Acceleration and propagation in the heliosphere

Heliospheric energetic particles represent a mixture of populations. Sites of original energization of those particles range from solar flares through coronal and interplanetary shocks to distant heliospheric and even galactic sources. Although increasingly sophisticated methods of measuring their energy spectra, composition, charge state, temporal variation and anisotropy help in distinguishing those populations, most studies on particle acceleration and propagation are based on measurements that cannot make such fine distinctions. The lack of clear-cut separation of populations is also reflected in the somewhat ambiguous classification of SH papers in ICRCs. "Solar emissions" and "Galactic cosmic rays in the heliosphere" appear reasonably well separated topics (although Galactic and Anomalous CR could be more appropriate, and space weather as part of the galactic CR topic could be questioned). Acceleration and propagation issues, however, can be only rather artificially separated from the above two. As it happened during this conference, the pre-assigned rapporteur for the "Acceleration and propagation" topic was unable to participate, and the other two rapporteurs for SH topics kindly agreed to report on most papers in the borderline range. Thus we report here only on a relatively small number of papers that could be classified into three general topics: a) Shocks and solar energetic particles; b) Solar energetic particle propagation; c) Radiation environment at Mars.