Open AccessVariability in the stellar initial mass function at high mass: coalescence models for starburst clusters
Author(s) -
Shadmehri Mohsen
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.08188.x
Subject(s) - physics , coalescence (physics) , initial mass function , astrophysics , cluster (spacecraft) , fragmentation (computing) , mass segregation , stellar mass , molecular cloud , high mass , star formation , star cluster , astronomy , galaxy , stars , computer science , programming language , operating system
A coalescence model using the observed properties of pre‐stellar condensations (PSCs) shows how an initially steep initial mass function (IMF) that might be characteristic of primordial cloud fragmentation can change into a Salpeter IMF or shallower IMF in a cluster of normal density after one dynamical time, even if the PSCs are collapsing on their own dynamical time. The model suggests that top‐heavy IMFs in some starburst clusters originate with PSC coalescence.