Under solar-scaled magnetograms with E_FR ∝ ⟨B★⟩², CME speed and mass rise roughly as v_CME ∝ ⟨B★⟩ and M_CME ∝ ⟨B★⟩^1.5, driven mainly by the upward Lorentz force.
The SOHO LASCO CME Catalog -- Version 2
1 Pith paper cite this work. Polarity classification is still indexing.
abstract
This paper provides an update on the coronal mass ejection (CME) catalog maintained at the CDAW Data Center, NASA Goddard Space Flight Center (https://cdaw.gsfc.nasa.gov/CME_list). This is version 2 (v2) of the Catalog that has been made as the default version as of May 1, 2024. The new features of the Catalog v2 are (i) online measurement tool, (ii) combination JavaScript movies from the STEREO and Solar Dynamics Observatory (SDO) missions, and (iii) insertion of newly identified CMEs for the period 1996 to 2004. The CME identification was revisited resulting in a set of $\sim$3000 new CMEs added to the Catalog. A vast majority of these CMEs are weak and narrow. The resulting statistical properties of CMEs are not significantly different from those reported using version 1.
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astro-ph.SR 1years
2026 1verdicts
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How Magnetic Field Strength Affects Stellar Coronal Mass Ejection Dynamics
Under solar-scaled magnetograms with E_FR ∝ ⟨B★⟩², CME speed and mass rise roughly as v_CME ∝ ⟨B★⟩ and M_CME ∝ ⟨B★⟩^1.5, driven mainly by the upward Lorentz force.