Abstract
AbstractWe describe ongoing work towards construction—via multidomain, modal, spectral methods—of helically symmetric spacetimes representing binary neutron stars. Adopting “particle” models, we focus here on solution of the helically reduced Einstein equations. These models allow us to remove the complication of a stellar fluid. However, the choice of inner boundary conditions for these models is also a stubborn issue. We examine this issue and its effect on the “harmonic gauge”.
Publisher
Springer International Publishing
Reference13 articles.
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3. Lau, S.R., Price, R.H.: Multidomain spectral method for the helically reduced wave equation. J. Comput. Phys. 227, 1126–1161 (2007). We regret an error in Eq. (42). The correct expressions are
$$\displaystyle \begin{aligned} \begin{aligned} u_t + f(u)_x &= 0, & (x,t) \in \mathbb{R}\times \mathbb{R}_{+},\\ u(0) &= u_0, \end{aligned} {} \end{aligned} $$
The right-hand side of the second equation of (69) is also off by a sign
4. Lau, S.R., Price, R.H.: Sparse spectral-tau method for the three-dimensional helically reduced wave equation on two-center domains. J. Comput. Phys. 231(2), 7695–7714 (2012)
5. Beroiz, M., Hagstrom, T., Lau, S.R., Price, R.H.: Multidomain, sparse, spectral-tau method for helically symmetric flow. Comput. Fluids 102, 250–265 (2014)