๐ Simulating galaxy formation with the IllustrisTNG model
Quicklook:
Pillepich, Annalisa et al. (2018) ยท Monthly Notices of the Royal Astronomical Society
Reads: 526 ยท Citations: 1936
DOI: 10.1093/mnras/stx2656
๐ https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.4077P/abstract
#Astronomy #Astrophysics #Cosmology #MethodsNumerical #GalaxiesEvolution
Simulating galaxy formation with the IllustrisTNG model
We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The overall framework builds upon the successes of the Illustris galaxy formation model, and includes prescriptions for star formation, stellar evolution, chemical enrichment, primordial and metal-line cooling of the gas, stellar feedback with galactic outflows, and black hole formation, growth and multimode feedback. In this paper, we give a comprehensive description of the physical and numerical advances that form the core of the IllustrisTNG (The Next Generation) framework. We focus on the revised implementation of the galactic winds, of which we modify the directionality, velocity, thermal content and energy scalings, and explore its effects on the galaxy population. As described in earlier works, the model also includes a new black-hole-driven kinetic feedback at low accretion rates, magnetohydrodynamics and improvements to the numerical scheme. Using a suite of (25 Mpc h<SUP>-1</SUP>)<SUP>3</SUP> cosmological boxes, we assess the outcome of the new model at our fiducial resolution. The presence of a self-consistently amplified magnetic field is shown to have an important impact on the stellar content of 10<SUP>12</SUP> M<SUB>โ</SUB> haloes and above. Finally, we demonstrate that the new galactic winds promise to solve key problems identified in Illustris in matching observational constraints and affecting the stellar content and sizes of the low-mass end of the galaxy population.
๐ Modules for Experiments in Stellar Astrophysics (MESA)
Quicklook:
Paxton, Bill et al. (2011) ยท The Astrophysical Journal Supplement Series
Reads: 482 ยท Citations: 4139
DOI: 10.1088/0067-0049/192/1/3
๐ https://ui.adsabs.harvard.edu/abs/2011ApJS..192....3P/abstract
#Astronomy #Astrophysics #SolarPhysics #MethodsNumerical #StarsEvolution
Modules for Experiments in Stellar Astrophysics (MESA)
Stellar physics and evolution calculations enable a broad range of research in astrophysics. Modules for Experiments in Stellar Astrophysics (MESA) is a suite of open source, robust, efficient, thread-safe libraries for a wide range of applications in computational stellar astrophysics. A one-dimensional stellar evolution module, MESAstar, combines many of the numerical and physics modules for simulations of a wide range of stellar evolution scenarios ranging from very low mass to massive stars, including advanced evolutionary phases. MESAstar solves the fully coupled structure and composition equations simultaneously. It uses adaptive mesh refinement and sophisticated timestep controls, and supports shared memory parallelism based on OpenMP. State-of-the-art modules provide equation of state, opacity, nuclear reaction rates, element diffusion data, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own explicitly defined public interface to facilitate independent development. Several detailed examples indicate the extensive verification and testing that is continuously performed and demonstrate the wide range of capabilities that MESA possesses. These examples include evolutionary tracks of very low mass stars, brown dwarfs, and gas giant planets to very old ages; the complete evolutionary track of a 1 M <SUB>sun</SUB> star from the pre-main sequence (PMS) to a cooling white dwarf; the solar sound speed profile; the evolution of intermediate-mass stars through the He-core burning phase and thermal pulses on the He-shell burning asymptotic giant branch phase; the interior structure of slowly pulsating B Stars and Beta Cepheids; the complete evolutionary tracks of massive stars from the PMS to the onset of core collapse; mass transfer from stars undergoing Roche lobe overflow; and the evolution of helium accretion onto a neutron star. MESA can be downloaded from the project Web site (<A href="http://mesa.sourceforge.net/">http://mesa.sourceforge.net/</A>).
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