Imaging vector polarimetry at the 10-5 level in the visible and near ultraviolent part of the solar spectrum

Details Imaging vector polarimetry at the 10-5 level in the visible and near ultraviolent part of the solar spectrum Imaging vector polarimetry at the 10-5 level in the visible and near ultraviolent part of the solar spectrum

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003spie.4843...89g&link_type=abstract

Polarimetry in Astronomy. Edited by Silvano Fineschi . Proceedings of the SPIE, Volume 4843, pp. 89-99 (2003).

Astronomy and Astrophysics

Astronomy

1

Scientific paper

New highly sensitive polarimetric instruments and observational techniques allow to observe weak polarization signals in the visible and near ultraviolet part of the solar spectrum. Many of these signals are caused by scattering processes in the upper photosphere and lower chromosphere and thus reflect the thermodynamics of these layers. Also magnetic fields lead to polarization via the Zeeman effect or alter scattering polarization via the Hanle effect. The observation of both effects requires highest polarimetric sensitivity in combination with very high spectral resolution. In the following the instrumental and observational concepts are described. Special emphasis will be given to the Zurich Imaging Polarimeter II, which is now sensitive to the near ultraviolet part of the solar spectrum down to the atmospheric cut-off around 300 nm thanks to the use of a special CCD sensor, which for the first time combines so-called 'open electrod structure' with fast on-chip demodulation in the kHz regime.

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