Abstract

Using smoothed particle hydrodynamical simulations (SPH) we investigate the formation of stellar clusters in self-gravitating collapsing turbulent molecular clouds. We mimick star formation by creating N-body particles from gas particles in regions where the the gas density exceeds the Jeans criterion and where the gas flow is convergent.

Shortly after the formation of the first stars, the remaining gas will be expelled by energy feedback of the massive stars, like ionizing radiation, stellar winds or supernova explosions. As a result of this gas expulsion phase some or all stars in the cluster will get unbound. The fraction of finally bound stars is mainly determined by the efficiency of star formation and the timescale of the gas expulsion.

To follow the dynamical evolution of the young cluster during and after the gas expulsion, we simulate the energy feedback by heating up the gas particles surrounding the N-body particles at a constant rate. Star formation stops and the gas is expelled on a short timescale. We present two models with low and high heating rates. The conditions under which a massive globular cluster forms are investigated.

Details

Kategorie: Kugelsternhaufen & Sternentstehung

Weiterlesen: Formation of Globular Clusters in Turbulent Molecular Clouds

Numerische Simulationen zur Entstehung von massereichen Sternhaufen

PhD Thesis (pdf) investigating the formation of massive bound star clusters from turbulent molecular clouds. 

Details

Kategorie: Kugelsternhaufen & Sternentstehung

Weiterlesen: Numerische Simulationen zur Entstehung von massereichen Sternhaufen