Multi-wavelengths observations of oscillatory phenomena in a solar network region and their relation to the magnetic field

Details Multi-wavelengths observations of oscillatory phenomena in a solar network region and their relation to the magnetic field Multi-wavelengths observations of oscillatory phenomena in a solar network region and their relation to the magnetic field

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012hell.conf....6k&link_type=abstract

10th Hellenic Astronomical Conference, Proceedings of the conference held at Ioannina, Greece, 5-8 September 2011. Edited by Io

Astronomy and Astrophysics

Astronomy

Scientific paper

The chromosphere is an inhomogeneous and highly dynamic layer of the solar atmosphere. New high resolution observations have revealed that it consists mainly of fine-scale structures which are directly related to the magnetic field. In this work we use multi-wavelength observations to study oscillatory phenomena in the quiet Sun and their relation to the magnetic field and the chromospheric fine-scale structures. The observations were obtained during a coordinated campaign which included space-borne instruments (i.e. the Transition Region and Coronal Explorer, the Michelson Doppler Imager onboard SoHO, and the Specropolarimeter onboard the Hinode spacecraft) and a ground-based telescope (i.e. the Dutch Open Telescope). The analysed data consist of time series of filtergrams of a solar network region observed at different atmospheric layers from the photosphere through the temperature minimum region and well into the chromosphere and also of high resolution magnetograms. Using wavelet analysis we investigate the oscillatory power distribution in the 2D field-of-view, as well as its vertical distribution and its relation with the fine-scale chromospheric mottles, while through phase difference analysis we investigate wave propagation characteristics. Our results show that the oscillatory power has a fibrilar distribution and that chromospheric mottles are directly related to power enhancement (power halo) or suppression (magnetic shadow). This finding is attributed to the interaction between acoustic oscillations and mottles which outline inclined magnetic fields and clearly indicate that mottles are the loci of wave tranmission, reflection and refraction. It also leads to the conclusion that these structures are directly related to the formation of the magnetic canopy, i.e. the layer that divides the atmosphere into two components, a magnetized and a non magnetized one. Extrapolation of the photospheric magnetic field up to the chromosphere using the current-free assumption and use of the VAL C atmospheric model allows the determination of the height of formation of the magnetic canopy and provide the opportunity to highlight the details of the interaction between acoustic o scillations and the magnetic field.

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