Formation dynamics of a rotating solar spicule-like event and associated energy-mass transport
Year: 2026
Type: article
Abstract: Vortical structures and elongated chromospheric spicule-like features are ubiquitous small-scale dynamic phenomena in the lower solar atmosphere. Both are important channels for transporting mass and energy from the solar surface to the corona. However, the physical connection between vortical motions and the formation of spicule-like structures, as well as their role in mass and energy transport, remains incompletely understood. We aim to investigate the connection between the vortex motion and the formation of a spicule-like event and the associated mass and energy transport. We performed three-dimensional radiative magnetohydrodynamic (3D RMHD) simulations in an upward-directed (positive-polarity) open magnetic field with an initial background strength of 10 G. We identified vortex-associated spicule-like events and carried out a detailed analysis of one representative event. Prior to the formation of this spicule-like event, a photospheric vortex appears and twists the magnetic field lines, then develops upwards into higher atmospheric layers, forming a magnetic tornado system. This event is generated during this process. At the periphery of this magnetic tornado, twisted magnetic field lines with negative vertical components reconnect with both external positive-polarity background fields and central positive-polarity fields. The magnetic reconnection sites rise and rotate together with the developed magnetic tornado, and many jet-like substructures in this event are closely associated with plasma upward ejections from these reconnection regions. A vertical force analysis shows that, for this event, plasma uplift in the photosphere and lower chromosphere is dominated by the pressure-gradient force, whereas in the upper chromosphere, the Lorentz force gradually becomes dominant. At a height of about 4,Mm above the solar surface, this event produces a mean upward mass flux density of the order of -7 ̊m kg m^ -2 s^ -1 and a mean upward Poynting flux density of approximately 525 ̊m W m^ -2 . The wave-mode decomposition results show that the energy transport associated with the rotational spicule-like event is dominated by the Alfvén mode. Alfvén waves, fast-mode waves, and slow-mode waves carry energy into the lower corona in an approximate ratio of 10:7:3. Our results demonstrate that spicule-like events can be driven jointly by the vortex motion in the lower atmosphere and the induced magnetic reconnection. During its formation process, considerable mass and energy are transported to the lower corona.
Source: Astronomy and Astrophysics
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $1,865
OpenAlex ID: W7221530513