next previous
Up: Abstract

Astron. Astrophys. Suppl. Ser. 133, 285-292

Fabry-Perot filter based solar video magnetograph

S.K. Mathew - A. Bhatnagar - C.D. Prasad - A. Ambastha

Send offprint request: S.K. Mathew

Udaipur Solar Observatory, Physical Research Laboratory, Udaipur - 313001, India

Received April 20; accepted June 11, 1998


A tunable Lithium Niobate (LiNbO3) Fabry-Perot filter (FP) (passband 165 mÅ at 6122 Å) based video magnetograph has been designed and fabricated. This instrument is capable of providing near simultaneous observations of photospheric longitudinal magnetic field, chromospheric H$\alpha$, and photospheric CaI pictures using the same telescope and back-end set-up. The magnetic field measurements are made by using the polarization properties of the Zeeman components of the photospheric CaI line at 6122 Å (Landé g factor of 1.75). The CaI line has been chosen due to its low temperature sensitivity and no blend with other solar or atmospheric lines. A variable electro-optic quarter wave retarder, KD*P (Potassium di-Deuterium Phosphate) along with a linear polarizer is used for analyzing the circular polarization of the Zeeman components. The filter tuned at 140 mÅ away from the line center in the blue wing is found to give the best linear response for the field strength up to 1500 Gauss. A field of view (FOV) of $\sim4 \times 3$ arcmin on the solar disk is imaged using a $699 \times 288$ pixel Cohu CCD camera in synchronous with the KD*P modulation. The $\lambda/4$ modulation is achieved by applying $\pm$2100 volts to the KD*P to obtain alternate frames of oppositely circular polarized images. These images are stored in separate frame buffers of an image acquisition system. To achieve high signal to noise ratio, a large number of images (maximum 256) are added in the respective frame buffers and then the difference between the left and the right circularly polarized images is obtained. This difference is related to the magnetic field strength. On comparing the video magnetograms (VMG) obtained at Udaipur Solar Observatory (USO) on 09 April 1997 at 09:32 UT with those taken by SOHO/MDI at 09:41 UT, it was found that all the magnetic features matched very well in both the magnetograms. In this paper we present the details of the instrument and examples of observations.

Key words: instruments: polarimeter -- Sun: activity; flares; magnetic fields

next previous
Up: Abstract

Copyright The European Southern Observatory (ESO)