Tootfinder

The evolution of CME sheath turbulence from L1 to Earth: Wind and MMS observations of the 2023-04-23 CME
Matthew R. Argall, Li-Jen Chen, No\'e Lugaz, Norberto Romanelli, Jaye L. Verniero, Charles W. Smith, Brandon Burkholder, Victoria Wilder
https://arxiv.org/abs/2505.13645

The evolution of CME sheath turbulence from L1 to Earth: Wind and MMS observations of the 2023-04-23 CME
An interplanetary shock driven by a coronal mass ejection (CME) containing an interval of sub-Alfvénic flow impacted Earth on April 23, 2024. In this article, we analyze the turbulence in the sheath region between the shock and CME to determine how it evolves from L1 (as observed by Wind) to Earth (as observed by MMS, upstream of the bow shock). Wind and MMS were separated by $55\,\mathrm{R_{E}}$ in the dawn-dusk direction, but the shock normals differ by only $2.8^{\circ}$ and the Pearson cor…

The Quasi-Radial Field-line Tracing (QRaFT): an Adaptive Segmentation of the Open-Flux Solar Corona
Vadim M. Uritsky, Christopher E. Rura, Cooper Downs, Shaela I. Jones, Charles Nickolos Arge, Nathalia Alzate
https://arxiv.org/abs/2506.14894

The Quasi-Radial Field-line Tracing (QRaFT): an Adaptive Segmentation of the Open-Flux Solar Corona
Optical observations of solar corona provide key information on its magnetic geometry. The large-scale open field of the corona plays an important role in shaping the ambient solar wind and constraining the propagation dynamics of the embedded structures, such as interplanetary coronal mass ejections. Rigorous analysis of the open-flux coronal regions based on coronagraph images can be quite challenging because of the depleted plasma density resulting in low signal-to-noise ratios. In this pape…

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What Causes Errors in Wang-Sheeley-Arge Solar Wind Modeling at L1 ?
Satabdwa Majumdar, Martin Reiss, Karin Muglach, Charles N. Arge
https://arxiv.org/abs/2506.09676

What Causes Errors in Wang-Sheeley-Arge Solar Wind Modeling at L1 ?
Previous ambient solar wind (SW) validation studies have reported on discrepancies between modeled and observed SW conditions at L1. They indicated that a major source of discrepancies stems from how we model the solar corona. Thus, enhancing predictive capabilities demands a thorough examination of coronal modeling. The Wang-Sheeley-Arge (WSA) model has been a workhorse model that provides the near-Sun SW conditions. An important component of it is the Potential Field Source Surface (PFSS) mod…

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