REPORT FROM ISAS 8-OCTOBER-1992 L. Acton SCIENCE & PUBLICATIONS On 30 September and 1 and 2 October an informal workshop was held at NAOJ-Mitaka on the subject ONE YEAR OF YOHKOH RESEARCH -What have we learned from the YOHKOH observation?- -What should (can) we do from now?- It is highly gratifying to learn of the large amount of quality science that is being stimulated by the new data from Yohkoh, the Nobeyma Radioheliograph and the various ground based observatories involved in this cooperative program. In particular, new results reported by Yoshimori and Kawabata on observations of the 15-November-91 flare by the Yohkoh Gamma Ray Spectrometer were extremely interesting. By comparing the time profile of the positron annihilation line at 511 keV and the prompt nuclear gamma ray lines at 4-7 MeV they are able to conclude for the largest gamma ray burst at 2238 UT that the high energy protons are mirroring quite high up where the density is about 10^13. I'm tremendously relieved to report the the SCIENCE paper and cover illustration have at last been accepted for publication in the the 23 October issue which is devoted to Science in Japan. I returned the galley proofs last night. The issue of Publications of the Astronomical Society of Japan which include the 30 initial papers will also be published in October as volume 43. SXT OPERATIONS The SXT continues to operate normally. We undertook to support the cooperative observint campaign "PHOTOSPHERIC AND CHROMOSPHERIC STUDIES OF SOLAR ACTIVITY AND FLARES" which was organized by Roberto Falciani and took place on 25-Sept to 7-Oct-92. Unfortunately, the sun was very quiet during this period so that the primary objectives of the observing were not achieved. In order to try to get better observations of the kind of small events that are prevalent now we have changed the Partial Frame sequence to observe a small (2.6'x2.6') field of view with a time resolution of 8 seconds and with an ARS1 pointing update every minute. This is a completely new observing philosophy as heretofore we updated pointing at most once per orbit and in the ARS2 mode forced the SXT PFI to follow the same active region. Although the region does dance around quite a lot it does appear that these data will be of value in studying transient brightenings in active regions with better time resolution than before. We also prepared and ran a FFI table concentrating on long quarter resolution images through all filters in support of coronal green, red, and yellow line observations from Norikura Coronagraph Station. The scientific objective here is to determine better emission measure models of coronal structures by combining the Norikura and SXT data. We have prepared a deep exposure table through all filters at quarter resolution for another 18' offpoint experiment to the east to observe the high corona. This experiment may be run for one KSC orbit within the next few days if activity remains low. We have also defined an x-ray bright point experiment to be run in cooperation with Kitt Peak on 19 and 20 October. In this case the quiet corona target will be selected by Karen Harvey and followed for 2 orbits (3 hours) on each day. The objective here is to obtain better time resolution and exposure on x-ray bright points than is provided by the standard SXT operating sequences. At the request of H. Hara the exposure of the AlMg exposures in the standard FFI table have been doubled to provide equivalent statistics in Al.1 and AlMg for temperature studies. Appropriate dark frames have been acquired. CADRE Presently the following U-side SXT persons are at ISAS. Loren Acton Sam Freeland Hugh Hudson Piet Martens Nariaki Nitta Acton will spend 3 weeks at the University of Hawaii beginning on 24 October 1992. He and Hudson will attend the Hawaii workshop on the 24-Oct-91 and 15-Nov-91 flares on 3-5 November.