# Characteristics of EUV Solar Coronal Bright Points Using Time Series Analyses

## TL;DR

This study analyzes the temporal behavior of solar coronal bright points at two EUV wavelengths, revealing differences in lifetimes, intensity fluctuations, and a time delay in peak emissions related to magnetic reconnection.

## Contribution

It introduces a detailed time series analysis of CBPs at 171 and 193 Å, highlighting differences in their lifetimes, intensity fluctuations, and the timing of peak emissions, which advances understanding of their magnetic dynamics.

## Key findings

- CBPs at 171 Å have longer lifetimes than at 193 Å.
- CBPs at 171 Å exhibit more intensity fluctuations and higher density features.
- Peak emissions at 171 Å generally occur before those at 193 Å by 12 seconds to 2 minutes.

## Abstract

Coronal bright points (CBPs) as characteristics of the solar corona are small-scale bright features ubiquitously observed at extreme ultraviolet passbands. Here, we focused on time series of CBPs in the periods of their lifetimes. We used Solar Dynamic Observatory (SDO) / Atmospheric Imaging Assembly (AIA) taken at 171 and 193 \AA. Using image processing methods, CBPs were extracted from data and tracked during their lifetimes. We found that CBPs observed in 171 \AA have more lifetimes than those of observed at 193 \AA. CBPs at 171 \AA are more fluctuated in intensity and appeared as highly density number (DN) features than 193 \AA CBPs. It was found that about $75 \%$ of CBPs are firstly achieved their peak at 171 \AA, and then, after 12 seconds two minutes are achieved to their peak at 193 \AA. Computing Pearson correlation for time series of CBPs at both wavelengths where the correlation reaches at maximum value gives information about time delay of magnetic reconnection about 40 seconds from one layer to the other one.