A Statistical Study of Protostars with Monitoring Observations in the X-ray Band

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(1) We obtained the proof that a Class 0 candidate emits X-rays. (2) In order to access the origin and the geometry of protostars by detecting flares from them, we investigated key parameters for a flare on stars. Using the Monitor of All-sky X-ray Image (MAXI), we searched huge X-ray flares on stars, and obtained the dependence of flare frequencies with flare energy and the relation of flare energy to the stellar spot size, ranging ten orders of magnitude, from small solar flares to huge stellar flares. (3) In a multi-wavelength observation of II Peg, we detected a huge version of two-ribbon flare. (4) We established a way to bend crystals by depositing Diamond Like Carbon on the surface of them. The bent crystals can be an X-ray imaging poralimetry which makes use of Bragg reflection. We also confirmed that the optics can converge X-ray beam.