Constraints on Neutron Star Crusts From Oscillations in Giant Flares

Details Constraints on Neutron Star Crusts From Oscillations in Giant Flares Constraints on Neutron Star Crusts From Oscillations in Giant Flares

2009-02-10

arxiv.org/abs/0902.1683v2

Phys.Rev.Lett.103:181101,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

5 pages, 3 figures; Version to appear in Phys. Rev. Lett

Scientific paper

10.1103/PhysRevLett.103.181101

We show that the fundamental seismic shear mode, observed as a quasi-periodic oscillation in giant flares emitted by highly-magnetized neutron stars, is particularly sensitive to the nuclear physics of the crust. The identification of an oscillation at ~ 30 Hz as the fundamental crustal shear mode requires a nuclear symmetry energy that depends very weakly on density near saturation. If the nuclear symmetry energy varies more strongly with density, then lower frequency oscillations, previously identified as torsional Alfven modes of the fluid core, could instead be associated with the crust. If this is the case, then future observations of giant flares should detect oscillations at around 18 Hz. An accurate measurement of the neutron skin thickness of lead will also constrain the frequencies predicted by the model.

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