Zhaojun Wang, Guoliang Lv, Chunhua Zhu, Wensheng Huo
In the neutron star, there is the relativistic degenerate electron gas which is the densest in the Universe. Due to electron-electron magnetic interaction, the differential susceptibility can equal or exceed 1, which results in the magnetic system of a neutron star being metastable or unstable states. The Fermi liquid of nucleons under the crust can be in the metastable state, while the crust is in the unstable state, which results in a phase transition occurring and the formation of domain structures in the later. The magnetizations of adjacent magnetic domains have opposite directions. The shearing stress acting on adjacent domains can result in a series of shifts or fractures in the crust. The crust releases the magnetic free energy, which corresponds to the bursts observed in magnetars. Simultaneously, a series of shifts or fractures which the deep crust closed to the Fermi liquid of nucleons undergoes can trigger the phase transition of the Fermi liquid of nucleons from the metastable state to a stable state. The free magnetic energy in the Fermi liquid of nucleons is released, which corresponds to the giant flares observed in some magnetars.
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http://arxiv.org/abs/1303.2442
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