Past exam of the mathematics course of the University of Cambridge / 2023 / iii / Paper 321 (Dynamics of Astrophysical Discs)

In the razor-thin disk approximation, the three-dimensional Poisson equation isFor a horizontal Fourier mode with wavevector $\mathbf{k}$ and $k=|\mathbf{k}|>0$, the Fourier transform of this equation isThe solution that decays away from the disk isConsequently the required razor-thin disk Poisson kernel in the midplane isThe spatially uniform $k=0$ background is excluded from this local perturbation formula.

For a Keplerian shearing sheet, the shear rate is $S=3\Omega /2$ and the shearing-sheet tidal potential isA uniform steady solution isThe Coriolis acceleration of this linear shear flow balances the radial tidal acceleration. The only nonzero background component of the viscous stress tensor that matters is $T_{xy}=-\nu ({\Sigma }_0){\Sigma }_{0}S$, which is spatially constant. Hence $\nabla \cdot \mathbf{T}=0$: a local uniform patch has no stress gradient or torque divergence to drive an accretion flow.

Write the perturbations as $(\sigma ,u,v)e^{i{k}_{x}x+\lambda t}$, set $k=|k_x|$, and evaluate all unmarked background quantities at ${\Sigma }_0$. DefineThe linearized mass conservation equation isThe radial and azimuthal momentum equations arewhere the razor-thin disk Poisson kernel gives $\varphi =-2\pi G\sigma /k$. The term proportional to $\beta$ comes from perturbing the density-dependent background shear stress $T_{xy}=-\nu \Sigma S$.

Eliminating $\sigma ,u,v$ and using $S=3\Omega /2$, so that the radial epicyclic frequency obeys ${\kappa }_r^2=2\Omega (2\Omega -S)={\Omega }^2$, gives the dispersion relation

Setting $\nu ={\nu }_b=0$, the dispersion relation reduces toAn axisymmetric density mode grows whenThe left-hand side is a concave quadratic function of $k$, with maximum $(\pi G{\Sigma }_0{)}^2/v_s^2$ at $k=\pi G{\Sigma }_0/v_s^2$. Growth is therefore possible precisely when the Toomre stability criterion is violated:

The constant term of the real cubic dispersion relation isA negative $c$ guarantees a positive real root because the cubic tends to $+\infty$ as $\lambda \to +\infty$.

If $\beta <0$, then $c<0$ at sufficiently small positive $k$, producing a viscous instability of an accretion disk. This is the local form of the global thin-disk diffusion equationSince $d(\nu \Sigma )/d\Sigma <0$, the effective diffusion reverses sign and amplifies surface-density variations.

If $\beta >0$, instability is still possible when the quadratic expression in parentheses is negative. Its minimum occurs at $k=\pi G{\Sigma }_0/v_s^2$, so the condition isorThis is a secular gravitational instability of an astrophysical disk: viscosity allows self-gravity to overcome rotational support even in part of the range that is stable by the inviscid $Q<1$ criterion.

Let $D/Dt={\partial }_t-Sx{\partial }_y$ be the material derivative along the background linear shear flow ${\mathbf{u}}_0=-Sx{\mathbf{e}}_y$. Linearizing about constant $\Sigma$ givesThe coefficient $2\Omega -S$ includes the contribution $\mathbf{v}\cdot \nabla {\mathbf{u}}_0=-S{v}_x{\mathbf{e}}_y$ from perturbation advection of the background shear.

The first-order perturbation of the vortensity isTaking the curl of the linearized momentum equation and using the linearized continuity equation yieldsThis is linearized vortensity conservation. It is the perturbative form of material conservation of potential vorticity in an inviscid barotropic fluid; the forcing $-\nabla \Psi$ is a gradient and therefore creates no vorticity.

For zero forcing, the given equation for $v_y$ isUse the shearing-wave ansatzThe explicit $x$ dependence cancels from the material derivative whenThe amplitude then obeys the time-dependent harmonic oscillator equationThis evolving wavevector is the characteristic signature of a shearing wave.

A satellite on a circular orbit is stationary in the corotating sheet. Write its tidal forcing and the response asSince $D=-iS{k}_{y}x$, the forced wave equation becomesThis ordinary differential equation describes a satellite-forced density wave in an astrophysical disk.

The homogeneous equation can be writtenIts solutions are locally oscillatory whereequivalentlyThe relative background orbital speed is $|{\mathbf{u}}_0|=|Sx|$, so propagating wave zones occur only where the relative motion of the satellite and disk material is supersonic.

Take the Fourier transform in $x$, with convention $\tilde{v}(k_x)=\int v(x)e^{-i{k}_{x}x}dx$. The differentiation rules $\widehat{v^{\prime \prime }}=-k_x^2\tilde{v}$ and $\widehat{x^{2}v}=-{\tilde{v}}^{\prime \prime }$ turn the forced equation intoFor the unforced equation, $d{k}_x/dt=S{k}_y$ impliesIt is therefore exactly the shearing-wave oscillator found in part c, now parametrized by radial wavenumber rather than time.

For a circular orbit of cylindrical radius $r$ in an axisymmetric gravitational potential,A small vertical displacement satisfiesso the vertical epicyclic frequency isFor a spherically symmetric potential $\Phi (R)$, where $R=(r^2+z^2{)}^{1/2}$,Hence $\boxed{{\Omega }_z=\Omega }$. Geometrically, a slightly tilted circular orbit remains a circular orbit in a different plane, and its height completes one oscillation per revolution.

Vertical hydrostatic equilibrium givesDefine vertically integrated pressure and the density-weighted disk scale height byMultiply the hydrostatic equation by $z$ and integrate. Since $zp\to 0$ at both boundaries, integration by parts givesTherefore

Introduce the dimensionless variablesUsing $P=\Sigma H^2{\Omega }_z^2$, vertical hydrostatic equilibrium becomes the parameter-free equationwith normalizations $\int \tilde{\rho }d\tilde{z}=1$ and $\int \tilde{p}d\tilde{z}=1$. For an isothermal atmosphere, $p=c_s^2\rho$, and these conventions give the Gaussian distribution

Gas in hydrostatic balance has zero vertical velocity. A dust grain subject to linear drag with aerodynamic stopping time $\tau$ therefore obeysThis is a damped harmonic oscillator. For ${\Omega }_z\tau >1/2$, the motion is underdamped, with angular frequencyand envelope $e^{-t/(2\tau )}$. Critical damping occurs at ${\Omega }_z\tau =1/2$. For ${\Omega }_z\tau <1/2$, the motion is overdamped. In the strong-drag limit ${\Omega }_z\tau \ll 1$, a rapid transient on timescale $\tau$ leaves slow dust settling in an astrophysical disk at rate ${\Omega }_z^2\tau$; in the weak-drag limit the grain makes many damped vertical oscillations.

Let $\zeta =z/H(t)$ label a fluid element and use the homologous vertical motion of an astrophysical diskBecause $D\zeta /Dt=0$ and $\nabla \cdot \mathbf{u}=\dot{H}/H$, this ansatz satisfies mass conservation. The pressure equation for an adiabatic process giveshenceThe vertical acceleration is $D{u}_z/Dt=\ddot{H}\zeta$. Using the dimensionless hydrostatic profiles from part c, the pressure force is $(P/\Sigma H)\zeta$, and the vertical momentum equation reduces towhere $C$ is constant.

At the equilibrium thickness $H_0$,Set $H=H_0+h$ and retain terms linear in $h$. The linearization isThus the vertical breathing mode of an astrophysical disk has angular frequency