Predicting the Magnetic Fields of a Stealth CME Detected by Parker Solar Probe at 0.5 AU

Abstract

Stealth coronal mass ejection (CMEs) are eruptions from the Sun that are not associated with appreciable low-coronal signatures. Because they often cannot be linked to a well-defined source region on the Sun, analysis of their initial magnetic configuration and eruption dynamics is particularly problematic. In this manuscript, we address this issue by undertaking the first attempt at predicting the magnetic fields of a stealth CME that erupted in 2020 June from the Earth-facing Sun. We estimate its source region with the aid of off-limb observations from a secondary viewpoint and photospheric magnetic field extrapolations. We then employ the Open Solar Physics Rapid Ensemble Information (OSPREI) modelling suite to evaluate its early evolution and forward-model its magnetic fields up to Parker Solar Probe, which detected the CME in situ at a heliocentric distance of 0.5 AU. We compare our hindcast prediction with in-situ measurements and a set of flux rope reconstructions, obtaining encouraging agreement on arrival time, spacecraft crossing location, and magnetic field profiles. This work represents a first step towards reliable understanding and forecasting of the magnetic configuration of stealth CMEs and slow, streamer-blowout events.

9 pages, 4 figures, 1 table, accepted for publication in The Astrophysical Journal

References in corpus (13)

• No Trace Left Behind: Stereo Observation of a Coronal Mass Ejection without Low Coronal Signatures
• The Solar Probe Cup on Parker Solar Probe
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Cited by in corpus (6)

• Parker Solar Probe: Four Years of Discoveries at Solar Cycle Minimum
• Multipoint interplanetary coronal mass ejections observed with Solar Orbiter, BepiColombo, Parker Solar Probe, Wind and STEREO-A
• OSPREI: A Coupled Approach to Modeling CME-Driven Space Weather with Automatically-Generated, User-Friendly Outputs
• A magnetic cloud prediction model for forecasting space weather relevant properties of Earth-directed coronal mass ejections
• On the utility of flux rope models for CME magnetic structure below 30$R_{\odot }$
• Is there a Dynamic Difference between Stealthy and Standard CMEs?