Numerical solution of the 1D spherical non stationary radiating shock using characteristics - Application to protostars

Details Numerical solution of the 1D spherical non stationary radiating shock using characteristics - Application to protostars Numerical solution of the 1D spherical non stationary radiating shock using characteristics - Application to protostars

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90..327m&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 3, Oct. 1980, p. 327-337.

Astronomy and Astrophysics

Astrophysics

Early Stars, Protostars, Radiative Transfer, Shock Wave Propagation, Stellar Evolution, Anisotropy, Approximation, Hydrodynamic Equations, Stellar Models, Transport Properties

Scientific paper

An implicit numerical code for solving, by means of characteristics the spherically symmetric hydrodynamical equations of stellar evolution is presented. Characteristics properties are used: (1) to solve the time dependent equations, (2) to locate in space and time, the shocks developing spontaneously within the gas, (3) to follow their subsequent motion with a shock fitting method, (4) to simplify the calculations of the supercritical shocks by the use of an isothermal shock approximation. The spherically symmetric transfer equation (grey and time independent approximations), with a discontinuous source function, is formulated as a two points boundary-value problem and solved simultaneously with hydrodynamics by means of a variable factor of anisotropy (instead of the variable Eddington factor). As an example the procedure is applied to the hydrodynamical collapse of protostars. Comments on the advantages of characteristics and on the validity of the models with pseudo-viscosity are given.

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