Grand unification of neutron stars

Kaspi, V. M.

doi:10.1073/pnas.1000812107

Cited by 218 publications

(188 citation statements)

References 99 publications

(85 reference statements)

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“…Hartman et al 1997) to 10 14 G (e.g. Kaspi 2010). As for the initial spin period, it is assumed to be a Gaussian distribution, centered at 30 s and ranging from 0.5 s to 100 s. The different accretion rates are set fromṀ 16 toṀ 18 .…”

Section: Spin Period Versus Accretion Mass (P -δM)mentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

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We investigate the spin period evolutions of recycled pulsars in binary accreting systems. Taking both the accretion induced field decay and spin-up into consideration, we calculate their spin period evolutions influenced by the initial magnetic field strengths, initial spin periods, and accretion rates. The results indicate that the minimum spin period (or maximum spin frequency) of a millisecond pulsar (MSP) is independent of the initial conditions and accretion rate when the neutron star (NS) accretes the mass of ∼0.2 M . The accretion torque with the fastness parameter and gravitational wave (GW) radiation torque may be responsible for the formation of the minimum spin period (maximum spin frequency). The fastest spin frequency (716 Hz) of MSP can be inferred to associate with a critical fastness parameter of about ω c = 0.55. Furthermore, comparisons with the observational data are presented in the field period (B − P) diagram.

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Section: Spin Period Versus Accretion Mass (P -δM)mentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

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“…Sources of giant X-and gamma-ray flashes are thought to arise in highly magnetised NSs, called magnetars, with B-fields ∼ 10 15 -10 16 Gauss. The source of high-energy radiation is believed to be powered by the decay of the magnetic field associated with stellar quakes [436].…”

Section: A Menagerie Of Neutron-star Sourcesmentioning

confidence: 99%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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“…Furthermore, neutron stars created in SNe may be endowed with magnetic fields b ∼ 10 12 G (pulsars) to ∼ 10 14 G (magnetars; see, e.g. Kaspi 2010). Nonetheless, the possible influence of the field on the explosion is less clear.…”

Section: Introductionmentioning

confidence: 99%

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

Obergaulinger¹,

Janka²,

Aloy³

2014

Monthly Notices of the Royal Astronomical Society

105

117

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We study the amplification of magnetic fields in the collapse and the post-bounce evolution of the core of a non-rotating star of 15 M in axisymmetry. To this end, we solve the coupled equations of magnetohydrodynamics and neutrino transport in the two-moment approximation. The pre-collapse magnetic field is strongly amplified by compression in the infall. Initial fields of the order of 10 10 G translate into proto-neutron star fields similar to the ones observed in pulsars, while stronger initial fields yield magnetar-like final field strengths. After core bounce, the field is advected through the hydrodynamically unstable neutrino-heating layer, where non-radial flows due to convection and the standing accretion shock instability amplify the field further. Consequently, the resulting amplification factor of order five is the result of the number of small-eddy turnovers taking place within the time scale of advection through the post-shock layer. Due to this limit, most of our models do not reach equipartition between kinetic and magnetic energy and, consequently, evolve similarly to the non-magnetic case, exploding after about 800 ms when a single or few highentropy bubbles persist over several dynamical time scales. In the model with the strongest initial field we studied, 10 12 G, for which equipartition between flow and field is achieved, the magnetic tension favours a much earlier development of such long-lived high-entropy bubbles and enforces a fairly ordered large-scale flow pattern. Consequently, this model, after exhibiting very regular shock oscillations, explodes much earlier than non-magnetic ones.

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Grand unification of neutron stars

Cited by 218 publications

References 99 publications

Spin period evolution of a recycled pulsar in an accreting binary

Spin period evolution of a recycled pulsar in an accreting binary

Sources of Gravitational Waves: Theory and Observations

Magnetic field amplification and magnetically supported explosions of collapsing, non-rotating stellar cores

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