## Slowly rotating two-fluid neutron star model
We study stationary axisymmetric configurations of a star model consisting of two barotropic fluids, which are uniformly rotating at two different rotation rates. Analytic approximate solutions in the limit of slow rotation are obtained with the classical method of Chandrasekhar, which consists of an expansion of the solution in terms of the rotation rate, and which is generalized to the case of two fluids in order to apply it to the present problem. This work has a direct application to neutron star models, in which the neutron superfluid can rotate at a different speed than the fluid of charged components. Two cases are considered, the case of two non-interacting fluids, and the case of an interaction of a special type, corresponding to the vortices of the neutron superfluid being completely pinned to the second fluid. The special case of the equation of state is solved explicitly as an illustration of the foregoing results.
This article contains no SIMBAD objects. ## Contents- 1. Introduction
- 2. The two-fluid model
- 3. The two-fluid model for neutron stars
- 4. Generalized Chandrasekhar expansion
- 5. Boundary conditions
- 6. Formal solution
- 7. Expansion, ellipticity and moment of inertia
- 8. Rotational coupling
- 9. Exact solution for the polytrope
- 10. Conclusions
- Acknowledgements
- References
© European Southern Observatory (ESO) 1999 Online publication: December 2, 1999 |