Abstract
We discuss dynamical instability of non-adiabatic anisotropic collapse of spherical self-gravitating systems through collapse equation in Palatini f(R) gravity. We take R+ϵRn model and assume hydrostatic equilibrium of celestial object at large past time such that T(−∞)=0. Considering perturbation from hydrostatic phase, and linearizing the dynamical as well as field equations, we evaluate instability constraints at Newtonian as well as post-Newtonian approximations. We conclude that pressure and heat flow assist collapsing phenomenon while Palatini f(R) dark source terms affect dynamics of self-gravitating object due to its non-attractive nature through stiffness parameter.
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Appendices
Appendix A
The dark source terms D0 and D1 of Eqs. (25) and (26) are
The portions of first and second dynamical equations (41) and (42) are
The extra curvature term of the collapse equation (48) is
Appendix B
The quantity D1S appearing in Eq. (40) is given as follows
The quantities ζ j are
The quantity D5(r) in the above equations is
The quantities ζ jG are
The coefficients of the differential equation (43) are given by
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Sharif, M., Yousaf, Z. Dynamical analysis of radiating spherical collapse in Palatini f(R) gravity. Astrophys Space Sci 354, 481–496 (2014). https://doi.org/10.1007/s10509-014-2116-3
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DOI: https://doi.org/10.1007/s10509-014-2116-3