Vadim Semenov

34 papers · 14 first-author · 8 led by students · 20 h-index · 1200+ citations · (based on ADS metrics, April 2026)

First author:

• Semenov 2026ApJ accepted · arXiv:2602.04950 · ADS
  How Do Disk Galaxies Form?
• Semenov, Conroy, Hernquist 2025ApJ 989, 219 · arXiv:2410.09205 · ADS
  From UV-bright Galaxies to Early Disks: the Importance of Turbulent Star Formation in the Early Universe
• Semenov, Conroy, Smith, Puchwein, Hernquist 2025ApJ 990, 7 · arXiv:2409.18173 · ADS
  How Early Could the Milky Way’s Disk Form?
• Semenov 2025ApJS 281, 37 · arXiv:2410.23339 · ADS
  Capturing Turbulence with Numerical Dissipation: a Simple Dynamical Model for Unresolved Turbulence in Hydrodynamic Simulations
• Semenov, Conroy, Chandra, Hernquist, Nelson 2024ApJ 962, 84 · arXiv:2306.09398 · ADS
  Formation of Galactic Disks I: Why did the Milky Way’s Disk Form Unusually Early?
• Semenov, Conroy, Chandra, Hernquist, Nelson 2024ApJ 972, 73 · arXiv:2306.13125 · ADS
  Formation of Galactic Disks II: the Physical Drivers of Disk Spin-up
• Semenov, Kravtsov, Diemer 2022ApJS 261, 16 · arXiv:2107.14240 · ADS
  Entropy-Conserving Scheme for Modeling Nonthermal Energies in Fluid Dynamics Simulations
• Semenov, Kravtsov, Gnedin 2021ApJ 918, 13 · arXiv:2103.13406 · ADS
  Spatial Decorrelation of Young Stars and Dense Gas as a Probe of the Star Formation–Feedback Cycle in Galaxies
• Semenov, Kravtsov, Caprioli 2021ApJ 910, 126 · arXiv:2012.01427 · ADS
  Cosmic Ray Diffusion Suppression in Star-Forming Regions Inhibits Clump Formation in Gas-Rich Galaxies
• Semenov, Kravtsov, Gnedin 2019ApJ 870, 79 · arXiv:1809.07328
  What Sets the Slope of the Molecular Kennicutt–Schmidt Relation?
• Semenov, Kravtsov, Gnedin 2018ApJ 861, 4 · arXiv:1803.00007
  How Galaxies Form Stars: the Connection between Local and Global Star Formation in Galaxy Simulations
• Semenov, Kravtsov, Gnedin 2017ApJ 845, 133 · arXiv:1704.04239
  The Physical Origin of Long Gas Depletion Times in Galaxies
• Semenov, Kravtsov, Gnedin 2016ApJ 826, 200 · arXiv:1512.03101
  Nonuniversal Star Formation Efficiency in Turbulent ISM
• Semenov 2013Astronomy Reports 57, 485 · ADS
  Statistical Analysis of the Large-Scale Structure of the Universe Using Observational Data and Numerical Modeling

Led by co-advised students:

• Kocjan, Semenov 2026ApJ 1007, 46 · arXiv:2602.02657 · ADS
  The Rhythm of the ISM: Tracing the Timescales of Gas Evolution and Star Formation across Galactic Environments
• Konietzka, Connor, Semenov, Beane, Springel, Hernquist 2025ApJ accepted · arXiv:2507.07090 · ADS
  Ray-tracing Fast Radio Bursts Through IllustrisTNG: Cosmological Dispersion Measures from Redshift 0 to 5.5
• Polzin, Kravtsov, Semenov, Gnedin 2024OJAp 7, 114 · arXiv:2407.11125 · ADS
  On the Universality of Star Formation Efficiency in Galaxies
• Polzin, Kravtsov, Semenov, Gnedin 2024ApJ 966, 172 · arXiv:2310.10712 · ADS
  Modeling Molecular Hydrogen in Low Metallicity Galaxies
• Chandra, Semenov, Rix, Conroy, Bonaca, Naidu, Andrae, Li, Hernquist 2024ApJ 972, 112 · arXiv:2310.13050 · ADS
  The Three-Phase Evolution of the Milky Way
• Han, Semenov, Conroy, Hernquist 2023ApJL 954, L24 · arXiv:2309.07208 · ADS
  Tilted Dark Halos are Common, Long-Lived, and Can Warp Galactic Disks
• Appel, Burkhart, Semenov, Federrath, Rosen, Tan 2023ApJ 954, 93 · arXiv:2301.07723 · ADS
  What Sets the Star Formation Rate of Molecular Clouds? The Density Distribution as a Fingerprint of Compression and Expansion Rates
• Appel, Burkhart, Semenov, Federrath, Rosen 2022ApJ 927, 75 · arXiv:2109.13271 · ADS
  The Effects of Magnetic Fields and Outflow Feedback on the Shape and Evolution of the Density PDF in Turbulent Star-Forming Clouds

In collaboration:

• Wheeler, Kravtsov, Chiti, Katz, Semenov 2025OJAp 8, 151 · arXiv:2507.03182 · ADS
  What Sets the Metallicity of Ultra-Faint Dwarfs?
• Segovia Otero, Agertz, Renaud, Kraljic, Romeo, Semenov 2025MNRAS 538, 2646 · arXiv:2410.08266 · ADS
  Cosmic evolution of the star formation efficiency in Milky Way-like galaxies
• Robinson, Avestruz, Gnedin, Semenov 2024OJAp subm. · arXiv:2412.15324 · ADS
  The effects of different cooling and heating function models on a simulated analog of NGC300
• Beane, Johnson, Semenov, Hernquist, Chandra, Conroy 2025ApJ 985, 221 · arXiv:2410.21580 · ADS
  Rising from the Ashes II: The Bar-driven Abundance Bimodality of the Milky Way
• Aung, Mandelker, Dekel, Semenov, van den Bosch 2024MNRAS 532, 2965 · arXiv:2403.00912 · ADS
  Entrainment of Hot Gas into Cold Streams: The Origin of Excessive Star-formation Rates at Cosmic Noon
• Kiihne, Appel, Burkhart, Semenov, Federrath 2025ApJ 979, 89 · arXiv:2305.11218 · ADS
  Fitting Probability Distribution Functions in Turbulent Star-Forming Molecular Clouds
• Jeffreson, Semenov, Krumholz 2023MNRAS 527, 7093 · arXiv:2301.10251 · ADS
  Clouds of Theseus: Long-lived Molecular Clouds are Composed of Short-lived H2 Molecules
• Shin, Tacchella, Kim, Iyer, Semenov 2023ApJ 947, 61 · arXiv:2211.01922 · ADS
  Star Formation Variability as a Probe for the Baryon Cycle within Galaxies
• Bialy, Zucker, Goodman, Foley, Alves, Semenov, Benjamin, Leike, Enßlin 2021ApJL 919, L5 · arXiv:2109.09763
  The Per-Tau Shell: A Giant Star-forming Spherical Shell Revealed by 3D Dust Observations
• Gnedin, Semenov, Kravtsov 2018JCoPh 359, 93 · arXiv:1801.03108
  Enforcing the Courant–Friedrichs–Lewy Condition in Explicitly Conservative Local Time Stepping Schemes
• Li, Gnedin, Gnedin, Meng, Semenov, Kravtsov 2017ApJ 834, 69 · arXiv:1608.03244
  Star Cluster Formation in Cosmological Simulations. I. Properties of Young Clusters
• Kim et al. (AGORA Collaboration) 2016ApJ 833, 202 · arXiv:1610.03066
  The AGORA High-resolution Galaxy Simulations Comparison Project. II. Isolated Disk Test