of plasma jets and accelerates non-thermal particles and relativistic charged particles. One of the most significant consequences of magnetic reconnection and the plasmoids formation in the solar Corona, as well as in the magnetopause and the Earth's magnetic tail, is the acceleration of charged particles towards the atmosphere. Based on a two-dimensional particle-in-cell simulation of plasmoid instability, the acceleration of charged particles within the solar coronal plasma is investigated through the charge particle distribution function. According to the distribution function of charged particles, electrons are capable of reaching upstream speeds upon plasmoid instability forming. During the early stages of the development of plasmoid instability, the Maxwell distribution function exhibits an additional hump due to an increase in the number of resonant electrons in the wave-particle interaction process. Eventually, this positive slope disappears and its energy is transferred to waves, but subsequent magnetic reconnection causes particles to travel at their most probable speed

Keywords

Particles acceleration

Magnetic reconnection

Plasmoid instability

Solar corona

Particle-in-cell simulation

Subjects

Plasma Physics

L Chen, et al., Nature Physics 4, 1 (2008) 19.
L Comisso, and L Sironi Physical Review Letters 121, 25 (2018) 255101.
G Zank and O Verkhoglyadova, Space Science Reviews, 130 (2007) 255.
B Cerutti, et al., The Astrophysical Journal770, 2 (2013) 147.
J Birn, and E Priest, Cambridge University Press (2007).
M Yamada, R Kulsrud, and H Ji, Reviews of Modern Physics 82 (2010) 08543.
W Gonzalez and E Parker, Astrophysics and space science library427 (2016) 542.
S Markidis et al., Processes Geophys. 19 (2012) 145.
N Loureiro, et al., Phys. Plasmas 14 (2007) 100703.
P Cargill, et al., Space Sci Rev 173 (2012) 223.
S Feng, et al., The Astrophysical Journal 753 (2012)
M Yamada and J Yoo, Nature communication 5 (2014) 4774.
W Wan, et al., Physics of Plasmas 15, 3 (2008).
J Dahlin, et al.,Physics of Plasma 21, 9 (2014).
H Wang, et al., Physics of Plasmas 24, 5 (2017).
P Muñozv and J Buechner, The Astrophysical Journal 864, 1 (2018) 92.
Q Zhang, et al., arXiv preprint arXiv (2404)
B Chen, et al, The Astrophysical Journal 866, 1 ( 2018) 62.
H Reid, E Kontar, The Astrophysical Journal 867, 2 ( 2018) 158.
L Feng, et al, Astronomy & Astrophysics 1, 538 (2012) A34.
M Shahraki Pour, and M Hosseinpour, Frontiers in Astronomy and Space Sciences 8 (2022) 802898.