Introduces a semi-deterministic star sampling method in simulations that derives the instantaneous IMF from current cluster mass using reservoir particles and on-the-fly cluster finding.
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6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
years
2026 6verdicts
UNVERDICTED 6representative citing papers
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
In 37 massive ETGs, the IMF becomes less bottom-heavy with radius, with average α_IMF falling from 2.16 to 1.74 and IMF gradients dominating M/L variations over stellar population effects.
D-CAF simulations show that ongoing gas collapse during star formation shortens stellar crossing times, rendering gas expulsion more adiabatic and thereby regulating the survival and expansion rates of young stellar systems.
Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.
Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.
citing papers explorer
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.