Neutron star kicks and supernova asymmetry

Lai, Dong

doi:10.1017/cbo9780511536236.032

Cited by 17 publications

(7 citation statements)

References 51 publications

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“…A much more detailed analysis can be found in [23]. It is accepted that pulsars have much higher proper velocities than their progenitors, some moving as quickly as 1000 km/s [24,44,45,46,47,48,49,50]. Such large velocities are unambiguously confirmed with the model independent measurement of pulsar B1508+55 moving 1083 +103 −90 km/s [22].…”

Section: Neutron Star Kicksmentioning

confidence: 66%

“…Currently no mechanism exists that can reliably kick the star hard enough. Explosions during collapse can only reliably kick a star 50 km/s [24], asymmetric explosions can only reach 200 km/s [50], and asymmetric neutrino emission is plagued by the problem that at temperatures high enough to produce the kick the neutrino is trapped inside the star [51,52]. More exotic mechanisms require exotic particles and more fine tuning.…”

Section: Neutron Star Kicksmentioning

confidence: 99%

See 1 more Smart Citation

Topological currents in neutron stars: kicks, precession, toroidal fields, and magnetic helicity

Charbonneau

Zhitnitsky

2010

J. Cosmol. Astropart. Phys.

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The effects of anomalies in high density QCD are striking. We consider a direct application of one of these effects, namely topological currents, on the physics of neutron stars. All the elements required for topological currents are present in neutron stars: degenerate matter, large magnetic fields, and parity violating processes. These conditions lead to the creation of vector currents capable of carrying momentum and inducing magnetic fields. We estimate the size of these currents for many representative states of dense matter in the neutron star and argue that they could be responsible for the large proper motion of neutron stars (kicks), the toroidal magnetic field and finite magnetic helicity needed for stability of the poloidal field, and the resolution of the conflict between type-II superconductivity and precession. Though these observational effects appear unrelated, they likely originate from the same physics-they are all P-odd phenomena that stem from a topological current generated by parity violation.

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Section: Neutron Star Kicksmentioning

confidence: 66%

Section: Neutron Star Kicksmentioning

confidence: 99%

Topological currents in neutron stars: kicks, precession, toroidal fields, and magnetic helicity

Charbonneau

Zhitnitsky

2010

J. Cosmol. Astropart. Phys.

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“…Any asymmetry in the SN, such as in the mass or neutrino loss (e.g. Janka, 2012;Lai, 2004), can give rise to a natal-kick v k to the star. Neutron stars are expected to receive a kick at birth of about 400 kms −1 (e.g.…”

Section: Supernova Explosionsmentioning

confidence: 99%

The evolution of hierarchical triple star-systems

2016

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Field stars are frequently formed in pairs, and many of these binaries are part of triples or even higher-order systems. Even though, the principles of single stellar evolution and binary evolution, have been accepted for a long time, the long-term evolution of stellar triples is poorly understood. The presence of a third star in an orbit around a binary system can significantly alter the evolution of those stars and the binary system. The rich dynamical behaviour in three-body systems can give rise to Lidov-Kozai cycles, in which the eccentricity of the inner orbit and the inclination between the inner and outer orbit vary periodically. In turn, this can lead to an enhancement of tidal effects (tidal friction), gravitational-wave emission and stellar interactions such as mass transfer and collisions. The lack of a self-consistent treatment of triple evolution, including both three-body dynamics as well as stellar evolution, hinders the systematic study and general understanding of the long-term evolution of triple systems. In this paper, we aim to address some of these hiatus, by discussing the dominant physical processes of hierarchical triple evolution, and presenting heuristic recipes for these processes. To improve our understanding on hierarchical stellar triples, these descriptions are implemented in a public source code TrES, which combines three-body dynamics (based on the secular approach) with stellar evolution and their mutual influences. Note that modelling through a phase of stable mass transfer in an eccentric orbit is currently not implemented in TrES, but can be implemented with the appropriate methodology at a later stage.

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“…Indeed its central body is a neutron star with radii of order of 10 km and masses of order of the solar mass (2 x 10 33 g), the nuclear density (10 14 -10 15 g / cm 3 ), superfluid neutrons and superconducting protons in inner regions and magnetic fields of order of 10 12 G at the surface.There are relativistic electrons and positrons in magnetospheres of neutron stars.These stars are formed during explosions of supernovae. Many unusual physical processes are realized in radio pulsars, and they can be used to verify some new theories and models.…”

Section: Introductionmentioning

confidence: 99%

“…Several mechanisms have been proposed to explain such high velocities, and are reviewed, for example, by Lai [3].…”

Section: Introductionmentioning

confidence: 99%

Anisotropic Distribution of Space Pulsar Velocities

Малов¹

2014

AJAA

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Abstract:On the base of new data it is shown that the observed proper motions and directions of the tangential velocities of pulsars manifest the extremely anisotropic distributions. These anisotropies cannot be explained by the structure of our Galaxy or by various types of solar motions. They can be caused by the cosmological vector potential and the action of the new force. This force must be stronger in higher magnetic fields. The positive correlation between tangential velocities V t and surface magnetic fields of pulsars B s is seen indeed. It is shown that the new force can provide pulsar velocities up to several thousands of km/sec.

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Neutron star kicks and supernova asymmetry

Cited by 17 publications

References 51 publications

Topological currents in neutron stars: kicks, precession, toroidal fields, and magnetic helicity

Topological currents in neutron stars: kicks, precession, toroidal fields, and magnetic helicity

The evolution of hierarchical triple star-systems

Anisotropic Distribution of Space Pulsar Velocities

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