Bibcode
Trujillo-Bueno, J.; Štěpán, J.; Casini, Roberto
Bibliographical reference
The Astrophysical Journal Letters, Volume 738, Issue 1, article id. L11 (2011).
Advertised on:
9
2011
Citations
52
Refereed citations
41
Description
We present some theoretical predictions concerning the amplitude and
magnetic sensitivity of the linear-polarization signals produced by
scattering processes in the hydrogen Lyα line of the solar
transition region. To this end, we have calculated the atomic-level
polarization (population imbalances and quantum coherences) induced by
anisotropic radiation pumping in semiempirical and hydrodynamical models
of the solar atmosphere, taking into account radiative transfer and the
Hanle effect caused by the presence of organized and random magnetic
fields. The line-center amplitudes of the emergent linear-polarization
signals are found to vary typically between 0.1% and 1%, depending on
the scattering geometry and the strength and orientation of the magnetic
field. The results shown here encourage the development of UV
polarimeters for sounding rockets and space telescopes with the aim of
opening up a diagnostic window for magnetic field measurements in the
upper chromosphere and transition region of the Sun.
Related projects
Magnetism, Polarization and Radiative Transfer in Astrophysics
Magnetic fields pervade all astrophysical plasmas and govern most of the variability in the Universe at intermediate time scales. They are present in stars across the whole Hertzsprung-Russell diagram, in galaxies, and even perhaps in the intergalactic medium. Polarized light provides the most reliable source of information at our disposal for the
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