Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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The Initial Mass Function of Stars: Evidence for Uniformity in Variable Systems
12 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The distribution of stellar masses that form in one star-formation event in a given volume of space is called the initial mass function (IMF). The IMF has been estimated from low-mass brown dwarfs to very massive stars. Combining IMF estimates for different populations in which the stars can be observed individually unveils an extraordinary uniformity of the IMF. This general insight appears to hold for populations including present-day star formation in small molecular clouds, rich and dense massive star-clusters forming in giant clouds, through to ancient and metal-poor exotic stellar populations that may be dominated by dark matter. This apparent universality of the IMF is a challenge for star formation theory because elementary considerations suggest that the IMF ought to systematically vary with star-forming conditions.
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JWST/MIRI detects [Ne V] 14.3 micron emission from O-star winds in 5 of 22 observed stars, enabling wind speed and mass-loss rate estimates even in weak-wind regimes.
Simultaneous measurement of low- and high-mass IMF slopes in 214 star-forming galaxies reveals diversity, weak correlation between ends, and links to stellar mass, star formation rate, and metallicity.
FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.
Machine learning regressors trained on Rapster simulations forecast that globular clusters rarely host black holes above 100 solar masses while a few nuclear star clusters may exceed this threshold.
PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p
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.
Lumina runs a 500 cMpc radiation-hydrodynamic simulation combining IllustrisTNG galaxy formation with six-bin M1 radiation transport to predict late stellar-driven HI reionization ending around z=4.75 and AGN-driven HeII reionization nearly complete by z=3.
Models apsidal precession and dynamical friction from extended matter to extend GRAVITY constraints on boson clouds around Sgr A* and assess impacts on S-star orbits.
Five of seven modeled M31 dwarf spheroidals show anomalously low central DM densities at 150 pc, with star formation heating disfavored as the sole cause.
Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.
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Predicting intermediate-mass black hole formation in star clusters with machine learning
Machine learning regressors trained on Rapster simulations forecast that globular clusters rarely host black holes above 100 solar masses while a few nuclear star clusters may exceed this threshold.