Tidal Stablization of Neutron Stars and White Dwarfs

Dong Lai
Phys. Rev. Lett. 76, 4878 – Published 24 June 1996
PDFExport Citation

Abstract

What happens to a neutron star or white dwarf near its maximum mass limit in a close binary orbit? Using an energy variational principle the tidal field reduces its central density, making it stable against radial collapse. For a cold white dwarf, the tidal field increases the maximum stable mass, but lowers the maximum central density by 30%. A white dwarf in a close binary may be more susceptible to the general relativistic instability than that with electron capture or pycronuclear reaction. We analyze radial stability of a neutron star using post-Newtonian approximation with a degenerate neutron gas equation of state. Tidal stablization implies that the neutron star in coalescing neutron star–neutron star or neutron star–black hole binaries does not collapse prior to merger or tidal disruption.

  • Received 29 January 1996

DOI:https://doi.org/10.1103/PhysRevLett.76.4878

©1996 American Physical Society

Authors & Affiliations

Dong Lai

  • Theoretical Astrophysics, 130-33, California Institute of Technology, Pasadena, California 91125

References (Subscription Required)

Click to Expand
Issue

Vol. 76, Iss. 26 — 24 June 1996

Reuse & Permissions
Access Options
Author publication services for translation and copyediting assistance advertisement

Authorization Required


×
×

Images

×

Sign up to receive regular email alerts from Physical Review Letters

Log In

Cancel
×

Search


Article Lookup

Paste a citation or DOI

Enter a citation
×