The core mass function in 30Dor-10 is consistent with a Salpeter-like slope, implying that stellar IMF variations in extreme environments result from evolutionary processes rather than initial fragmentation.
The Origin and Universality of the Stellar Initial Mass Function
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abstract
We review current theories for the origin of the Stellar Initial Mass Function (IMF) with particular focus on the extent to which the IMF can be considered universal across various environments. To place the issue in an observational context, we summarize the techniques used to determine the IMF for different stellar populations, the uncertainties affecting the results, and the evidence for systematic departures from universality under extreme circumstances. We next consider theories for the formation of prestellar cores by turbulent fragmentation and the possible impact of various thermal, hydrodynamic and magneto-hydrodynamic instabilities. We address the conversion of prestellar cores into stars and evaluate the roles played by different processes: competitive accretion, dynamical fragmentation, ejection and starvation, filament fragmentation and filamentary accretion flows, disk formation and fragmentation, critical scales imposed by thermodynamics, and magnetic braking. We present explanations for the characteristic shapes of the Present-Day Prestellar Core Mass Function and the IMF and consider what significance can be attached to their apparent similarity. Substantial computational advances have occurred in recent years, and we review the numerical simulations that have been performed to predict the IMF directly and discuss the influence of dynamics, time-dependent phenomena, and initial conditions.
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UNVERDICTED 4representative citing papers
Hydrodynamical simulations of Milky Way-like cluster formation find that most binaries are bound from formation, half are disrupted by the end of the star-formation epoch, and multiple formation accounts for at least 57% of stars.
Across seven molecular clouds the integrated filament linear density function follows a power law with slope 1.30-1.34, matching the Salpeter IMF slope of 1.35.
ALMA survey finds 4 starless cores in Orion B North consistent with turbulent collapse simulations; virial analysis indicates Chamaeleon I cores are less bound with external pressure dominating unlike Orion B North and Ophiuchus.
citing papers explorer
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The fragmentation properties of massive star-forming regions in 30Dor-10 at 2000 au resolution
The core mass function in 30Dor-10 is consistent with a Salpeter-like slope, implying that stellar IMF variations in extreme environments result from evolutionary processes rather than initial fragmentation.
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The bound origin of low-mass stellar binaries
Hydrodynamical simulations of Milky Way-like cluster formation find that most binaries are bound from formation, half are disrupted by the end of the star-formation epoch, and multiple formation accounts for at least 57% of stars.
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A Salpeter-like filament linear density function across nearby molecular clouds
Across seven molecular clouds the integrated filament linear density function follows a power law with slope 1.30-1.34, matching the Salpeter IMF slope of 1.35.
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An ALMA search for substructure and fragmentation in starless cores in Orion B North
ALMA survey finds 4 starless cores in Orion B North consistent with turbulent collapse simulations; virial analysis indicates Chamaeleon I cores are less bound with external pressure dominating unlike Orion B North and Ophiuchus.