Coronal hole picoflare jets are progenitors of both fast and Alfv\'enic slow solar wind

TL;DR

This study links coronal hole picoflare jets to the origins of both fast and Alfvénic slow solar wind, showing how jet activity influences wind properties through observations from Solar Orbiter.

Contribution

It provides the first direct observational evidence connecting picoflare jets in coronal holes to different types of solar wind, unifying their origins.

Findings

Picoflare jets are widespread in coronal holes.

Jet activity correlates with the emergence of fast and Alfvénic slow solar wind.

Radial expansion of coronal holes influences wind speed.

Abstract

Solar wind, classified by its bulk speed and the Alfv\'enic nature of its fluctuations, generates the heliosphere. The elusive physical processes responsible for the generation of the different types of this wind are a topic of active debate. Recent observations reveal intermittent jets, with kinetic energy in the picoflare range, emerging from dark areas of a polar coronal hole threaded by open magnetic field lines. These could substantially contribute to solar wind. However, their ubiquity and direct links to solar wind have not been established. Here, we report a unique set of remote-sensing and in situ observations from the Solar Orbiter spacecraft that establish a unified picture of fast and Alfv\'{e}nic slow wind, connected to the similar widespread picoflare jet activity in two coronal holes. Radial expansion of coronal holes ultimately regulates the speed of the emerging wind.