REVIEW 9 cited by
The initial mass function of stars
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
The initial mass function (IMF) is one of the most important functions in astrophysics because it is key to reconstructing the cosmological matter cycle, understanding the formation of super-massive black holes, and deciphering the light from high-redshift observations. The IMF's dependency on the physical conditions of the gas and its connection to the galaxy-wide IMF connects the molecular clumps to the cosmological scale. The extraction of the IMF from observational data requires a thorough understanding of stellar evolution, the time-dependent stellar multiplicity, the stellar-dynamical evolution of dense stellar populations, and the structures, star formation histories, and chemical enrichment histories of galaxies. The IMF in galaxies, referred to as the galaxy-wide IMF (gwIMF), and the IMF in individual star-forming regions (the stellar IMF) need not be the same, although the former must be related to the latter. Observational surveys inform on whether star-forming regions provide evidence for the stellar IMF being a probability density distribution function. They may also indicate star formation to optimally follow an IMF shaped by the physical conditions of the star-forming gas. Both theoretical and observational evidence suggest a relationship between the initial mass function of brown dwarfs and that of stars. Late-type stars may arise from feedback-regulated fragmentation of molecular cloud filaments, which build up embedded clusters. In contrast, early-type stars form under more violent accretion and feedback-regulated conditions near the centers of these clusters. The integration over all star-forming molecular cloud clumps and their stellar IMFs in a galaxy via the IGIMF theory yields its gwIMF which sensitively depends on the physical properties of the molecular cloud clumps and the range of their masses that depends on the SFR of the galaxy.
Forward citations
Cited by 9 Pith papers
-
The Influence of Dust Composition on Accretion Outbursts
Using 1D simulations with dust evaporation and condensation, the paper shows that dead-zone accretion outbursts vaporize dust out to about 0.5 au and that higher dust sublimation temperatures produce stronger but less...
-
The initial conditions and initial mass functions of Alpha Persei, Pleiades and Praesepe
For Alpha Persei, the Pleiades, and Praesepe, the initial mass function is top-light (α_high ≈ 2.98 ± 0.22) and shows possible cluster-to-cluster scatter, based on Gaia DR3 plus N-body emulator inference.
-
Baryonic mass budgets in the central regions of the Bullet Cluster and their consistency with strong lensing in MOND
MOND strong-lensing masses in the Bullet Cluster’s three BCG cores lie between lower and upper IGIMF baryonic mass estimates from JWST photometry.
-
A method for constructing the joint mass function of binary stars
A Fredholm integral equation lets you construct the joint mass distribution of binary-star primary and secondary masses for arbitrary pairing rules, solving the previously open uniform-pairing case.
-
The Corona-Australis star-forming region: New insights on its formation history from detailed stellar and disk analysis
The Corona Australis complex formed through two supernova-triggered star formation episodes, the second of which may have produced the nearby pulsar RX J1856.5-3754.
-
The effect of the environment-dependent stellar initial mass function on the baryonic Tully Fisher relation
Model galaxies with a variable stellar IMF and the MOND relation reproduce the observed high-mass deviation of the baryonic Tully-Fisher relation.
-
Effect of Galactic Chemical Evolution on Exoplanet Properties
Planets that formed early in the Galaxy have less iron in their building blocks, so they end up with smaller cores and lower densities than planets formed later.
-
The impact of the formation channel on gravitational-wave-galaxy cross-correlations
GW-galaxy cross-correlation forecasts depend strongly on the assumed binary time-delay distribution but barely on the mass-transfer prescription, with detections predicted only for long delays against shallow surveys.
-
Are binary-star populations regionally different? --in memory of Sverre Aarseth--
A review arguing that stars form mostly as binaries and that cluster dynamics, not star formation conditions, explains most observed differences in binary populations.
Discussion (0). Continue with ORCID to comment.