Pulsar kicks by anisotropic neutrino emission from quark matter in strong magnetic fields

Sagert, Irina; Schaffner-Bielich, J.

doi:10.1051/0004-6361:20078530

Cited by 37 publications

(33 citation statements)

References 88 publications

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“…Such a plasma is a thermally equilibrated, but nonisotropic ground state. Because of this and in sharp contrast to the commonly assumed diffusion through an isotropic hot matter [528][529][530][531], the asymmetry of the neutrino distribution is build up rather than wash out by interaction with the stellar plasma.…”

Section: Pulsar Kicks Due To Chiral Shiftmentioning

confidence: 93%

Quantum field theory in a magnetic field: From quantum chromodynamics to graphene and Dirac semimetals

2015

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a b s t r a c tA range of quantum field theoretical phenomena driven by external magnetic fields and their applications in relativistic systems and quasirelativistic condensed matter ones, such as graphene and Dirac/Weyl semimetals, are reviewed. We start by introducing the underlying physics of the magnetic catalysis. The dimensional reduction of the low-energy dynamics of relativistic fermions in an external magnetic field is explained and its role in catalyzing spontaneous symmetry breaking is emphasized. The general theoretical consideration is supplemented by the analysis of the magnetic catalysis in quantum electrodynamics, chromodynamics and quasirelativistic models relevant for condensed matter physics. By generalizing the ideas of the magnetic catalysis to the case of nonzero density and temperature, we argue that other interesting phenomena take place. The chiral magnetic and chiral separation effects are perhaps the most interesting among them. In addition to the general discussion of the physics underlying chiral magnetic and separation effects, we also review their possible phenomenological implications in heavy-ion collisions and compact stars. We also discuss the application of the magnetic catalysis ideas for the description of the quantum Hall effect in monolayer and bilayer graphene, and conclude that the generalized magnetic catalysis, including both the magnetic catalysis condensates and the quantum Hall ferromagnetic ones, lies at the basis of this phenomenon. We also consider how an external magnetic field affects the underlying physics in a class of three-dimensional quasirelativistic condensed matter systems, Dirac semimetals. While at sufficiently low temperatures and zero density of charge carriers, such semimetals are expected to reveal the regime of the magnetic catalysis, the regime of Weyl semimetals with chiral asymmetry is realized at nonzero density. Finally, we discuss the interplay between relativistic quantum field theories (including quantum electrodynamics and quantum chromodynamics) in a magnetic field and noncommutative field theories, which leads to a new type of the latter, nonlocal noncommutative field theories.

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Section: Pulsar Kicks Due To Chiral Shiftmentioning

confidence: 93%

Quantum field theory in a magnetic field: From quantum chromodynamics to graphene and Dirac semimetals

2015

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“…The CCSN dynamics obtained in our simulation is aligned with the neutrino-heating explosion mechanism although the computation is not long enough to make a firm conclusion. Since we did not incorporate magnetic fields, rotations and non-standard neutrino physics in this simulation, the result presented in this paper is distinct from other mechanisms to produce PNS proper motions that advocate asymmetric neutrino emissions (Bisnovatyi-Kogan 1993;Fuller et al 2003;Kusenko et al 2008;Sagert & Schaffner-Bielich 2008). Interestingly, although the property of asymmetric neutrino emissions is the same as in LESA (leptonemission self-sustained asymmetry), the origin may be different from those discussed in Tamborra et al (2014); Glas et al (2018); Powell & Müller (2018).…”

Section: Introductionmentioning

confidence: 90%

Possible Early Linear Acceleration of Proto-neutron Stars via Asymmetric Neutrino Emission in Core-collapse Supernovae

Nagakura

Sumiyoshi

Yamada

2019

ApJL

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In this Letter, we present the result of an axisymmetric CCSN simulation conducted with appropriate treatments of neutrino transport and proper motions of proto-neutron star (PNS), in which a remarkable PNS acceleration is observed in association with asymmetric neutrino emissions by the time of 300ms after bounce. We find that these asymmetric neutrino emissions play important roles in the acceleration of PNS in this phase. The correlation between the PNS proper motion and the asymmetric ejecta is similar to that in the neutron star (NS) kick of hydrodynamic origin. Both electron-type neutrinos (ν e ) and their anti-particles (ν e ) have ∼ 10% level of asymmetry between the northern and southern hemispheres, while other heavy-leptonic neutrinos (ν x ) have much smaller asymmetry of ∼ 1%. The emissions ofν e and ν x are higher in the hemisphere of stronger shock expansion whereas the ν e emission is enhanced in the opposite hemisphere: in total the neutrinos carry some linear momentum to the hemisphere of the stronger shock expansion. The asymmetry is attributed to the non-spherical distribution of electron-fraction (Y e ) in the envelope of PNS. Although it is similar to LESA (lepton-emission self-sustained asymmetry), the Y e asymmetry seems to be associated with the PNS motion: the latter triggers lateral circular motions in the envelope of PNS by breaking symmetry of the matter distribution there, which are then sustained by a combination of convection, lateral neutrino diffusion and matter-pressure gradient. Our findings may have an influence on the current theories on the NS kick mechanism although long-term simulations are required to assess their impact on the later evolution.

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“…Compact objects are thought to receive a kick at birth (natal kick), because of asymmetric supernova (SN) explosions (e.g Janka & Mueller 1994;Burrows & Hayes 1996) or anisotropic emission of neutrinos (e.g. Woosley 1987;Bisnovatyi-Kogan 1993;Fryer & Kusenko 2006;Kusenko et al 2008;Sagert & Schaffner-Bielich 2008). In addition, if the SN occurs in a binary star, we expect the so-called Blaauw kick to affect the orbital properties of the binary system, even if mass loss is completely symmetric (Blaauw 1961).…”

Section: Introductionmentioning

confidence: 99%

Revising Natal Kick Prescriptions in Population Synthesis Simulations

Giacobbo

Mapelli

2020

ApJ

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Natal kicks are matter of debate and significantly affect the merger rate density of compact objects. Here, we present a new simple formalism for natal kicks of neutron stars (NSs) and black holes (BHs). We describe the magnitude of the kick as v kick ∝ f H05 m ej m −1 rem , where f H05 is a normalization factor, drawn from a Maxwellian distribution with one-dimensional root-mean-square velocity σ = 265 km s −1 , m ej is the mass of the supernova (SN) ejecta and m rem is the mass of the compact object. This formalism matches the proper motions of young Galactic pulsars and can naturally account for the differences between core-collapse SNe of single stars, electron-capture SNe and ultra-stripped SNe occurring in interacting binaries. Finally, we use our new kick formalism to estimate the local merger rate density of binary NSs (R BNS ), BH-NS binaries (R BHNS ) and binary BHs (R BBH ), based on the cosmic star formation rate density and metallicity evolution. In our fiducial model, we find R BNS ∼ 600 Gpc −3 yr −1 , R BHNS ∼ 10 Gpc −3 yr −1 and R BBH ∼ 50 Gpc −3 yr −1 , fairly consistent with the numbers inferred from the LIGO-Virgo collaboration.

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Pulsar kicks by anisotropic neutrino emission from quark matter in strong magnetic fields

Cited by 37 publications

References 88 publications

Quantum field theory in a magnetic field: From quantum chromodynamics to graphene and Dirac semimetals

Quantum field theory in a magnetic field: From quantum chromodynamics to graphene and Dirac semimetals

Possible Early Linear Acceleration of Proto-neutron Stars via Asymmetric Neutrino Emission in Core-collapse Supernovae

Revising Natal Kick Prescriptions in Population Synthesis Simulations

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