Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies

By G. Stinson, Anil Seth, Neal Katz, James Wadsley, Fabio Governato, Thomas R. Quinn. 2006

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We present an analysis of star formation and feedback recipes appropriate for galactic smoothed particle hydrodynamics simulations. Using an isolated Milky Way-like galaxy, we constrain these recipes based on well-established observational results. Our star formation recipe is based on that of Katz (1992) with the additional inclusion of physically motivated supernova feedback recipes. We propose a new feedback recipe in which type II supernovae are modelled using an analytical treatment of blastwaves. With this feedback mechanism and a tuning of other star formation parameters, the star formation in our isolated Milky Way-like galaxy follows the slope and normalisation of the observed Schmidt law. In addition, we reproduce the low density cutoff and filamentary structure of star formation observed in disk galaxies. Our final recipe will enable better comparison of N-body simulations with observations.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bba8600d6d9b0ef00326325214cfc117ca3c1cf8

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Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “…(e.g., Hernquist & Springel 2003; Oppenheimer & Davé 2006; Vogelsberger et al. 2013; Ford et al. 2013; Marinacci et al. 2014) or gas cooling (e.g., Stinson et al. 2006; Governato et al. 2007; Shen et al. 2010; Guedes et al. 2011) as kinetic or thermal energy is injected to model stellar feedback.”
The formation of disc galaxies in a ΛCDM universe (2010, methodology): “Calculations of relevant timescales and numerical tests using the SPH formalism was carried out by Stinson et al. (2006).”
Hierarchical formation of bulgeless galaxies: why outflows have low angular momentum (2010, methodology): “This problem has largely been overcome in simulations by increasingly effective recipes for feedback from supernovae (Thacker & Couchman 2000; Stinson et al. 2006; Governato et al. 2007), and increased resolution that decrease spurious angular momentum losses (Mayer et al. 2008; Sales et al. 2010).”
Galaxy formation theory (2010, methodology): “…means that it is put in by hand using a semianalytic approach (Thacker and Couchman 2000; Kay et al. 2002; Marri and White 2003; White 2004; Stinson et al. 2006; Cox et al. 2006; Scannapieco et al. 2006a; Tasker and Bryan 2006; Stinson 2007; Vecchia and Schaye 2008; Oppenheimer and Davé…”
Riding the Spiral Waves: Implications of Stellar Migration for the Properties of Galactic Disks (2008, background): “When the gas reaches densities and temperatures which allow for star formation, the star formation and supernova (SN) feedback cycles are initiated (Stinson et al. 2006).”
FORMING REALISTIC LATE-TYPE SPIRALS IN A ΛCDM UNIVERSE: THE ERIS SIMULATION (2011, background): “The heated gas has its cooling shut off until the end of the snowplow phase of the SN blastwave, which is set by the local gas density and temperature and by the total amount of energy injected E (Stinson et al. 2006).”
The role of minor mergers in the recent star formation history of early-type galaxies (2007, result): “These SFRs are in good agreement with those for low-mass objects found in previous simulations of isolated galaxies (e.g. Stinson et al. 2006).”
The Dynamical and Chemical Evolution of Dwarf Spheroidal Galaxies with GEAR (2009, methodology): “In GEAR, the cooling of the gas particle affected by the thermal feedback is switched off for a short adiabatic period of time, tad (a few Myr) (Gerritsen 1997; Mori et al. 1997; Thacker & Couchman 2000; Sommer-Larsen et al. 2003; Brook et al. 2004; Stinson et al. 2006).”
THE GENESIS OF THE MILKY WAY'S THICK DISK VIA STELLAR MIGRATION (2010, methodology): “Star formation and stellar feedback are modeled with subgrid recipes as described in Stinson et al. (2006).”
The effects of radial migration on the vertical structure of Galactic discs (2012, background): “Once the simulation begins, the gas cools and collapses into a disc that forms stars according to a standard prescription (Stinson et al. 2006) with a density threshold of 0.1 amu/cc and a temperature cutoff of1.”
(Star)bursts of FIRE: observational signatures of bursty star formation in galaxies (2015, result): “In contrast, several recent simulations have attempted to physically model the effects of feedback on star-forming clouds instead of imposing a sub-resolution description of them (Stinson et al. 2006; Mashchenko et al. 2008; Governato et al. 2010; Zolotov et al. 2012; Teyssier et al. 2013).”
Simulating galactic outflows with kinetic supernova feedback (2008, background): “…et al. 2002; Springel & Hernquist 2003; Oppenheimer & Davé 2006; Dubois & Teyssier 2008) and/or suppressing radiative cooling by hand (e.g. Gerritsen 1997; Mori et al. 1997; Thacker & Couchman 2000; Kay et al. 2002; Sommer-Larsen, Götz, & Portinari 2003; Brook et al. 2004; Stinson et al. 2006).”
Hierarchical formation of bulgeless galaxies – II. Redistribution of angular momentum via galactic fountains (2011, methodology): “Details of the manner in which metals are incorporated into the code are found in Stinson et al. (2006).”
Radial migration in disc galaxies — I. Transient spiral structure and dynamics (2011, background): “The tuning of the sub-grid star formation and feedback prescriptions are described extensively in Stinson et al. (2006).”
Effects of supernova feedback on the formation of galaxy discs (2008, background): “…2002; Abadi et al. 2003; Marri & White 2003; Sommer-Larsen, Götz & Portinari 2003; Springel & Hernquist 2003; Brook et al. 2004; Okamoto et al. 2005; Oppenheimer & Davé 2006; Stinson et al. 2006; Governato et al. 2007; Dalla Vecchia & Schaye 2008; Dubois & Teyssier 2008; Finlator & Davé 2008).”
REPRODUCING THE STELLAR MASS/HALO MASS RELATION IN SIMULATED ΛCDM GALAXIES: THEORY VERSUS OBSERVATIONAL ESTIMATES (2012, methodology): “As in previous works using the “blastwave” SN feedback approach (Stinson et al. 2006; Governato et al. 2012), mass, thermal energy, and metals are deposited into nearby gas when massive stars evolve into SNe.”
Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, methodology): “The simulations use a common recipe for star formation described in Stinson et al. (2006) that we summarize here.”
The formation and survival of discs in a ΛcDM universe (2008, background): “…star formation histories and chemical abundances (e.g. Springel & Hernquist 2003; Brook et al. 2004; Okamoto et al. 2005; Oppenheimer & Davé 2006; Stinson et al. 2006; Governato et al. 2007; Dalla Vecchia & Schaye 2008; Dubois & Teyssier 2008; Finlator & Davé 2008; Scannapieco et al. 2008…”