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Control of star formation by supersonic turbulence
Understanding the formation of stars in galaxies is central to much of modern astrophysics. However, a quantitative prediction of the star formation rate and the initial distribution of stellar…
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Comparing the statistics of interstellar turbulence in simulations and observations - Solenoidal versus compressive turbulence forcing
Context. Molecular clouds (MCs) exhibit supersonic turbulent velocity and density fluctuations on virtually all scales observed by modern telescopes. The origin and structural characteristics of this…
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Kinetic Energy Decay Rates of Supersonic and Super-Alfvénic Turbulence in Star-Forming Clouds
We compute 3D models of supersonic, sub-Alfvenic, and super-Alfvenic decaying turbulence, with an isothermal equation of state appropriate for star-forming interstellar clouds of molecular gas. We…
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THE STAR FORMATION RATE OF TURBULENT MAGNETIZED CLOUDS: COMPARING THEORY, SIMULATIONS, AND OBSERVATIONS
The role of turbulence and magnetic fields is studied for star formation in molecular clouds. We derive and compare six theoretical models for the star formation rate (SFR)—the Krumholz & McKee (KM),…
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Analyzing Inverse Problems with Invertible Neural Networks
TLDR
It is argued that a particular class of neural networks is well suited for this task -- so-called Invertible Neural Networks (INNs), and it is verified experimentally that INNs are a powerful analysis tool to find multi-modalities in parameter space, to uncover parameter correlations, and to identify unrecoverable parameters.
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The Density Probability Distribution in Compressible Isothermal Turbulence: Solenoidal versus Compressive Forcing
The probability density function (PDF) of the gas density in turbulent supersonic flows is investigated with high-resolution numerical simulations. In a systematic study, we compare the density…
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ON THE STAR FORMATION EFFICIENCY OF TURBULENT MAGNETIZED CLOUDS
We study the star formation efficiency (SFE) in simulations and observations of turbulent, magnetized, molecular clouds. We find that the probability density functions (PDFs) of the density and the…
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SIMULATIONS ON A MOVING MESH: THE CLUSTERED FORMATION OF POPULATION III PROTOSTARS
The cosmic dark ages ended a few hundred million years after the big bang, when the first stars began to fill the universe with new light. It has generally been argued that these stars formed in…
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Modelling CO formation in the turbulent interstellar medium
We present results from high-resolution three-dimensional simulations of turbulent interstellar gas that self-consistently follow its coupled thermal, chemical and dynamical evolution, with a…
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TOPoS - II. On the bimodality of carbon abundance in CEMP stars Implications on the early chemical evolution of galaxies
Context. In the course of the TOPoS (Turn Off Primordial Stars) survey, aimed at discovering the lowest metallicity stars, we have found several carbon-enhanced metal-poor (CEMP) stars. These stars…
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