Star formation simulations: caveats
نویسندگان
چکیده
منابع مشابه
Insights from simulations of star formation
Although the basic physics of star formation is classical, numerical simulations have yielded several essential insights into how stars form. They show that star formation is a highly nonuniform runaway process characterized by the emergence of nearly singular peaks in density, followed by the accretional growth of embryo stars that form at these density peaks. Circumstellar disks often form fr...
متن کاملNumerical Simulations of Galaxy Formation: Cooling, Heating, Star Formation
Formation of luminous matter in the Universe is a complicated process, which includes many processes and components. It is the vastly different scales involved in the process (from star formation on few parsec scales to galaxy clusters and superclusters on megaparsecs scales) and numerous ill-understood processes, which make the whole field a maze of unsolved, but exciting problems. We present ...
متن کاملThe physics and modes of star cluster formation: simulations.
We review progress in numerical simulations of star cluster formation. These simulations involve the bottom-up assembly of clusters through hierarchical mergers, which produces a fractal stellar distribution at young (approx. 0.5 Myr) ages. The resulting clusters are predicted to be mildly aspherical and highly mass-segregated, except in the immediate aftermath of mergers. The upper initial mas...
متن کاملStar Formation History of Dwarf Galaxies in Cosmological Hydrodynamic Simulations
We examine the past and current work on the star formation (SF) histories of dwarf galaxies in cosmological hydrodynamic simulations. The results obtained from different numerical methods are still somewhat mixed, but the differences are understandable if we consider the numerical and resolution effects. It remains a challenge to simulate the episodic nature of SF history in dwarf galaxies at l...
متن کاملModeling Molecular Hydrogen and Star Formation in Cosmological Simulations
We describe a phenomenological model for molecular hydrogen formation suited for applications in galaxy formation simulations, which includes non-equilibrium formation of H2 on dust and approximate treatment of both its self-shielding and shielding by dust from the dissociating UV radiation. The model is applicable in simulations in which individual star forming regions – the giant molecular co...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2009
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921310011713