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Birth accelerations of neutron stars

  • Ricardo Heras (a1)
Abstract
Abstract

We suggest that neutron stars experienced at birth three related physical changes, which may originate in magneto-rotational instabilities: (i) an increase in period from the initial value P0 to the current value Ps, implying a change of rotational energy Δ Erot; (ii) an exponential decay of its magnetic field from the initial value B0 to the current surface value Bs, implying a change of radiative energy Δ Erad; and (iii) an increase of space velocity from the initial value v0 to the current value v, implying a change of kinetic energy Δ Ekin. These changes are assumed to be connected by Δ Erad + Δ Ekin = Δ Erot. This means that the radiation loss and increase of kinetic energy are both at the expense of a rotational energy loss. It is shown that this energy conversion occurs during times of order of 10−4 s if the neutron stars are born with magnetic fields in the range of 1015–1016 G and initial periods in range 1–20 ms. It is shown that the birth accelerations of neutron stars are of the order of 108g.

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This list contains references from the content that can be linked to their source. For a full set of references and notes please see the PDF or HTML where available.

U. Geppert & M. Rheinhardt 2006, A&A, 456, 639

E. R. Harrison & E. Tademaru , 1975, ApJ, 201, 447

A. Lyne , et al., 1993, MNRAS, 265, 1003

A. Lyne & D. Lorimer , 2006, Nature, 369, 127

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Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
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