Abstract
Results of a study of the theoretically predicted and observed X-ray properties of local massive star clusters are presented, with a focus on understanding the mass and energy flow from these clusters into the interstellar medium via a cluster wind. A simple theoretical model, based on the 1985 work of Chevalier & Clegg, is used to predict the theoretical cluster properties, and these are compared to those obtained from recent Chandra observations. The model includes the effect of lower energy transfer efficiency and mass loading. In spite of limited statistics, some general trends are indicated: the observed temperature of the diffuse X-ray emission is lower than that predicted from the stellar mass and energy input rates, but the predicted scaling of X-ray luminosity with cluster parameters is seen. The implications of these results are discussed.
| Original language | English |
|---|---|
| Pages (from-to) | 280-288 |
| Number of pages | 9 |
| Journal | Royal Astronomical Society. Monthly Notices |
| Volume | 339 |
| Issue number | 1 |
| DOIs | |
| Publication status | Published - 1 Feb 2003 |
Keywords
- shock waves
- open clusters and associations : general
- hydrodynamics
- galaxies : star clusters
- stars : winds, outflows