Network and Internetwork: a compared Multiwavelength Analysis

TL;DR

This study investigates the temporal behavior of solar network bright points and internetwork areas, revealing their magnetic associations and oscillation differences at various atmospheric levels using multiwavelength observations.

Contribution

It provides a comparative analysis of NBPs and internetwork oscillations across multiple wavelengths, highlighting magnetic correlations and wave propagation characteristics.

Findings

NBPs are co-spatial with enhanced magnetic fields.

NaD2 line emission proxies magnetic structures.

NBPs show a 2.2 mHz oscillation peak at chromospheric levels.

Abstract

We analyze the temporal behavior of Network Bright Points (NBPs), present in the solar atmosphere, using a set of data acquired during coordinated observations between ground-based observatories (mainly at the NSO/Sacramento Peak) and the Michelson Doppler Interferometer onboard SOHO. We find that, at any time during the observational sequence, all the NBPs visible in the NaD2 images are co-spatial within 1 arcsec with locations of enhanced magnetic field. In analogy with the Ca II K line, the NaD2 line center emission can be used as a proxy for magnetic structures. We also compare the oscillation properties of NBPs and internetwork areas. At photospheric levels no differences between the two structures are found in power spectra, but analysis of phase and coherence spectra suggests the presence of downward propagating waves in the internetwork. At chromospheric levels some differences are evident in the power spectrum between NBPs and internetwork. The power spectrum of NBPs at the Halpha core wavelength shows an important peak at 2.2 mHz (7 minutes), not present in the internetwork areas. Its coherence spectrum with Halpha wings shows very low coherence at this frequency, implying that the oscillations at these chromospheric levels are not directly coupled with those present in lower layers.