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.
Title resolution pending
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
-
Individual Star Sampling in Star Formation Simulations: A Semi-Deterministic Model
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.
-
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%.
-
The MASSIVE SURVEY XXI: Local Variations in the Stellar Initial Mass Function of MASSIVE Early-Type Galaxies
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.
-
Dynamical Cluster Assembly Framework (D-CAF): The Link Between Star Cluster Formation and Expansion Rates
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.
-
Centrally concentrated star formation in young clusters II: Jet feedback
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.
-
Getting to know the Stellar Clusters in NGC 1569: Bayesian inference of stellar cluster properties in a dwarf starburst galaxy
Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.