On the relationship between G-band bright point dynamics and their magnetic field strengths

TL;DR

This study investigates how the magnetic field strength of G-band bright points influences their motion, revealing that stronger magnetic fields correlate with slower, more erratic movements, highlighting magnetic flux's role in solar surface dynamics.

Contribution

The paper provides a detailed analysis of the relationship between GBP magnetic field strength and their dynamic behavior using high-resolution observations, a novel approach in solar physics.

Findings

Stronger magnetic fields lead to slower GBP motions.

Weaker magnetic fields are associated with faster, straighter GBP paths.

Magnetic flux concentrations resist convective flows more effectively.

Abstract

G-band bright points (GBPs) are regarded as good manifestations of magnetic flux concentrations. We aim to investigate the relationship between the dynamic properties of GBPs and their longitudinal magnetic field strengths. High spatial and temporal resolution observations were recorded simultaneously with G-band filtergrams and Narrow-band Filter Imager (NFI) Stokes I and V images with Hinode /Solar Optical Telescope. The GBPs are identified and tracked in the G-band images automatically, and the corresponding longitudinal magnetic field strength of each GBP is extracted from the calibrated NFI magnetograms by a point-to-point method. After categorizing the GBPs into five groups by their longitudinal magnetic field strengths, we analyze the dynamics of GBPs of each group. The results suggest that with increasing longitudinal magnetic field strengths of GBPs correspond to a decrease in their horizontal velocities and motion ranges as well as by showing more complicated motion paths. This suggests that magnetic elements showing weaker magnetic field strengths prefer to move faster and farther along straighter paths, while stronger ones move more slowly in more erratic paths within a smaller region. The dynamic behaviors of GBPs with different longitudinal magnetic field strengths can be explained by that the stronger flux concentrations withstand the convective flows much better than weaker ones.