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BibTeX export options can be customized via Preferences -> BibTeX in Mendeley Desktop  @article{SpringelYoshidaWhite2001, @article{Pontzenetal2013,  abstract = {We describe the newly written code GADGET which {Pynbody  is suitable both for cosmological simulations of structure formation and a lightweight, portable, format-transparent analysis package  for the simulation of interacting galaxies. GADGET evolves self-gravitating collisionless fluids with the traditional astrophysical  N-bodyapproach,  and a collisional gas by smoothed smooth  particle hydrodynamics. Along with the serial version of the code, we discuss a parallel version that has been designed to run on massively parallel supercomputers with distributed memory. While both versions use a tree algorithm to compute gravitational forces, the serial version of GADGET can optionally employ the special-purpose hardware GRAPE instead of hydrodynamic simulations supporting PKDGRAV/Gasoline, Gadget, N-Chilada, and RAMSES AMR outputs. Written in python,  the tree. Periodic boundary conditions core tools  are supported accompanied  bymeans of an Ewald summation technique. The code uses individual and adaptive timesteps for all particles, and it combines this with a scheme for dynamic tree updates. Due to its Lagrangian nature, GADGET thus allows  a very large dynamic range to be bridged, both in space and time. So far, GADGET has been successfully used to run simulations with up to 7.5***INVALID BYTE SEQUENCE HERE******INVALID BYTE SEQUENCE HERE***10 7 particles, including cosmological studies of large-scale structure formation, high-resolution simulations of the formation of clusters of galaxies, as well as workstation-sized problems of interacting galaxies. In this study, we detail the numerical algorithms employed, and show various tests of the code. We publicly release both the serial and the massively parallel version library  of the code.}, publication-level analysis routines.},  author = {Springel, Volker {Pontzen, Andrew  and Yoshida, Naoki Ro{\v{s}}kar, Rok  and White, Simon D.M.},  doi = {10.1016/S1384-1076(01)00042-2},  file = {:Users/jhummel/Documents/papers/literature/2001/Springel, Yoshida, White{\_}2001.pdf:pdf},  issn = {13841076}, Stinson, Greg and Woods, Rory},  journal = {New Astronomy},  month = {apr},  number = {2},  pages = {79--117}, {Astrophysics Source Code Library},  title = {{GADGET: a code {{pynbody: N-Body/SPH analysis  for collisionless and gasdynamical cosmological simulations}}, python}},  url = {http://adsabs.harvard.edu.ezproxy.lib.utexas.edu/abs/2001NewA....6...79S},  volume = {6}, {http://adsabs.harvard.edu.ezproxy.lib.utexas.edu/abs/2013ascl.soft05002P},  year = {2001} {2013}  }  @article{PallaSalpeterStahler1983,  abstract = {The thermal and chemical evolution of a collapsing spherical cloud composed of pure hydrogen gas is investigated. It is assumed that the cloud is in pressure-free collapse. Over a broad range of initial conditions, virtually all the gas is converted to molecular form by a density n = 10 to the 12th/cu cm. The reactions found to be most effective are the three-body ones: H + H + H yielding H2 + H; and H + H + H2 yielding 2H2. As a consequence of significant cooling from the molecules, the temperature rise is slowed, and the Jeans mass eventually falls below 0.1 solar mass for clouds less massive than 100 solar masses. Such clouds should thus be capable of fragmenting into low-mass stars. This conclusion is even more valid if angular momentum slows the collapse. Also included in a heuristic manner is the effect of shock heating from colliding fragments in a turbulent collapsing cloud. Owing to the early destruction of hydrogen molecules, the Jeans mass cannot drop as far with substantial heating.The primordial stellar mass spectrum may thus be a sensitive function of the degree and effectiveness of intercloud collisions.}, 
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volume = {125},  year = {2013}  }  @article{SpringelYoshidaWhite2001,  abstract = {We describe the newly written code GADGET which is suitable both for cosmological simulations of structure formation and for the simulation of interacting galaxies. GADGET evolves self-gravitating collisionless fluids with the traditional N-body approach, and a collisional gas by smoothed particle hydrodynamics. Along with the serial version of the code, we discuss a parallel version that has been designed to run on massively parallel supercomputers with distributed memory. While both versions use a tree algorithm to compute gravitational forces, the serial version of GADGET can optionally employ the special-purpose hardware GRAPE instead of the tree. Periodic boundary conditions are supported by means of an Ewald summation technique. The code uses individual and adaptive timesteps for all particles, and it combines this with a scheme for dynamic tree updates. Due to its Lagrangian nature, GADGET thus allows a very large dynamic range to be bridged, both in space and time. So far, GADGET has been successfully used to run simulations with up to 7.5***INVALID BYTE SEQUENCE HERE******INVALID BYTE SEQUENCE HERE***10 7 particles, including cosmological studies of large-scale structure formation, high-resolution simulations of the formation of clusters of galaxies, as well as workstation-sized problems of interacting galaxies. In this study, we detail the numerical algorithms employed, and show various tests of the code. We publicly release both the serial and the massively parallel version of the code.},  author = {Springel, Volker and Yoshida, Naoki and White, Simon D.M.},  doi = {10.1016/S1384-1076(01)00042-2},  file = {:Users/jhummel/Documents/papers/literature/2001/Springel, Yoshida, White{\_}2001.pdf:pdf},  issn = {13841076},  journal = {New Astronomy},  month = {apr},  number = {2},  pages = {79--117},  title = {{GADGET: a code for collisionless and gasdynamical cosmological simulations}},  url = {http://adsabs.harvard.edu.ezproxy.lib.utexas.edu/abs/2001NewA....6...79S},  volume = {6},  year = {2001}  }  @article{Springel2014,  abstract = {Numerical methods play an ever more important role in astrophysics. This is especially true in theoretical works, but of course, even in purely observational projects, data analysis without massive use of computational methods has become unthinkable. The key utility of computer simulations comes from their ability to solve complex systems of equations that are either intractable with analytic techniques or only amenable to highly approximative treatments. Simulations are best viewed as a powerful complement to analytic reasoning, and as the method of choice to model systems that feature enormous physical complexity such as star formation in evolving galaxies, the topic of this 43rd Saas Fee Advanced Course. The organizers asked me to lecture about high performance computing and numerical modelling in this winter school, and to specifically cover the basics of numerically treating gravity and hydrodynamics in the context of galaxy evolution. This is still a vast field, and I necessarily had to select a subset of the relevant material. The written notes presented here quite closely follow the lectures as held in Villars-sur-Ollon, which were meant to provide a general overview about some of the most pertinent techniques that may be relevant for students working on numerical models of galaxy evolution and star formation. The discussion is hence often at an introductory level, giving precedence to a presentation of the main numerical concepts rather than to a mathematically detailed exposition of the techniques.},  archivePrefix = {arXiv},