Coronal streamers on the Sun and their physical properties

Porfir'eva, G. A.; Yakunina, G. V.; Delone, A. B.; Oreshina, A. V.; Oreshina, I. V.

doi:10.30970/jps.13.2901

Cited by 7 publications

(1 citation statement)

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“…Figure 11 flows. From 3.5 to 20R s , the flow speeds increase from 78 to 340 km s −1 in CR 2177, and from 55 to 360 km s −1 in CR 2212 for low-speed flows, which is basically consistent with the white-light observations of the LASCO SOHO C2 and C3 (Porfiréva et al 2009). Meanwhile, the flow speeds of the LDHS flows increase from 300 to 660 km s −1 in CR 2177 and from 264 to 625 km s −1 in CR 2212, which is basically compatible with the previous coronal observations (Pätzold et al 1997).…”

Section: Steady Solar Corona Near the Sunsupporting

confidence: 84%

Implicit Solar Coronal Magnetohydrodynamic (MHD) Modeling with a Low-dissipation Hybridized AUSM-HLL Riemann Solver

Wang

Xiang

Liu

et al. 2022

ApJ

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In this paper, we develop a 3D implicit single-fluid magnetohydrodynamic (MHD) model to simulate the steady-state solar corona with a wide range of Mach numbers and low plasma β. We employ a low-dissipation advection upstream splitting method (AUSM) to calculate the convective flux in the regions of low Mach numbers for a high resolution, and hybridize the AUSM with Harten-Lax-van Leer Riemann solver in the regions of high Mach numbers to improve the solver’s robustness. The inner boundary condition of no backflow is implemented by numerical flux. A reconstruction method based on the divergence-free radial basis function is adopted to enhance the divergence-free constraint of magnetic field. Also, an anisotropic thermal conduction term is considered; the positivity-preserving reconstruction method is used to prevent the presence of negative thermal pressure and plasma density, and the implicit lower-upper symmetric Gauss Seidel method is implemented for a better convergence rate. After establishing the implicit solar wind MHD model, we employ it to simulate steady-state solar coronal structures in Carrington rotations 2177 and 2212. The simulations demonstrate that the MHD model’s computational efficiency is desirable, and the modeled results are basically in agreement with the solar coronal observations and the mapped in situ measurements from the OMNI archive. Consequently, this implicit MHD model is promising to simulate a complex plasma environment with high-intensity magnetic field and wide-ranging Mach numbers.

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Section: Steady Solar Corona Near the Sunsupporting

confidence: 84%