How Small-scale Jetlike Solar Events from Miniature Flux Rope Eruptions Might Produce the Solar Wind

Abstract

We consider small-scale jetlike events that might make the solar wind, as has been suggested in recent studies. We show that the events referred to as “coronal jets” and as “jetlets” both fall on a power-law distribution that also includes large-scale eruptions and spicule-sized features; all of the jetlike events could contribute to the solar wind. Based on imaging and magnetic field data, it is plausible that many or most of these events might form by the same mechanism: Magnetic flux cancelation produces small-scale flux ropes, often containing a cool-material minifilament. This minifilament/flux rope erupts and reconnects with adjacent open coronal field, along which “plasma jets” flow and contribute to the solar wind. The erupting flux ropes can contain twist that is transferred to the open field, and these become Alfvénic pulses that form magnetic switchbacks, providing an intrinsic connection between switchbacks and the production of the solar wind.

Source Region of the Solar Wind: Statistics of the Doppler Velocities at the Chromosphere

“…Such a proposal is preferential for the in situ observations of the prevalent small-scale magnetic flux ropes (Zhao et al 2020;Chen et al 2020;Huang et al 2023). The occurrence frequency follows a negative correlation of the sizes of the erupted filament (Sterling et al 2024). Direct evidence has been obtained (Uritsky et al 2023) of power-law distribution of the occurrence rate according to different characteristics of the ∼2300 outflows observed in the polar region of the AIA/171 Å image.…”

“…All the above small-scale jets are suggested to be generated by a similar process as the coronal jets or coronal mass ejections, i.e., the magnetic reconnection of the opposite magnetic polarities, which are responsible for the filament eruption at different scales Sterling et al 2024). Such a proposal is preferential for the in situ observations of the prevalent small-scale magnetic flux ropes (Zhao et al 2020;Chen et al 2020;Huang et al 2023).…”

“…As the reference region that we selected is not absolute flux balanced and the remnant flux is more preferential to be distributed at the magnetic concentrations, it is still reasonable that the samples at the network boundaries show similar features between the CH regions and the reference quiet region. However, the distribution similarity of the network samples and the entire CH region samples may indicate that the downflows are not distributed everywhere at the network boundaries but at specific locations, such as the places where the jetlike events (Shen 2021;Sterling et al 2024) originate.…”

Axial Flux Evolution of Small-scale Magnetic Flux Ropes from 0.06 to 10 au

“…No information about magnetic flux is currently available for the events in Huang et al (2023). It may be possible to compare with existing estimates of the number of eruptions on the Sun at any given time as a function of size (e.g., Sterling & Moore 2016;Sterling et al 2024) if one makes assumptions about the field strength. However, the number of flux ropes on the Sun at a time is not necessarily the number of flux ropes passing through the inner heliosphere at a time, which depends on the SMFR rate of occurrence (unknown in the near-Sun interplanetary space), speed (known through spacecraft measurements), and length (completely unknown as of yet).…”

“…Based on observations of magnetic discontinuities, Borovsky (2008) proposed that the solar wind is filled with flux tubes of photospheric origin. However, recent findings indicate that small-scale solar eruptions may contribute numerous flux ropes to the heliosphere (Sterling & Moore 2020;Huang et al 2023;Sterling et al 2024).…”