On fibrils and field lines: The nature of H$\alpha$ fibrils in the solar chromosphere

TL;DR

This study uses 3D radiation-MHD simulations to explore the complex relationship between H-alpha fibrils and magnetic field lines in the solar chromosphere, revealing their dynamic interactions and the caution needed when interpreting fibril motions.

Contribution

It provides the first detailed analysis of the connection between synthetic H-alpha fibrils and magnetic field lines, highlighting their complex, dynamic relationship in the chromosphere.

Findings

Fibrils sometimes trace the same magnetic field line along their length.

Fibrils sample different field lines at different locations.

Fibrils are influenced by slow-mode and transverse waves along field lines.

Abstract

Observations of the solar chromosphere in the line-core of the \Halpha\ line show dark elongated structures called fibrils that show swaying motion. We performed a 3D radiation-MHD simulation of a network region, and computed synthetic \Halpha\ images from this simulation to investigate the relation between fibrils and the magnetic field lines in the chromosphere. The periods, amplitudes and phase-speeds of the synthetic fibrils are consistent with those observed. We analyse the relation between the synthetic fibrils and the field lines threading through them, and find that some fibrils trace out the same field line along the fibril's length, but there are also fibrils that sample different field lines at different locations along their length. Fibrils sample the same field lines on a time scale of $\sim200$~s. This is shorter than their own lifetime. We analysed the evolution of the atmosphere along a number of field lines that thread through fibrils and find that they carry slow-mode waves that load mass into the field line, as well as transverse waves that propagate with the Alfv\'en speed. Transverse waves propagating in opposite directions cause an interference pattern with complex apparent phase speeds. The relationship between fibrils and field lines is complex. It is governed by constant migration and swaying of the field lines, their mass loading by slow modes and subsequent draining, and their actual visibility in \Halpha. Field lines are visible where they lie close to the optical depth unity surface. The location of the latter is governed by the height at which the column mass in the chromosphere reaches a certain value. We conclude that using the swaying motion of fibrils as a tracer of chromospheric transverse oscillations must be done with caution.