Kobayashi, T.

Paper	Title	Page
TUPAN043	RF Amplitude and Phase Tuning of J-PARC DTL	1481
	M. Ikegami, Z. Igarashi, H. Tanaka KEK, Ibaraki H. Asano, T. Kobayashi JAEA/J-PARC, Tokai-Mura, Naka-Gun, Ibaraki-Ken K. Hasegawa, T. Ito, T. Morishita, S. Sato, A. Ueno JAEA/LINAC, Ibaraki-ken H. Sako JAEA, Ibaraki-ken
	The beam commissioning of J-PARC linac has been started in November 2006. In the beam commissioning, the tuning of the RF phase and amplitude for its DTL (Drift Tube Linac) has been performed with a phase-scan method. Detailed results of the RF tuning are presented with a brief discription of the tuning procedure.
WEPMN024	RF Feedback Control Systems of the J-PARC Linac	2101
	Z. Fang, S. Anami, S. Michizono, S. Yamaguchi KEK, Ibaraki T. Kobayashi JAEA/J-PARC, Tokai-Mura, Naka-Gun, Ibaraki-Ken H. Suzuki JAEA, Ibaraki-ken
	The commissioning of the J-PARC 181MeV proton linac was started from October of 2006. The RF sources of the linac consist of 4 solid-state amplifiers and 20 klystrons. In each RF source, the RF fields are controlled by a digital RF feedback system installed in a compact PCI (cPCI) to realize the accelerating field stability of ±1% in amplitude and ±1 degree in phase. In this paper the performance of the RF feedback control systems will be reported in detail.
WEPMN039	Performance of J-PARC Linac RF System	2128
	T. Kobayashi JAEA/J-PARC, Tokai-Mura, Naka-Gun, Ibaraki-Ken S. Anami, Z. Fang, Y. Fukui, M. Kawamura, S. Michizono, K. Nanmo, S. Yamaguchi KEK, Ibaraki E. Chishiro, T. Hori, H. Suzuki, M. Yamazaki JAEA, Ibaraki-ken
	High power operation of all the RF systems of J-PARC linac was started for the cavity conditioning in October 2006. Twenty 324-MHz klystrons have powered the accelerating cavities successfully, and the beam commissioning was started in November 2006. The performance of the RF drive and control system will be presented.
FRZKI02	Neutrino Physics	3835
	T. Kobayashi KEK, Ibaraki
	Twenty years have passed after the supernova SN1987A. Before SN1987A, it was often said that neutrino physics was largely an art of learning a great deal by observing nothing. But after SN1987A, the neutrino became a little less mysterious. The solar neutrino deficit which was observed in the Homestake solar neutrino experiment, was confirmed by Kamiokande, Gallex and SAGE. An atmospheric neutrino anomaly was observed in Kamiokande. IMB, MACRO and SUDEN reconfirmed this anpmaly. In 1998 Super-Kamiokande obtained the evidence of atmospheric neutrino oscillations. This was the first discovery of a finite neutrino mass. The atmospheric neutrino oscillations were reconfirmed by K2K. In 2002 SNO detected the evidence of flavor-transformation of solar neutrinos, and KamLAND detected the evidence of reactor antineutrino oscillations. In my talk what we learned from the above neutrino experiments is briefly reviewed, and what we will learn by on-going and proposed neutrino experiments is discussed.
	Slides