Bibcode
Beck, C.; Tritschler, A.; Wöger, F.
Referencia bibliográfica
Astronomische Nachrichten, Vol.331, Issue 6, p.574-576
Fecha de publicación:
6
2010
Número de citas
9
Número de citas referidas
8
Descripción
We investigate the thermodynamical and magnetic properties of a
``dark-cored" fibril seen in the chromospheric Ca II IR line at 854.2 nm
to determine the physical process behind its appearance. We analyse a
time series of spectropolarimetric observations obtained in the Ca II IR
line at 854.2 nm and the photospheric Fe I line at 630.25 nm. We
simultaneously invert the spectra in both wavelength ranges with the SIR
code to obtain the temperature and velocity stratification with height
in the solar atmosphere and the magnetic field properties in the
photosphere. The structure can be clearly traced in the line-of-sight
(LOS) velocity and the temperature maps. It connects from a small pore
with kG fields to a region with lower field strength. The flow velocity
and the temperature indicate that the height of the structure increases
with increasing distance from the inner footpoint. The Stokes V signal
of 854.2 nm shows a Doppler-shifted polarization signal with the same
displacement as in the intensity profile, indicating that the supersonic
flow seen in the LOS velocity is located within magnetized plasma. We
conclude that the chromospheric dark-cored fibril traces a siphon flow
along magnetic field lines, driven by the gas pressure difference caused
by the higher magnetic field strength at the inner footpoint. We suggest
that fast flows guided by the magnetic field lead to the appearance of
``dark-cored" fibrils in intensity images. Although the observations
included the determination of the polarization signal in the
chromospheric Ca II IR line, the signal could not be analysed
quantitatively due to the low S/N. Chromospheric polarimetry will thus
require telescopes of larger aperture able to collect a sufficient
number of photons for a reliable determination of polarization in deep
and only weakly polarized spectral lines.
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