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Outflows from Clusters of Massive Stars

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

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Outflows from Clusters of Massive Stars

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  1. 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

  2. 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)?

  3. 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?

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