Solar energy paper index
The Internal Magnetic Field Structure of ICMEs in the Heliosphere
One-line summary
A solar energy research paper on The Internal Magnetic Field Structure of ICMEs in the Heliosphere.
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Chinese explanation / 中文解读
中文解读待补充：本站会优先为光伏效率、钙钛矿太阳能电池、储能技术、太阳能热利用、BIPV、并网技术等高价值论文补充中文说明。
Original abstract
Interplanetary coronal mass ejections (ICMEs) are major drivers of heliospheric disturbances and space-weather effects. Here we present a multi-spacecraft study of 96 magnetic clouds (MCs) distributed over a broad range of heliocentric distances, and reconstruct their internal magnetic structure with a uniform-twist Gold--Hoyle (GH) flux-rope model. From the fits, we derive the axial field strength $B_0$, the twist density (turn density) $τ$, the GH parameter $ω$, and the integrated twist number $n$. We find that $B_0$ and the turn density $τ$ both decrease with increasing heliocentric distance, consistent with expansion and axial stretching during propagation. A key result is that the upper envelope in the $τ$--$R$ plane corresponds to a nearly constant boundary in the dimensionless GH parameter $ω=2πRτ$, close to $ω\sim2$. Therefore, the inferred upper value of $τ$ is not scale-independent, but follows $τ_{\max}\simeq ω_{\max}/(2πR)$ for a given flux-rope radius. In contrast, the estimated integrated turn number $n$ shows no similarly clear radial organization in the present sample. This study investigates the ICME structure and magnetic field characteristics across heliocentric distances from 0.07 to 5.4~AU, thereby providing observational constraints on the large-scale evolution of interplanetary magnetic flux ropes.
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