Statistical Properties of Magnetic Bright Points at Different Latitudes and Longitudes of the Sun

Abstract

Magnetic bright points (MBPs) are located in intergranular channels on the solar surface. Studying the properties and evolution process of MBPs can help us to better understand solar activity and predict solar events that have a significant impact on Earth. In this study, we performed a statistical analysis of MBPs at different latitudes and longitudes. Data from the quiet-Sun (QS) in the eastward-equator (8 June 2021) and in the southern hemisphere (31 July 2020), as well as data from the QS near the disk center (30 July 2020), are analyzed. We studied the properties of MBPs, including lifetime, intensity contrast, and velocity. Moreover, we analyzed the intensity contrast of isolated MBPs at the moments of their birth and disappearance at different latitudes and longitudes, as well as the variation in the number of MBPs that appeared and disappeared in each frame. The results show that non-isolated MBPs have longer lifetimes than isolated MBPs, and the average lifetime of non-isolated MBPs located in the southern hemisphere (SH) is significantly shorter than that of MBPs near the disk center (DC) in the eastward-equator (EE). We find that the lifetime of non-isolated MBPs in the SH is negatively correlated with the intensity contrast, with higher intensity contrast associated with a shorter lifetime. The velocities of isolated MBPs at different latitudes and longitudes follow a Rayleigh distribution, while the velocities of non-isolated MBPs follow a log-normal distribution. Non-isolated MBPs exhibit higher horizontal velocities, with the maximum horizontal velocity reaching 8 km s⁻¹. Finally, we find that the number of isolated MBPs per square Mm at different latitudes and longitudes remains stable during consecutive periods, and the intensity contrast of isolated MBPs is similar at the moment of their birth and disappearance.