Soňa Ehlerová

THE FORMATION OF SECONDARY STELLAR GENERATIONS IN MASSIVE YOUNG STAR CLUSTERS FROM RAPIDLY COOLING SHOCKED STELLAR WINDS

We study a model of rapidly cooling shocked stellar winds in young massive clusters and estimate the circumstances under which secondary star formation, out of the reinserted winds from a first stellar generation (1G), is possible. We have used two implementations of the model: a highly idealized computationally inexpensive spherically symmetric semi-analytic model, and a complex three-dimensional radiation-hydrodynamic simulations, and they are in a good mutual agreement. The results confirm our previous findings that in a cluster with 1G mass

Supershells: origin, evolution and fragmentation

10^7

Gould’s Belt

M

HI Shells in the Leiden-Dwingeloo HI Survey

_\odot

Gould's Belt: Local Large Scale Structure in the Milky Way

and half-mass radius

Bimodal regime in young massive clusters leading to subsequent stellar generations

2.38

The triggered star formation in rotating disks

pc, the shocked stellar winds become thermally unstable, collapse into dense gaseous structures that partially accumulate inside the cluster, self-shield against ionizing stellar radiation and form the second generation (2G) of stars. We have used the semi-analytic model to explore a subset of the parameter space covering a wide range of the observationally poorly constrained parameters: the heating efficiency,

How to Interpret the Bubble-Dominated ISM in the LMC?

\eta_\mathrm{he}

Self-shielding clumps in starburst clusters

, and the mass loading,

An automatic identification of HI shells in the 2nd and 3rd Galactic Quadrants

\eta_\mathrm{ml}