Modeling solar coronal bright point oscillations with multiple nanoflare heated loops

TL;DR

This study models coronal bright point oscillations using a multithreaded nanoflare heated loop model, revealing that observed intensity oscillations are likely shock wave propagations along magnetic loops.

Contribution

It introduces a novel multithreaded nanoflare heated loop model to simulate and analyze bright point oscillations, linking observed periods to shock wave dynamics.

Findings

Oscillation periods match previous observations

Oscillations are likely shock wave propagations

Adiabatic standing modes can be extracted with background subtraction

Abstract

Intensity oscillations of coronal bright points (BPs) have been studied for past several years. It has been known for a while that these BPs are closed magnetic loop like structures. However, initiation of such intensity oscillations is still an enigma. There have been many suggestions to explain these oscillations, but modeling of such BPs have not been explored so far. Using a multithreaded nanoflare heated loop model we study the behavior of such BPs in this work. We compute typical loop lengths of BPs using potential field line extrapolation of available data (Chandrashekhar et al. 2013), and set this as the length of our simulated loops. We produce intensity like observables through forward modeling and analyze the intensity time series using wavelet analysis, as was done by previous observers. The result reveals similar intensity oscillation periods reported in past observations. It is suggested these oscillations are actually shock wave propagations along the loop. We also show that if one considers different background subtractions, one can extract adiabatic standing modes from the intensity time series data as well, both from the observed and simulated data.