Emergence of Internetwork Magnetic Fields through the Solar Atmosphere

• Published in: The Astrophysical journal Vol. 911; no. 1; pp. 41 - 58
• Main Authors: Gošić, M., Pontieu, B. De, Bellot Rubio, L. R., Sainz Dalda, A., Pozuelo, S. Esteban
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-04-2021; IOP Publishing
• Subjects: Astrophysics; Atmosphere; Chromosphere; Magnetic fields; Magnetic flux; Magnetic loops; Magnetism; Photosphere; Polarimetry; Quiet Sun; Solar atmosphere; Solar chromosphere; Solar energy; Solar magnetic field; Solar magnetic fields; Solar magnetic flux emergence; Solar photosphere; Solar surface; Solar transition region
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/abe7e0

Abstract
Internetwork (IN) magnetic fields are highly dynamic, short-lived magnetic structures that populate the interior of supergranular cells. Since they emerge all over the Sun, these small-scale fields bring a substantial amount of flux, and therefore energy, to the solar surface. Because of this, IN fields are crucial for understanding the quiet Sun (QS) magnetism. However, they are weak and produce very small polarization signals, which is the reason why their properties and impact on the energetics and dynamics of the solar atmosphere are poorly known. Here we use coordinated, high-resolution, multiwavelength observations obtained with the Swedish 1 m Solar Telescope and the Interface Region Imaging Spectrograph (IRIS) to follow the evolution of IN magnetic loops as they emerge into the photosphere and reach the chromosphere and transition region. We studied in this paper three flux emergence events having total unsigned magnetic fluxes of 1.9 × 10
18
, 2.5 × 10
18
, and 5.3 × 10
18
Mx. The footpoints of the emerging IN bipoles are clearly seen to appear in the photosphere and to rise up through the solar atmosphere, as observed in Fe
i
6173 Å and Mg
i
b
2
5173 Å magnetograms, respectively. For the first time, our polarimetric measurements taken in the chromospheric Ca
ii
8542 Å line provide direct observational evidence that IN fields are capable of reaching the chromosphere. Moreover, using IRIS data, we study the effects of these weak fields on the heating of the chromosphere and transition region.