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These b oson stars form a one parameter family. Boundary Conditions at the Origin. Content may be subject to copyright. Raphson method was then employed b y linearizing the equations of motion with respect to the sp ectral. However full n umerical results awa y from the perturbative regime have yet only been presented. If they are perturbatively stable then their non-linear stability determines whether the corresponding. The fact that Chebyshev approximations ha ve exponential convergence[34] leads to a n umber of. As the central energy density.

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