Direct Observation of A Large-scale CME Flux Rope Event Arising from an Unwinding Coronal Jet

TL;DR

This study documents a large-scale CME flux rope formation from an unwinding coronal jet, highlighting magnetic interactions and twist transport that contribute to solar eruptions and space weather phenomena.

Contribution

It provides the first detailed stereoscopic observation linking unwinding jets to large-scale CME flux ropes, revealing magnetic coupling processes during solar eruptions.

Findings

Unwinding blowout jet can generate a large-scale flux rope.

Twist of 1.4-2.0 turns is transported into the flux rope.

Eruption involves two-stage magnetic reconnection.

Abstract

Coronal mass ejections (CMEs) and coronal jets are two types of common solar eruptive phenomena, which often independently happen at different spatial scales. In this work, we present a stereoscopic observation of a large-scale CME flux rope arising from an unwinding blowout jet in a multipolar complex magnetic system. Based on a multi-band observational analysis, we find that this whole event starts with a small filament whose eruption occurs at a coronal geyser site after a series of homologous jets. Aided by magnetic field extrapolations, it reveals that the coronal geyser site forms above an elongate opposite-polarity interface, where the emergence-driven photospheric flux cancellation and repetitive reconnection are responsible for those preceding recurrent jets and also contribute to the ultimate filament destabilization. By interacting with overlying fields, the erupting filament breaks one of its legs and results in an unwinding blowout jet. Our estimation suggests that around 1.4$-$2.0 turns of twist release in its jet spire. This prominent twist transport in jet spire rapidly creates a newborn larger-scale flux rope from the jet base to a remote site. Soon after its formation, this large-scale flux rope erupts towards the outer coronae causing an Earth-directed CME. In its source region, two sets of distinct post-flare loops form in succession, indicating this eruption involves two-stage of flare magnetic reconnection. This work not only reveals a real magnetic coupling process between different eruptive activities but provides a new hint for understanding the creation of large-scale CME flux ropes during the solar eruption.