On the Formation of Lyman β and the O i 1027 and 1028 Spectral Lines

• Published in: The Astrophysical journal 2020-09, Vol.900 (1), p.34
• Main Authors: Hasegawa, Takahiro, Noda, Carlos Quintero, Shimizu, Toshifumi, Carlsson, Mats
• Format: Article
• Language: English
• Subjects: Astrophysics; Atmospheric models; Chromosphere; Computation; Computer simulation; Doppler effect; Gas dynamics; Line of sight; Line spectra; Oxygen; Parameter sensitivity; Physical properties; Quiet Sun; Radiative transfer; Response functions; Solar atmosphere; Solar chromosphere; Solar corona; Solar Orbiter (ESA); Solar orbits; Spatial distribution; Synthesis; Temperature; Velocity
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aba95c

We study the potential of Lyman β and the O i 1027 and 1028 spectral lines to help in understanding the properties of the chromosphere and transition region (TR). The oxygen transitions are located in the wing of Lyman β, which is a candidate spectral line for the solar missions Solar Orbiter/Spectral Imaging of the Coronal Environment and Solar-C (EUVST). We examine the general spectroscopic properties of the three transitions in the quiet Sun by synthesizing them assuming nonlocal thermal equilibrium and taking into account partial redistribution effects. We estimate the heights where the spectral lines are sensitive to the physical parameters, computing the response functions to temperature and velocity using a 1D semiempirical atmospheric model. We also synthesize the intensity spectrum using the 3D enhanced network simulation computed with the Bifrost code. The results indicate that Lyman β is sensitive to the temperature from the middle chromosphere to the TR, while it is mainly sensitive to the line-of-sight (LOS) velocity at the lower atmospheric layers, around 2000 km above the optical surface. The O i lines form lower in the middle chromosphere, being sensitive to the LOS velocities at heights lower than those covered by Lyman β. The spatial distribution of the intensity signals computed with the Bifrost atmosphere, as well as the inferred velocities from the line core Doppler shift, confirms the previous results. Therefore, these results indicate that the spectral window at 1025 contains several spectral lines that complement each other to seamlessly trace the thermal structure and gas dynamics from the middle chromosphere to the lower TR.