Tuesday, September 17, 14:00-18:30
Nicola Schneider (I. Physik. Institut, University of Cologne)
Hans Zinnecker (ex-DSI, University of Stuttgart, retired DSI guest/visitor)
Alfred Krabbe (DSI)
Maja Kaźmierczak-Barthel (DSI)
Massive stars play a key role in the evolution of the interstellar medium (ISM) in galaxies. They "stir" the ISM through various processes such as ionization, stellar winds, radiation pressure, and finally supernova explosions. This mechanical and radiative feedback of massive stars on their environment regulates the physical conditions of the ISM, sets its emission characteristics, and ultimately governs the star formation activity through negative (molecular cloud destruction) and positive (cloud compression) feedback. Understanding the physical processes that regulate the impact of massive stars on their environment is thus a key question in modern astrophysics.
Significant observational progress has been achieved during the last decade in particular by submm/(far)-infrared facilities such as Spitzer, Herschel, ALMA, IRAM, SOFIA, and many others. For example, accretion and ejection processes involved in protostellar evolution have been investigated, the ubiquity of Galactic and extragalactic HII-region bubbles was revealed, and spectroscopy of mm- to FIR-lines of CO, of (ionized) carbon, and (neutral) oxygen, helped to better understand the gas cooling of the ISM. In parallel, increasingly more complex simulations and theoretical studies allowed us to advance our understanding of molecular cloud formation and star formation.
We here propose a splinter meeting with the aim of summarizing our current observational and theoretical understanding of feedback effects in the ISM. Individual aspects and current topical projects will be highlighted by presentations of experts in the field. The objective is to stimulate discussions within the community of observers and modelers.
Some key questions that will be addressed are:
- How can we translate our observations into diagnostics of ISM parameters such gas
density, gas temperature, strength of UV-field, etc. and what is the best way to compare
- Which improvements are needed for PDR- and shock-modelling (time dependence,
dynamics,..) to better explain the observations?
- Which are the dominant feedback processes, including shocks, in various regions? - What about diagnostics for triggered star formation, cluster formation?
- What about evidence for protocluster collapse? protostellar accretion bursts?
14:00 - 14:15 Introduction talk (Hans Zinnecker, Santiago)
14:20 - 14:40 (invited) Bubbles and Feedback (Xander Tielens, Leiden/Maryland)
14:45 - 15:05 (invited) Massive SF: observations (Henrik Beuther, Heidelberg)
15:10 - 15:40 Coffee break
Session: "Comparing observations and modelling: where do we stand and where do we need to go?"
15:40 - 16:00 (invited) PDR modelling (Markus Roellig, Cologne)
16:05 - 16:25 (invited) Shock modelling (Antoine Gusdorf, Paris)
16:30 - 16:50 (invited) Synthetic observations (Daniel Seifried, Cologne)
16:55 - 17:15 (invited) Accretion and feedback in high-mass SF regions (Rolf Kuiper Tuebingen)
17:20 - 17:30 short presentation
17:30 - 17:40 short presentation
17:40 - 17:50 short presentation
17:50 - 18:00 short presentation
18:00 - 18:30 summary and discussion (Moderators N. Schneider & H. Zinnecker)
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