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Abstract: We introduce and test a new and highly efficient method for treating thethermal and radiative effects influencing the energy equation in SPHsimulations of star formation. The method uses the density, temperature andgravitational potential of each particle to estimate a mean optical depth,which then regulates the particle-s heating and cooling. The method captures -at minimal computational cost - the effects of (i) the rotational andvibrational degrees of freedom of H2, H2 dissociation, H0 ionisation, (ii)opacity changes due to ice mantle melting, sublimation of dust, molecularlines, H-, bound-free and free-free processes and electron scattering; (iv)external irradiation; and (v) thermal inertia. The new algorithm reproduces theresults of previous authors and-or known analytic solutions. The computationalcost is comparable to a standard SPH simulation with a simple barotropicequation of state. The method is easy to implement, can be applied to bothparticle- and grid-based codes, and handles optical depths 0


Autor: D. Stamatellos (1), A. P. Whitworth (1), T. Bisbas (1), S. Goodwin (2) ((1) Cardiff University, (2) Sheffield University)

Fuente: https://arxiv.org/







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