Emergence of granular-sized magnetic bubbles through the solar atmosphere. II. Non-LTE chromospheric diagnostics and inversions

Abstract

Magnetic flux emergence into the outer layers of the Sun is a fundamental mechanism for releasing energy into the chromosphere and the corona. In this paper, we study the emergence of granular-sized flux concentrations and the structuring of the corresponding physical parameters and atmospheric diagnostics in the upper photo- sphere and in the chromosphere. We make use of a realistic 3D MHD simulation of the outer layers of the Sun to study the formation of the Ca II 8542 line. We also derive semi-empirical 3D models from non-LTE inversions of our observations. These models contain depth-dependent information of the temperature and line-of-sight stratification. Our analysis explains the peculiar Ca II 8542 profiles observed in the flux-emerging region. In addition, we derive detailed temperature and velocity maps describing the ascent of magnetic bubbles from the photosphere to the chromosphere. The inversions suggest that, in active regions, granular-sized bubbles emerge up to the lower chromosphere where the existing large-scale field hinders their ascent. We report hints of heating when the field reaches the chromosphere.

arXiv commentSubmitted to ApJ, 10 Figures

References in corpus (47)

• The Interface Region Imaging Spectrograph (IRIS)
• On Solving the Coronal Heating Problem
• The stellar atmosphere simulation code Bifrost
• CRISP Spectropolarimetric Imaging of Penumbral Fine Structure
• Prevalence of Small-scale Jets from the Networks of the Solar Transition Region and Chromosphere
• An Ab Initio Approach to the Solar Coronal Heating Problem
• The formation of the Halpha line in the solar chromosphere
• CRISPRED: A data pipeline for the CRISP imaging spectropolarimeter
• The formation of IRIS diagnostics II. The formation of the Mg II h&k lines in the solar atmosphere
• Heating of the magnetized solar chromosphere by partial ionization effects
• An Open Source, Massively Parallel Code for Non-LTE Synthesis and Inversion of Spectral Lines and Zeeman-induced Stokes Profiles
• Solar surface emerging flux regions: a comparative study of radiative MHD modeling and Hinode SOT observations
• Non-equilibrium hydrogen ionization in 2D simulations of the solar atmosphere
• Emergence of small-scale magnetic loops through the quiet solar atmosphere
• On the prevalence of small-scale twist in the solar chromosphere and transition region
• Twisted flux tube emergence from the convection zone to the corona
• Spatially coupled inversion of spectro-polarimetric image data I: Method and first results
• 2D Radiative MHD Simulations of the Importance of Partial Ionization in the Chromosphere
• The Unresolved Fine Structure Resolved - IRIS observations of the Solar Transition Region
• Transverse component of the magnetic field in the solar photosphere observed by Sunrise
• Multiwavelength Observations of Small-Scale Reconnection Events triggered by Magnetic Flux Emergence in the Solar Atmosphere
• The Solar Internetwork. I. Contribution to the Network Magnetic Flux
• DELO-Bezier formal solutions of the polarized radiative transfer equation
• Three-dimensional non-LTE radiative transfer computation of the Ca 8542 infrared line from a radiation-MHD simulation
• 3D Temperature Mapping of Solar Photospheric Fine Structure Using Ca II H Filtergrams
• The origin of the reversed granulation in the solar photosphere
• Non-local thermodynamic equilibrium inversions from a 3D MHD chromospheric model
• The effect of the relative orientation between the coronal field and new emerging flux: I Global Properties
• The usefulness of analytic response functions
• Emergence of granular-sized magnetic bubbles through the solar atmosphere: I. Spectropolarimetric observations and simulations
• Opposite polarity field with convective downflow and its relation to magnetic spines in a sunspot penumbra
• Twisted flux tube emergence from the convection zone to the corona II: Later states
• Isotopic anomaly and stratification of Ca in magnetic Ap stars
• Solar velocity references from 3D HD photospheric models
• Heating of the magnetic chromosphere: observational constraints from Ca II 8542 spectra
• Non-equilibrium calcium ionisation in the solar atmosphere
• Clusters of small eruptive flares produced by magnetic reconnection in the sun
• The magnetic flux of the quiet Sun internetwork as observed with the Tenerife Infrared Polarimeter
• Scattering Polarization of the Ca II IR Triplet for Probing the Quiet Solar Chromosphere
• The Role of Partial Ionization Effects in the Chromosphere
• The effect of isotopic splitting on the bisector and inversions of the solar Ca II 854.2 nm line
• Temporal Evolution of Velocity and Magnetic Field in and around Umbral Dots
• Solar Flare Chromospheric Line Emission: Comparison Between IBIS High-resolution Observations and Radiative Hydrodynamic Simulations
• Scattering polarization in the CaII Infrared Triplet with Velocity Gradients
• Chromospheric diagnosis with Ca II lines: forward modeling in forward scattering (I)
• Heavy Calcium in CP Stars
• The calcium isotopic anomaly in magnetic CP stars

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