Tidal Stripping Radii

Class providing models of tidal stripping radii for satellites—the radius (in Mpc) within which material remains gravitationally bound to the satellite against the tidal field of the host halo. Beyond this radius the tidal force exceeds the satellite’s self-gravity, so mass is stripped away. The tidal radius depends on the satellite mass, the host density at the satellite’s orbital position, and the choice of tidal criterion (e.g.King 1962 or Jacobi radius). It sets the outer boundary used by tidal stripping rate models.

Default implementation: satelliteTidalStrippingRadiusKing1962

Methods

radius → double precision

Returns the tidal stripping radius (in units of Mpc) for the given satellite node, i.e., the radius within which material remains gravitationally bound against the tidal field of the host halo.

  • type(treeNode), intent(inout), target :: node

satelliteTidalStrippingRadiusKing1962

A satellite tidal radius class which uses the method of King (1962):

\[r_\mathrm{tidal}=\left(\frac{GM_\mathrm{sat}}{\gamma_\mathrm{c} \omega^2-d^2\Phi/dr^2}\right)^{1/3},\]

where \(\omega\) is the orbital angular velocity of the satellite, \(\Phi(r)\) is the gravitational potential due to the host, and \(\gamma_\mathrm{c}=\)[efficiencyCentrifugal] is the a model parameter that controls the efficiency of centrifugal force. The calculation is based on the dark matter only density profile of the satellite—no accounting is made for the baryonic components.

(Default implementation)

Parameters

  • [efficiencyCentrifugal] (default 1.0d0) — Efficiency of the centrifugal force. For zero value, the centrifugal force is neglected in computing the tidal radius.

  • [applyPreInfall] (default .false.) — If true, tidal radii are computed pre-infall, allowing tidal stripping to begin acting on satellites before they formally enter the host virial radius.