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- W1567152513 abstract "The theory of the structure of rotating stars becomes relatively simple if the centrifugal acceleration can be derived from a potential V: $$ {omega^2}s{e_s} = - nabla Vquad, $$(42.1)where e s is a unit vector perpendicular to the axis of rotation (pointing outwards) and s is the distance from this axis. One can easily see that a sufficient and necessary condition for the existence of such a potential is that in the system of cylindrical coordinates s, ϕ, z the angular velocity depends on s only: ∂ω/∂z = ∂ω/∂ϕ= 0, i.e. ω is constant on cylinders. We call such an angular-velocity distribution (to which the case of solid-body rotation also belongs) conservative." @default.
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- W1567152513 date "2012-01-01" @default.
- W1567152513 modified "2023-09-25" @default.
- W1567152513 title "The Thermodynamics of Rotating Stellar Models" @default.
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- W1567152513 doi "https://doi.org/10.1007/978-3-642-30304-3_44" @default.
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