Other
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.3803s&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #38.03; Bulletin of the American Astronomical Society, Vol. 24, p.788
Other
Scientific paper
Density discontinuities produced by rapid composition variations, as well as smooth variations in entropy, both provide sources of buoyancy which influence the global oscillation spectra of neutron stars. Previous calculations by Finn (1987) and McDermott (1990) investigated the g-modes induced by density discontinuities at zero temperature. That is, they neglected the contributions to buoyancy due to smooth variations in entropy at finite temperature. They also investigated only pure fluid models. We have extended these previous calculations by computing the quadrupole oscillation spectra, both with and without a single density discontinuity, of two finite-temperature, three-component (core, crust, ocean) neutron star models. We assumed the presence in each model of a density discontinuity associated with the (56) Fe to (62) Ni transition predicted by the BPS equation of state (Baym, Pethick and Sutherland 1971). For one model this discontinuity occurs in the solid crust of the star, while for the other, hotter (younger) model it resides in the fluid ocean overlying the crust. When the discontinuity resides in the solid crust we find no significant differences between the oscillation spectra computed with and without the discontinuity. However, when the discontinuity lies in the fluid ocean the g-mode spectrum is significantly altered. In particular, the period of the fundamental g-mode of this model drops from about 50 ms to 35 ms. The periods of successive overtones are also perturbed away from their values without a discontinuity. {References} Baym, G., Pethick, C. & Sutherland, P., 1971, {it Ap. J.}, 170, 299. Finn, L. S., 1987, M. N. R. A. S., 227, 265. McDermott, P. N., 1990, M. N. R. A. S., 245, 508.
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