1 / 3

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

tybalt
Download Presentation

Outflows from Clusters of Massive Stars

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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?

More Related