In order to derive solar magnetic fields, a 2D spectro-polarimeter working in the near-infrared wavelength range is under development. A voltage-wavelength-tunable lithium-niobate (LiNbO3) etalon filtergraph is used as the 2D spectrometer. A rotating waveplate for modulating the polarization is used, which has a nearly constant retardation of about 127 degrees over a wide wavelength range. The filtergraph consists of two etalons, 0.9 mm and 1.2 mm thick, optimized for ordinary ray transmission for both the He I 1083 nm chromospheric line and the photospheric magnetic-sensitive line of Fe I 1564 nm when used in tandem-etalon configuration. The etalons are Y-cut LiNbO3 wafers coated with reflective and conductive (ITO) layers. A linear polarizer between the rotating retarder and the filtergraph functions as a polarization analyzer and selects the ordinary ray transmission. We carried out polarization observations of solar active regions at several wavelength points in the He I 1083 nm line with a high-speed IR camera at Hida Observatory, Kyoto University. Some observational results together with the instrumental properties are presented.
We describe newly developed voltage-tunable lithium-niobate (LiNbO3) Fabry-Perot etalons for solar near-infrared filtergraph. Two etalons were fabricated for tandem use: One etalon is 0.9 mm thick and the other is 1.2 mm thick, optimized in ordinary ray transmission for both He I 1083.035 nm and magnetic sensitive Fe I 1564.85 nm lines. The etalons are Y-cut lithium-niobate wafers coated with highly reflective and conductive (ITO) layers. We examined optical and voltage-tunable properties of the etalons using the horizontal spectrograph of the Domeless Solar Telescope at Hida Observatory, Kyoto University. Some solar observations with tandem etalons were also ran and their good imaging quality was demonstrated. Some results from the measurements are reported.
Solar Magnetic Activity Research Telescope (SMART) at Hida observatory is in operational to monitor the solar activity. As a new solar Hα observing instrument for SMART, we developed "Solar Dynamics Doppler Imager (SDDI)", which can measure the three-dimensional motion of solar eruptive phenomena. These eruptive events could be affective to the earth magnetism and cause serious damage to our society. The purpose of SMART/SDDI is monitoring and forecasting the geo-affective solar eruptions. In this paper, we present the development of the tunable filter "F40", the key component of SDDI. The features of TF40 are, (1) fast tuning of observation wavelength, (2) narrow transmission width and large free spectral range (FSR), (3) large field-of-view that covers the entire solar disk with a 20 cm objective lens. TF40 has 7 stages of optical blocks. Each stage consists of a linear polarizer, calcites, a quartz as half waveplate and a Liquid Crystal Variable Retarder (LCVR), and has the periodic transmission profile with 0.05, 0.1, 0.2, 0.4, 0.8, 1.6 and 3.2 nm period at Hα line (656.2808 nm), respectively. Combining the 7 stages, the 0.025 nm transmission width and 3.2 nm FSR are achieved. Retardation of each LCVR and its dependence on applied voltage and temperature were measured for modeling its characteristics, with which we calculate the voltage for desired retardation. Best-shaped transmission profile is obtained by further adjustment of voltages of individual LCVRs using the real solar light. We report the performance and current observing status of the TF40.
In this work, we introduce an image enhancement method ideally suited for the visualization of coronal intensity images. The steep radial gradient of the coronal brightness is adjusted by normalising the coronal image with the Fourier approximation of its local average. A method based on deconvolution and localised normalising of the data at many different spatial scales is used to further enhance the fine structures, and a wavelet shrinkage denoising method is used for noise suppression. The effectiveness of this method is demonstrated on a series of images observed by various instruments including spacial and earth-based coronagraphs as well as photos during total solar eclipse. This method is very helpful for qualitative analysis of solar coronal structures that are mostly invisible on original images.
We have developed a new narrowband tunable filter to perform imaging spectroscopy of the solar chromosphere.
Using Liquid Crystal Variable Retarders (LCVRs) as the tuning elements for wavelength, wide-band polarizers
and super achromatic half-wave plates, it is possible to make high speed tuning (about 0.1Sec), to exclude
mechanical drives (and oil tank), and to cover a wide wavelength range (510-100nm). This filter builds up
with seven stages each consisting of a pair of calcites, LCVR, half-wave plates and linear polarizer. The full
width at half maximum (FWHM) of the filter transmission is about 0.025nm at 656.3nm.We demonstrate that
the concept of the universal tunable filter using the LCVR's as tuning elements is highly promising for future
application to space mission and ground based observations.
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