Wave propagation and shock formation in different magnetic structures

Abstract

Velocity oscillations "measured" simultaneously at the photosphere and the chromosphere -from time series of spectropolarimetric data in the 10830 A region- of different solar magnetic features allow us to study the properties of wave propagation as a function of the magnetic flux of the structure (i.e. two different-sized sunspots, a tiny pore and a facular region). While photospheric oscillations have similar characteristics everywhere, oscillations measured at chromospheric heights show different amplitudes, frequencies and stages of shock development depending on the observed magnetic feature. The analysis of the power and the phase spectra, together with simple theoretical modeling, lead to a series of results concerning wave propagation within the range of heights of this study. We find that, while the atmospheric cut-off frequency and the propagation properties of the different oscillating modes depend on the magnetic feature, in all the cases the power that reaches the high chromosphere above the atmospheric cut-off comes directly from the photosphere by means of linear vertical wave propagation rather than from non-linear interaction of modes.

Accepted for publication in The Astrophysical Journal. 29 pages, 9 figures, 12pt, preprint

References in corpus (6)

• Spectropolarimetric investigation of the propagation of magnetoacoustic waves and shock formation in sunspot atmospheres
• Channeling 5-min photospheric oscillations into the solar outer atmosphere through small-scale vertical magnetic flux tubes
• The influence of coronal EUV irradiance on the emission in the He I 10830 A and D3 multiplets
• Influence of atomic polarization and horizontal illumination on the Stokes profiles of the He I 10830 multiplet
• Signatures of Incomplete Paschen-Back Splitting in the Polarization Profiles of the He I 10830 multiplet
• Spicule emission profiles observed in \ion{He}{i} 10830 Å

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