Issue |
A&A
Volume 510, February 2010
|
|
---|---|---|
Article Number | A41 | |
Number of page(s) | 11 | |
Section | The Sun | |
DOI | https://doi.org/10.1051/0004-6361/200912841 | |
Published online | 05 February 2010 |
Power halo and magnetic shadow in a solar quiet region observed in the Hα line
1
National Observatory of Athens, Institute for Space
Applications and Remote Sensing, Lofos Koufos, 15236 Palea Penteli, Greece e-mail: [jkonto;georgia;kostas]@space.noa.gr
2
Department of Astrophysics, Astronomy and Mechanics, Faculty of Physics, National and Kapodistrian University of Athens, 15784 Zografos, Greece
Received:
7
July
2009
Accepted:
7
December
2009
Context. We investigate the oscillatory behavior of the quiet solar
chromosphere and its discrete components in terms of oscillation properties, i.e. network and internetwork. For this purpose, we use
a time series of high resolution filtergrams at five wavelengths along
the profile, obtained by the Dutch Open Telescope.
Aims. We aim to gain
insight on the distribution of power in different period bands and
its variation between network and internetwork. Our spectral
resolution provides information on the vertical distribution of
power, since the line has both photospheric and chromospheric
components. We investigate the effect of
mottles on
chromospheric oscillations, since they are the most prominent
feature of the
chromosphere and outline inclined magnetic
fields.
Methods. We use wavelet and phase difference analyses of
intensities and Doppler signals. Two-dimensional power maps in the
3, 5 and 7 min period bands as well as coherence and phase
difference maps were constructed.
Results. At photospheric heights, where
the ± 0.7 Å wing is formed, the 3 and 5 min power is
enhanced around the network, and forms power halos. Higher in the
chromosphere these areas are replaced by magnetic shadows, i.e.
places of power suppression. Interestingly, the
power maps show a filamentary structure in the network which correlates very well
with mottles. These areas show positive phase differences at the
3 min period band. At the 5 min and 7 min period bands both
positive and negative phase differences are obtained with an increased
number of pixels with high coherence, indicating the existence of
both upward and downward propagating waves.
Conclusions. We attribute our
findings to the interaction between acoustic oscillations and the
magnetic fields that constitute the magnetic network. The network
flux tubes diverge at chromospheric levels and obtain a significant
horizontal component, which is betrayed by the presence of mottles.
The variation of power reveals the discrete role of the magnetic
field at different heights, which guides or suppresses the
oscillations, depending on its inclination. Spectral resolution in
provides useful information on the coupling between the acoustic
sub-canopy atmosphere and the magnetized chromosphere.
Key words: Sun: chromosphere / Sun: oscillations
© ESO, 2010
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