The ionization of the the Local Interstellar Cloud (LIC) is quite unusual compared with most warm (T ~ 104 K) interstellar gas. Hydrogen and helium are both partially ionized with helium surprisingly more ionized than hydrogen. Directly observed ionization sources including nearby stellar EUV sources and the diffuse emission of the Soft X-ray Background (SXRB), do not provide enough ionization and heating to account for both the ionization state and temperature of the LIC. We propose that an evaporative boundary between the LIC and the hot gas of the Local Bubble can provide the necessary ionizing radiation. Results of detailed models of the emission from the interface are presented and shown to be adequate to explain the observations.

At the end of the regularly scheduled conference, the organizers made available a large sunny conference room for the remaining participants to continue discussion. The main topics were the structure of the Local Bubble and the properties of the Galactic X-ray halo. Here we try to summarize the main points of those discussions.

The properties of the Local Bubble, Local Fluff complex of nearby interstellar clouds, and the heliosphere are mutually constrained by data and theory. Observations and models of the diffuse radiation field, interstellar ionization, pickup ion and anomalous cosmic-ray populations, and interstellar dust link the physics of these regions. The differences between the one-asymmetric-superbubble and twosuperbubble views of the Local Bubble are discussed.

During this workshop, a considerable amount of data was presented, some refined versions of earlier results and some entirely new. While no completely definite picture of the local interstellar medium can be presented yet, some general conclusions can be drawn. We attempt to draw together the most relevant data in Section III. Some new UV results are collated with published results to help state the physical properties of the gas. A morphological view of the local medium is given in Section III. We confine ourselves to the region within 100 pc with the caveat that the distance of much of the material under discussion is poorly known.