From dsmith@apollo.ssl.berkeley.edu Mon Jul 22 12:35:24 2002 Received: from darksun (darksun [128.32.98.218]) by ssl.berkeley.edu (8.11.6+Sun/8.9.3) with SMTP id g6MJZHa13021; Mon, 22 Jul 2002 12:35:17 -0700 (PDT) Message-Id: <200207221935.g6MJZHa13021@ssl.berkeley.edu> Date: Mon, 22 Jul 2002 12:35:16 -0700 (PDT) From: David Smith Reply-To: David Smith Subject: co-Tohban report, 7/22 To: manfred@apollo.ssl.berkeley.edu, rlin@apollo.ssl.berkeley.edu, ghurford@apollo.ssl.berkeley.edu, sharadk@apollo.ssl.berkeley.edu, jimm@apollo.ssl.berkeley.edu, richard.schwartz@gsfc.nasa.gov, Brian.R.Dennis.1@gsfc.nasa.gov, hhudson@apollo.ssl.berkeley.edu, peters@apollo.ssl.berkeley.edu, jloran@ssl.berkeley.edu, lhyatt@uclink.berkeley.edu, ncraig@ssl.berkeley.edu Cc: Alex.Zehnder@psi.ch, Martin.Fivian@psi.ch, cmj@ssl.berkeley.edu, csillag@ssl.berkeley.edu, jfthors@apollo.ssl.berkeley.edu, pjlehr@apollo.ssl.berkeley.edu, ricks@apollo.ssl.berkeley.edu, prh@solen.ssl.berkeley.edu, krucker@ssl.berkeley.edu, markl@apollo.ssl.berkeley.edu, rauch@apollo.ssl.berkeley.edu, dsmith@apollo.ssl.berkeley.edu MIME-Version: 1.0 Content-Type: TEXT/plain; charset=us-ascii Content-MD5: kzcgUZwm24PHEzjfqd6VKQ== X-Mailer: dtmail 1.3.0 @(#)CDE Version 1.4.6_06 SunOS 5.8 sun4u sparc Content-Length: 2064 Status: R co-Tohban report, 7/22/02, David Smith We got excellent coverage of the peak of the X-3 flare on July 20 to make up for missing the rise and peaks of smaller X flares on July 15 and July 18. M flares were seen on July 17 and 18. We skipped about 1/2 day of quiet-Sun data twice to manage memory: Once on July 16 and once on July 21. The thin shutter was put in on the 16th, out on the 18th, and back in on the 19th. On the July 20 flare, once the *thick* attenuator had used up its 5 chopping cycles during the early decline phase of the X3 flare, it went to its default position -- out (the default is in for the thin shutter). This resulted in some very saturated/piled-up data for the rest of the orbit, and probably about an extra 10% of the SSR that we wouldn't otherwise have filled. Hugh Hudson suggested that we might want to reconsider this default. Rear decimation is still occuring at all high magnetic latitude zones regardless of night/day. I have nearly completed an algorithm to identify decimation transitions from quicklook data, which is not 100% reliable but is much faster than taking spectra for every minute of the mission. I will try to get this to Jim and Richard shortly for approval and I will ask Peter Schroeder to help me in applying it to the mission data record to date. On the 17th I lowered the HV on G2 from 2400 to 2000 V to try to lower the rate of arcing and the rate of resets and electronic noise counts -- all three had been recently increasing. The latter two decreased immediately, and we are waiting to see whether the detector is now less likely to arc. Peter Schroeder had noticed that the arcing had after-effects we hadn't seen before: for about 1/2 hour after each arc (there was an average of one per day), the detector efficiency and gain were both considerably lowered. Reminder to the new tohban and the operators: please email me right away when shutter state is changed or decimation changed or memory is skipped, for my event pages, including the time the change takes effect. Thanks, David