scholarly journals Sink particle radiative feedback in smoothed particle hydrodynamics models of star formation

2018 ◽  
Vol 480 (2) ◽  
pp. 2562-2577 ◽  
Author(s):  
Michael O Jones ◽  
Matthew R Bate
Keyword(s):  
Star Formation ◽  
Smoothed Particle Hydrodynamics ◽  
Radiative Feedback ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Smoothed Particle Hydrodynamics Models

scholarly journals Magnetic fields and Turbulence in Star Formation using Smoothed Particle Hydrodynamics

2010 ◽  
Vol 6 (S270) ◽  
pp. 169-177
Author(s):  
Daniel J. Price
Keyword(s):  
Star Formation ◽  
Mach Number ◽  
Magnetic Fields ◽  
Turbulent Flows ◽  
Smoothed Particle Hydrodynamics ◽  
Current State ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Smoothed Particle Hydrodynamics Method ◽  
The Relationship

AbstractFirstly, we give a historical overview of attempts to incorporate magnetic fields into the Smoothed Particle Hydrodynamics method by solving the equations of Magnetohydrodynamics (MHD), leading an honest assessment of the current state-of-the-art in terms of the limitations to performing realistic calculations of the star formation process. Secondly, we discuss the results of a recent comparison we have performed on simulations of driven, supersonic turbulence with SPH and Eulerian techniques. Finally we present some new results on the relationship between the density variance and the Mach number in supersonic turbulent flows, finding σ2ln ρ = ln(1 + b22 with b = 0.33 up to Mach 20, consistent with other numerical results at lower Mach number (Lemaster & Stone 2008) but inconsistent with observational constraints on σρ and in Taurus and IC5146.

scholarly journals Radiation Driven Implosion and Triggered Star Formation

2010 ◽  
Vol 6 (S270) ◽  
pp. 263-266
Author(s):  
T. G. Bisbas ◽  
A. P. Whitworth ◽  
R. Wünsch ◽  
D. A. Hubber ◽  
S. Walch
Keyword(s):  
Star Formation ◽  
Ionizing Radiation ◽  
Smoothed Particle Hydrodynamics ◽  
Critical Parameter ◽  
External Source ◽  
Incident Flux ◽  
Particle Hydrodynamics ◽  
Smoothed Particle

AbstractWe present simulations of stable isothermal clouds exposed to ionizing radiation from a discrete external source, and identify the conditions that lead to Radiatively Driven Implosion and Star Formation. We use the Smoothed Particle Hydrodynamics code SEREN (Hubber et al. 2010) and the HEALPix-based photoionization algorithm described in Bisbas et al. (2009). We find that the incident ionizing flux is the critical parameter determining the evolution; high fluxes disperse the cloud, whereas low fluxes trigger star formation. We find a clear connection between the intensity of the incident flux and the parameters of star formation.

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