Outflows from Clusters of Massive Stars

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Presentation transcript:

Outflows from Clusters of Massive Stars Summary of presentations: Gayley: Thermal vs NT, uniform vs clumpy Beuther: jet mechanism? High vs low mass? Silich: Radiative cooling of winds important Townsley: diffuse vs stellar xray emission Lang: xraydio sources in the GC Arches cluster Law: embedded sources vs external illumination

Outflows from Clusters of Massive Stars 3 types of massive outflows tracing cluster life: Jets from young massive stars Stellar winds from adult O and WR stars SN ejecta with swept up ISM material Focusing on the winds as Xraydio sources: Do CWs always result in both radio and xray? What is the degree of feedback between the two? How does acceleration efficiency affect this? How important is the partitioning of energy (ions vs electrons)?

What’s Important? Investigate roles of: Star formation (single or low mass coalesence, mixture of temperatures) Turbulence (source and dissipation of) Metallicity (effect on winds and cooling) ISM (density, composition, magnetic fields) Magnetic fields (orientation, strength) Radiative cooling (affects scales) Tripod of observation, theory, and simulation seems out of whack: what should the latter two explore?