Simon Glover
0000-0001-6708-1317
University of Heidelberg
204 papers found
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Importance of Thermodynamics for Fragmentation and Star Formation
Formation of Stellar Clusters and the Importance of Thermodynamics for Fragmentation
Star Formation at Very Low Metallicity. I. Chemistry and Cooling at Low Densities
Radiative feedback from ionized gas
Star Formation at Very Low Metallicity. II. On the Insignificance of Metal‐Line Cooling During the Early Stages of Gravitational Collapse
Simulating the Formation of Molecular Clouds. II. Rapid Formation from Turbulent Initial Conditions
Simulating the Formation of Molecular Clouds. I. Slow Formation by Gravitational Collapse from Static Initial Conditions
cooling in primordial gas
Assessing the influence of metallicity on fragmentation of proto-galactic gas
Assessing The Influence Of Metallicity On The Fragmentation Of Protogalactic Gas
H3+ Cooling in Primordial Gas
RHD Simulations on the Radiative Feedback from First Stars
Cloud Fragmentation and Proplyd-like Features in HiiRegions Imaged by theHubble Space Telescope
Cosmological Implications of the Uncertainty in H−Destruction Rate Coefficients
The Destruction of Molecular Hydrogen
Cosmological Implications of the Uncertainty in Astrochemical Rate Coefficients
The Lack of Influence of Metallicity on Cooling and Collapse of Ionized Gas in Small Protogalactic Halos
The Formation Of The First Stars In The Universe
Rapid Formation of Molecular Clouds from Turbulent Atomic Gas
Cosmological Implications of the Uncertainties in Astrochemical Rate Coefficients
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