The outine of a new solar Flare-Monitoring-Telescope is given, which was built at the Hida Observatory of Faculty of Science, Kyoto University, in the first financial year of the Japan's STEP project. The telescope is unique among currently-operating solar flare-patrol-telescopes, because it can simultaneously observe five solar images, which are four full disc images in Ha center, Ha + 0.8 A, Ha -0.8 A and continuum, and one solar limb image in Ha center. After its start of operation it was confirmed that this telescope system is very useful to study the dynamical features of Ha filament disappearance, because it can, for the first time, continuously record the full solar disc simultaneously in three wavelengths of the Ha line. Two typical examples of Ha filament disappearance observed with the telescope are demonstrated and are comparatively studied. It is found that the more dynamical and more energetic Ha filament eruption causes the larger enhancement of soft X-ray bright arcade structure observed with the Soft X-ray Telscope of Yohkoh.

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To obtain full Stokes spectra in multi-wavelength windows simultaneously, we developed a new spectro-polarimeter on the Domeless Solar Telescope at Hida Observatory. The new polarimeter consists of a 60 cm aperture vacuum telescope on an altazimuth mount, an image rotator, a high dispersion spectrograph, polarization modulator and analyzer composed of a continuously rotating waveplate with a retardation nearly constant around 127 • in 500 -1100 nm and a polarizing beam splitter located closely behind the focus of the telescope, fast and large format CMOS cameras and an infrared camera. The slit spectrograph allows us to obtain spectra in as many wavelength windows as the number of cameras. We characterized the instrumental polarization of the entire system and established the polarization calibration procedure. The cross-talks among the Stokes Q,U and V are evaluated to be about 0.06% ∼ 1.2% depending on the degree of the intrinsic polarizations. In a typical observing setup, a sensitivity of 0.03% can be achieved in 20 -60 second for 500 nm -1100 nm. The new polarimeter is expected to provide a powerful tool to diagnose the 3D magnetic field and other 1 vector physical quantities in the solar atmosphere.