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Wolf‐Rayet Phenomena in Massive Stars and Starburst Galaxies: IAU Symposium 193

The international hot star community organized IAU Symposium 193 at the Camino Real Hotel in Puerto Vallarta as part of their continuing series of “beach symposia.” There was very active participation from astronomers from Mexico, who hosted the conference; 186 individuals attended from 24 countries, and 54 oral papers and 130 posters were presented. The weather was warm and sunny, the surroundings peaceful, and informal discussions occurred while dining, drinking, and sitting on the beach. The poster sessions colocated with the meeting rooms were particularly well attended and remained up for the entire conference. This summary is a personal appraisal, one which might well be very different in the hands of another reporter. W-R phenomena as strong broad emission lines were first identified in stars in 1867. We now know that this is due to intense stellar winds. W-R stars are initially high-mass, very luminous objects that are undergoing processes that result in a great deal of mass loss, much of which is currently observable. Models for single-star evolution with extensive mass loss indicate that the anomalous composition of W-R stars (subtypes: WN, nitrogenand helium-rich; WC, heliumand carbon-rich) is a result of core burning products being present at the stellar “surface” owing to previous mass loss and/or mixing. Starburst galaxies are those systems in which strong (narrow) nebular recombination lines are seen, indicating the presence of a large number of hot exciting stars, mostly of type O. Those starburst galaxies with broad emission lines in the integrated spectrum from W-R stars are referred to as W-R galaxies. Roughly 70% of the Symposium was devoted to issues concerned with W-R stars; the remainder, to that of galaxies. It is a measure of the explosion of studies in the past few years in this field that this was by far the best attended “hot star” Symposium and one in which there was a substantial interaction between astrophysicists with “stellar” and “galaxy” backgrounds. The imminent publication of new catalogs of W-R stars in the Galaxy and Magellanic Clouds was announced; the census amounts to 211 stars in the former, 132 in the LMC, and nine in the SMC. An analysis of the W-R populations of the other Local Group galaxies was given. A new catalog of W-R galaxies lists 126 members, indicating a doubling time of 3.5 yr since the initial serendipitous discovery in 1976. W-R stars radiate from the X-ray to radio region, which is, from the UV