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These absorption features are produced by rapidly outflowing atoms that absorb the radiation from the underlying stellar surface.
A mass as puny as the earth's would not move a star any more than the random boiling motions of a stellar surface.
Mass loss rates normalized to stellar surface area as a function of age for stars in Table 6.
The viscosity peaks at the stellar surface, identified as a shock by the scheme, and drops in the interior.
A stellar surface changes throughout the course of an iterative solution, potentially stalling the convergence.
Any inclination of the magnetic field relative to the stellar surface is allowed.
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This can happen, e.g., close to stellar surfaces as a result of oscillations in the solution.
We present a new multidomain spectral method for the treatment of non-spherical stellar surfaces in iterative methods for binary neutron stars.
Unlike current collocation (or nodal) approaches for treating surfaces (which rely on coordinate transformations to ensure that stellar surfaces arise at subdomain boundaries), our approach requires no regridding or nontrivial Jacobians.
This behaviour is to be contrasted with the typical situation encountered when evolving inspiralling binary neutron stars, where the stellar surfaces move very supersonically with respect to the floor and most of the errors at the surface are absorbed into the shocks.
Even a moderate increase in the stellar central surface density does not yield any global spiral modes.
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