ALPHONSE STERLING

• Spicules

• I hope to bring to the workshop BBSO centerline H-alpha data for 1998 June 19, with 1'' pixels and one-minute cadence for the whole day.
• In addition to the H-alpha data, I will also bring Yohkoh SXT data to the workshop.
  As a minimum, these will included processed full-frame and partial frame data from 12 UT - 20 UT on 1998 June 19, and less-complete data for the rest of that day.

• Multi-wavelength manifestations of spicule-like features.
  "Traditional" solar spicules are chromospheric jet-like features. Yet, spicule-like features have also been seen in UV and EUV (e.g., Dere et al. 1983, Karovska et al. 1994; see reviews in Sterling 1998, 2000). Both types of jets tend to occur in the chromospheric network regions, but just how the chromospheric and UV features are related is not known. At the workshop, I hope to be able to compare network brightenings seen in CDS, SUMER, and TRACE, with H-alpha features, and absorption features in TRACE. Most spicules or UV spicules are very small (1'' wide and a few arcsec long), and therefore "true" spicules (whatever that is!) may be difficult to see with CDS, SUMER, and less-than-exceptional H-alpha data. Nonetheless, some network brightenings or "blinkers" could possibly have corresponding "large" or "macro-" spicules. The presence or absence of such a connection, and the specifics of any such connection, could help to differentiate between competing models for the formation of spicules, and other network features.
  In my talk, I will present a model (Sterling et al. 1993) which predicts a connection between brightenings in UV and features in H-alpha, and discuss how I would expect this connection to manifest itself in the data available at the workshop.

• Dere, K. P. et al. 1983, ApJ, 267, L65
• Karovska, M. et al. 1994, ApJ, 428, 854
• Sterling, A. C. et al. 1993, ApJ, 407, 778
• Sterling, A. C. 1998, ApJ, 508, 916
• Sterling, A. C. 2000, Solar Phys., 196, 79

• Working with others, I hope to find (or establish the absence of) correspondences in H-alpha to blinkers, UV microflares, and other brightening phenomena in UV/EUV. I am specifically interested in examining the relative timings between H-alpha and UV/EUV features when both are seen.