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The Fundamental Building Blocks of Galaxies
Pavel Kroupa
Most stars form in compact, dense embedded clusters with memberships ranging from a dozen stars to many millions of stars. Embedded clusters containing more than a few hundred star…
IMF variations and their implications for Supernovae numbers
C. Weidner, P. Kroupa
The stellar initial mass function (IMF) integrated over an entire galaxy is an integral over all separate star-formation events. Since most stars form in star clusters with differe…
How star clusters could survive low star formation efficiencies
M. Fellhauer, P. Kroupa
After the stars of a new, embedded star cluster have formed they blow the remaining gas out of the cluster. Especially winds of high mass stars and definitely the on-set of the fir…
A Formation Scenario for the Heavy-Weight Cluster W3 in NGC 7252
M. Fellhauer, P. Kroupa
The young star cluster W3 (age 300-500 Myr) in NGC 7252 is the most luminous star cluster known to date. Dynamical mass estimates result in 8 +/- 2 * 10^7 M_sun. With an effective…
The Pleiades mass function: models versus observations
E. Moraux, P. Kroupa, J. Bouvier
Two stellar-dynamical models of binary-rich embedded proto-Orion-Nebula-type clusters that evolve to Pleiades-like clusters are studied with an emphasis on comparing the stellar ma…
Implications for the formation of star clusters from extra-galactic star-formation rates
C. Weidner, P. Kroupa, S. S. Larsen
Observations indicate that young massive star clusters in spiral and dwarf galaxies follow a relation between luminosity of the brightest young cluster and the star-formation rate…