How Do Radial Oscillations Affect Star Stability?

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SUMMARY

This discussion focuses on the impact of radial oscillations on star stability, specifically through the analysis of two key equations related to fluid dynamics and thermal energy. The equations presented are derived from the Navier-Stokes equations and the conservation of energy, indicating that the system has been linearized around a static equilibrium state. The variable ##\xi_r## represents small radial displacements, and the discussion emphasizes the importance of understanding the time dependence of oscillations, particularly through the application of the operator ##\partial/\partial t## and the substitution of velocity terms. The final derived equation suggests a complex interplay between pressure gradients and oscillatory motion.

PREREQUISITES
  • Understanding of fluid dynamics principles, particularly the Navier-Stokes equations.
  • Familiarity with linearization techniques in differential equations.
  • Knowledge of oscillatory motion and its mathematical representation, including complex exponentials.
  • Basic grasp of thermodynamics, specifically the relationship between pressure, density, and energy.
NEXT STEPS
  • Study the derivation and implications of the Navier-Stokes equations in astrophysical contexts.
  • Learn about linear stability analysis in the context of oscillatory systems.
  • Explore the mathematical techniques for solving ordinary differential equations (ODEs) with oscillatory solutions.
  • Investigate the role of radial oscillations in stellar evolution and stability through astrophysical simulations.
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Astronomers, astrophysicists, and students studying stellar dynamics, particularly those interested in the stability of stars and the effects of oscillations on stellar structures.

ergospherical
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Homework Statement
The spherically symmetric oscillations of a star satisfy the Sturm-Liouville equation\begin{align*}
\frac{d}{dr} \left[ \frac{\gamma p}{r^2} \frac{d}{dr}(r^2 \xi_r) \right] - \frac{4}{r} \frac{dp}{dr} \xi_r + \rho \omega^2 \xi_r = 0
\end{align*}
Relevant Equations
N/A
So far I have not made much meaningful progress beyond two equations; \begin{align*}
\rho \frac{D\mathbf{u}}{Dt} = - \nabla p \implies \rho \left( \frac{\partial}{\partial t} + u \frac{\partial}{\partial r} \right)u = - \frac{\partial p}{\partial r}
\end{align*}and thermal energy:\begin{align*}
\frac{Dp}{Dt} = -\gamma p \nabla \cdot \mathbf{u} \implies \left( \frac{\partial}{\partial t} + u \frac{\partial}{\partial r} \right)p = -\gamma p \frac{\partial}{\partial r}(r^2 u)
\end{align*}I'm somewhat confused why there's no time dependence in the form given. What exactly is ##\xi_r##?
 
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You are dealing with oscillations, and there is an \omega^2 in the ODE. That suggests variables are assumed to be functions of r alone times e^{i\omega t}. I suspect \xi_r denotes (small) radial displacement from an equilibrium position, in which case <br /> u_r = \frac{\partial}{\partial t}(\xi_r(r)e^{i\omega t}) = i\omega \xi_r(r) e^{i\omega t}. The ODE you are trying to derive is linear and the governing PDEs are not, which suggests that the system has been linearised about the static equiblibrium state.
 
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Thank you. I applied ##\partial/\partial t## to my first equation and ##\partial/\partial r## to my second equation, and subsequently eliminated ##\partial^2 p / \partial r \partial t##. Then I substituted for ##u = i\omega \xi_r e^{i \omega t}## and kept only terms to linear order in ##\xi_r##. After some manipulation,
\begin{align*}
(\xi_r p')' + (\gamma p(r^2 \xi_r)')' + \rho \omega^2 \xi_r = 0
\end{align*}Seems likely that I made at least one slip. I will check again tomorrow with fresher eyes!
 
ergospherical said:
I will check again tomorrow with fresher eyes!
Have you cleared that with the fresher? :eek:
 
pbuk said:
Have you cleared that with the fresher? :eek:
That would imply that they have a choice!
 

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