Solar Atmospheric Oscillations and the Chromospheric Magnetic Topology

Details Solar Atmospheric Oscillations and the Chromospheric Magnetic Topology Solar Atmospheric Oscillations and the Chromospheric Magnetic Topology

2006-11-07

arxiv.org/abs/astro-ph/0611206v1

Astron.Astrophys. 461 (2007) L1-L4

Astronomy and Astrophysics

Astrophysics

4 pages, 3 figure, A&A Letters in press

Scientific paper

10.1051/0004-6361:20066415

We investigate the oscillatory properties of the quiet solar chromosphere in relation to the underlying photosphere, with particular regard to the effects of the magnetic topology. We perform a Fourier analysis on a sequence of line-of-sight velocities measured simultaneously in a photospheric (Fe I 709.0 nm) and a chromospheric line (Ca II 854.2 nm). The velocities were obtained from full spectroscopic data acquired at high spatial resolution with the Interferometric BIdimensional Spectrometer (IBIS). The field of view encompasses a full supergranular cell, allowing us to discriminate between areas with different magnetic characteristics. We show that waves with frequencies above the acoustic cut-off propagate from the photosphere to upper layers only in restricted areas of the quiet Sun. A large fraction of the quiet chromosphere is in fact occupied by ``magnetic shadows'', surrounding network regions, that we identify as originating from fibril-like structures observed in the core intensity of the Ca II line. We show that a large fraction of the chromospheric acoustic power at frequencies below the acoustic cut-off, residing in the proximity of the magnetic network elements, directly propagates from the underlying photosphere. This supports recent results arguing that network magnetic elements can channel low-frequency photospheric oscillations into the chromosphere, thus providing a way to input mechanical energy in the upper layers.

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