isothermal stellar collapse
Does anyone know how to solve this problem for an isothermal collapse of molecular gas say at T = 10K. I would like to look at how the density "p",M(r), and P changes with time at this stage of protostellar developement.(in one dimension)
eqn of motion: GM(r)/r^2 + (1/"p")(dP/dr) = (d^2r/dt^2) mass conservation: dM(r)/dr = 4(pi)r^2"p" eqn of state: P = R_g"p"T/"u" where "p" is the density, M(r) is the mass inside the radius r, "u" is a constant=2, P is the pressure and all the dirivitives are actually partial derivitives. Boundary Conditions: P(t) = constant or R(t)=constant 
Re: isothermal stellar collapse
There is standard literature on the subject in Graduate level astrophysics curriculuum. The first work on the subject was by Hyashi. I think the standard "best" text is Stellar Evolution by Martin Schwartzschild. I would start there. By the way, rotation is important. The problem gets to be at least 2D rather quickly. Nongravitational effects (i.e. radiation) also become important. The problem gets quite tricky.

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