First campaign scheduled for November 8-13, 2003.
Hugh Hudson (
hhudson@ssl.berkeley.edu)
will be the campaign coordinator.
| TITLE: | RHESSI/TRACE Micro-Events |
| AUTHORS: | Sam Krucker (
krucker@ssl.berkeley.edu)
RHESSI/Berkeley
Bob Lin (boblin@ssl.berkeley.edu) RHESSI/Berkeley Karel Schrijver (schrijver@lmsal.com) TRACE/LMSAL |
| VERSION: | 7 November 2003 |
| CONTACT | Hugh Hudson (Campaign Coordinator for November 2003 run) |
| SUMMARY: | Microflares or nanoflares are often cited as a mechanism for coronal heating. RHESSI and TRACE are providing the most sensitive hard X-ray observations and highest-resolution EUV observations, respectively, and can explore this suggestion. We do not think that microflares as such, ie those following flare statistics, can do the job; however "micro-events" (Benz & Krucker, ApJ 568, 413, 2002) might represent the long-sought nanoflare contribution envisaged by Parker (cf Katsukawa and Tsuneta, ApJ 557, 343, 2001). |
| SOLIS VSM | Contact: Christoph Keller NSO |
| SUMMARY | SOLIS VSM will make observations (magnetograms in the photosphere and the chromosphere, photospheric vector field measurements, and He10830A intensity spectra) with about two minutes cadence following the TRACE field of view. |
| TRACE | Contact: Karel Schrijver LMSAL |
| SUMMARY | TRACE will observe at angular coordinates (0, 200) (heliographic N00W12), ie just W of disk center on the quiet Sun. |
| RHESSI | Contact: Hugh Hudson , UC Berkeley |
| SUMMARY | RHESSI observes the whole Sun continuously, with the exception of normal gaps for SAA passages and orbit night. Please see the predicted ephemeris for details. During this campaign the thin shutter will be out to the maximum extent, implying the best possible low-energy observations. |