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Jeong-Gyu Kim (Seoul National University)21/10/2013, 09:00PosterThe neutral component of the interstellar medium (ISM) is segregated into the cold neutral medium (CNM) and warm neutral medium (WNM) as a result of thermal instability. It was found that the CNM--WNM evaporation interface, across which the CNM undergoes thermal expansion, is linearly unstable to corrugational disturbances, in complete analogy with the Darrieus-Landau instability (DLI)...Go to contribution page
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Jonathan Heiner (CRyA, UNAM Morelia)21/10/2013, 09:00PosterCold, self-absorbing atomic hydrogen can be seen as absorption features in the broader HI profile. However, unless emission of molecular gas (typically CO) at the same velocity as the absorption feature is detected, it is not always possible to distinguish between self-absorption and the lack of HI emission. Ideally one would want to dispense with the need to detect molecular emission, since...Go to contribution page
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Jonathan Smoker (European Southern Observatory (VLT))21/10/2013, 09:00PosterWe describe a search for tiny-scale structure in the interstellar medium using archive twin-epoch measurements of resolution 42,000 and 120,000 towards hundreds of stars. Our aim is to discover more examples of time-variation in the interstellar medium and determine if they can be explained by varying physical conditions, the statistical properties of the ISM, or by ""real"" structures such as...Go to contribution page
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21/10/2013, 09:00PosterWe present a suite of simulations of a vertical stratified box with extents of +- 20 kpc and a footprint of 1 kpc^2 including self-gravity, supernova feedback, magnetic fields and a resolution of 2pc. We are able to resolve the ISM structure in the disk midplane and follow SN ejecta using tracer particles based on an Monte-Carlo advection scheme. The large vertical extents allow us to follow...Go to contribution page
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Catherine McEvoy (Queen's University Belfast)21/10/2013, 09:00PosterThe tiny scale structure (from 1 AU to 1 pc) of the ISM is generally poorly understood. High resolution optical spectroscopic observations, both new and archival, have been used to delve into this tiny structure to see just how ubiquitous it is and to try to understand what causes such variation to occur. Interstellar absorption lines from a selection of 96 O and B type stars spectra,...Go to contribution page
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Simon Bihr (Max Planck Institute for Astronomy)21/10/2013, 09:00PosterHow do molecular clouds form from the diffuse atomic interstellar medium? To address this and further questions we are conducting the THOR survey, a galactic plane survey (l = 15 to 60dec and b = -1 to +1dec) of the 21cm HI line, four OH lines, and 20 recombination lines as well as the continuum from 1 to 2 GHz at a spatial resolution of ~20arcsec. We got granted 110 hours at the VLA in...Go to contribution page
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Norbert S. Schulz (MIT)21/10/2013, 09:00PosterThe interstellar medium (ISM) absorbs and scatters X-rays and its signatures can be used to diagnose its states of matter, compositions, and dynamical properties. With the availability of precision X-ray optics and spectrometers as onboard the Chandra X-ray Observatory, scattering halos around bright X-ray sources and K/L shell X-ray absorption are now observed and masured in detail....Go to contribution page
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