On the effect of oscillatory phenomena on Stokes inversion results

Abstract

Stokes inversion codes are crucial in returning properties of the solar atmosphere, such as temperature and magnetic field strength. However, the success of such algorithms to return reliable values can be hindered by the presence of oscillatory phenomena within magnetic wave guides. Returning accurate parameters is crucial to both magnetohydrodynamics studies and solar physics in general. Here, we employ a simulation featuring propagating MHD waves within a flux tube with a known driver and atmospheric parameters. We invert the Stokes profiles for the 6301 $\unicode{0xc5}$ and 6302 $\unicode{0xc5}$ line pair emergent from the simulations using the well-known Stokes Inversions from Response functions (SIR) code to see if the atmospheric parameters can be returned for typical spatial resolutions at ground-based observatories. The inversions return synthetic spectra comparable to the original input spectra, even with asymmetries introduced in the spectra from wave propagation in the atmosphere. The output models from the inversions match closely to the simulations in temperature, line-of-sight magnetic field and line-of-sight velocity within typical formation heights of the inverted lines. Deviations from the simulations are seen away from these height regions. The inversion results are less accurate during passage of the waves within the line formation region. The original wave period could be recovered from the atmosphere output by the inversions, with empirical mode decomposition performing better than the wavelet approach in this task.

arXiv commentAccepted for publication in Phil. Trans. R. Soc. A, 20 pages, 4 figures

References in corpus (39)

• On the Generation, Propagation, and Reflection of Alfven Waves from the Solar Photosphere to the Distant Heliosphere
• VFISV: Very Fast Inversion of the Stokes Vector for the Helioseismic and Magnetic Imager
• An Open Source, Massively Parallel Code for Non-LTE Synthesis and Inversion of Spectral Lines and Zeeman-induced Stokes Profiles
• Advanced Forward Modeling and Inversion of Stokes Profiles Resulting from the Joint Action of the Hanle and Zeeman Effects
• STiC -- A multi-atom non-LTE PRD inversion code for full-Stokes solar observations
• Properties of Magneto-Hydrodynamic Waves in the Solar Photosphere with Hinode
• Physical Properties of a Sunspot Chromosphere with Umbral Flashes
• Dynamics of the Solar Magnetic Network: Two-dimensional MHD Simulations
• On the validity of the 630 nm Fe I nm lines for the magnetometry of the internetwork quiet Sun
• Spectropolarimetric NLTE inversion code SNAPI
• Photospheric observations of surface and body modes in solar magnetic pores
• Stokes Inversion based on Convolutional Neural Networks
• The Velocity Distribution of Solar Photospheric Magnetic Bright Points
• On the properties of slow mhd sausage waves within small-scale photospheric magnetic structures
• Wave propagation and energy transport in the magnetic network of the Sun
• The Magnetic Response of the Solar Atmosphere to Umbral Flashes
• Magnetic field strength distribution of magnetic bright points inferred from filtergrams and spectro-polarimetric data
• Spectropolarimetric inversions of the Ca ii 8542 Å line in a M-class solar flare
• Non-linear propagation of kink waves to the solar chromosphere
• A High-Resolution Three-Dimensional Model of the Solar Photosphere Derived from Hinode Observations
• Magnetic field variations associated with umbral flashes and penumbral waves
• A Hot Downflowing Model Atmosphere For Umbral Flashes And The Physical Properties Of Their Dark Fibrils
• Dynamic properties of bright points in an active region
• Spectropolarimetric analysis of an active region filament. I. Magnetic and dynamical properties from single component inversions
• Hinode observations reveal boundary layers of magnetic elements in the solar photosphere
• Propagating Spectropolarimetric Disturbances in a Large Sunspot
• Inversions of synthetic umbral flashes: effects of the scanning time on the inferred atmospheres
• Inference of magnetic fields in the very quiet Sun
• Fast inversion of solar Ca II spectra
• The potential of many-line inversions of photospheric spectropolarimetric data in the visible and near UV
• Height variation of magnetic field and plasma flows in isolated bright points
• The magnetic properties of photospheric magnetic bright points with high resolution spectropolarimetry
• Kinematics of Magnetic Bright Features in the Solar Photosphere
• Spectropolarimetric observations of an arch filament system with the GREGOR solar telescope
• Stokes Diagnostics of Magneto-Acoustic Wave Propagation in the Magnetic Network on the Sun
• Magnetic Properties and Flow Angle of the Inverse Evershed Flow at Its Downflow Points
• Milne-Eddington inversion of the Fe I line pair at 630~nm
• Magnetic upflow events in the quiet-Sun photosphere. I. Observations
• Inversions of synthetic umbral flashes: selection of wavelength sampling

Cited by in corpus (4)

• Waves in the lower solar atmosphere: the dawn of next-generation solar telescopes
• A novel approach to identify resonant MHD wave modes in solar pores and sunspot umbrae: $B-\omega$ analysis
• High-resolution wave dynamics in the lower solar atmosphere
• Inferring Line-of-Sight Velocities and Doppler Widths from Stokes Profiles of GST/NIRIS Using Stacked Deep Neural Networks