Neutron stars in the laboratory

Graber, Vanessa; Andersson, Nils; Hogg, Michael

doi:10.1142/s0218271817300154

Cited by 60 publications

(58 citation statements)

References 462 publications

(734 reference statements)

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“…Refs. [7,110,111,112,113,114] for recent reviews; see also Sedrakian&Haskell in this volume). For all these reasons, the inner crust of a neutron star is a unique environment, whose extreme conditions imposed by the huge gravitational field of the star cannot be reproduced in terrestrial laboratories.…”

Section: Inner Crustmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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Formed in the aftermath of gravitational core-collapse supernova explosions, neutron stars are unique cosmic laboratories for probing the properties of matter under extreme conditions that cannot be reproduced in terrestrial laboratories. The interior of a neutron star, endowed with the highest magnetic fields known and with densities spanning about ten orders of magnitude from the surface to the centre, is predicted to exhibit various phases of dense strongly interacting matter, whose physics is reviewed in this chapter. The outer layers of a neutron star consist of a solid nuclear crust, permeated by a neutron ocean in its densest region, possibly on top of a nuclear "pasta" mantle. The properties of these layers and of the homogeneous isospin asymmetric nuclear matter beneath constituting the outer core may still be constrained by terrestrial experiments. The inner core of highly degenerate, strongly interacting matter poses a few puzzles and questions which are reviewed here together with perspectives for their resolution. Consequences of the dense-matter phases for observables such the neutron-star mass-radius relationship and the prospects to uncover their structure with modern observational programmes are touched upon.

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Section: Inner Crustmentioning

confidence: 99%

Phases of Dense Matter in Compact Stars

Blaschke

Chamel

2018

The Physics and Astrophysics of Neutron Stars

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“…See e.g. Graber et al (2017) for typical length scale estimates. For a fiducial magnetic field strength of B ≈ 10 12 G, the inter-fluxtube distance is d ft ≈ 10 3 fm, leading to pinning forces per unit length of f ≈ 8 × 10 15 dyn cm −1 .…”

Section: Glitch Rise Modelingmentioning

confidence: 99%

Glitch Rises as a Test for Rapid Superfluid Coupling in Neutron Stars

Graber

Cumming

Andersson

2018

ApJ

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Pulsar glitches provide a unique way to study neutron star microphysics because short post-glitch dynamics are directly linked to strong frictional processes on small scales. To illustrate this connection between macroscopic observables and microphysics, we review calculations of vortex interactions focusing on Kelvin wave excitations and determine the corresponding mutual friction strength for realistic microscopic parameters in the inner crust. These density-dependent crustal coupling profiles are combined with a simplified treatment of the core coupling and implemented in a three-component neutron star model to construct a predictive framework for glitch rises. As a result of the density-dependent dynamics, we find the superfluid to transfer angular momentum to different parts of the crust and the core on different timescales. This can cause the spin frequency change to become non-monotonic in time, allowing for a maximum value much larger than the measured glitch size, as well as a delay in the recovery. The exact shape of the calculated glitch rise is strongly dependent on the relative strength between the crust and core mutual friction, providing the means to probe not only the crustal superfluid but also the deeper neutron star interior. To demonstrate the potential of this approach, we compare our predictive model with the first pulse-to-pulse observations recorded during the December 2016 glitch of the Vela pulsar. Our analysis suggests that the glitch rise behavior is relatively insensitive to the crustal mutual friction strength as long as B 10 −3 , while being strongly dependent on the core coupling strength, which we find to be in the range 3 × 10 −5 B core 10 −4 .

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“…INTRODUCTIONNeutron stars are interesting astrophysical objects whose phenomena are induced by combinations of fundamental forces, i.e., strong interaction, weak interaction, electromagnetic interaction and gravitation (see Refs. [1,2] for recent reviews). Studying neutron stars by several different signals can open a new approach to unveil the interiors in neutron stars.…”

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confidence: 99%

Phase structure of neutron P23 superfluids in strong magnetic fields in neutron stars

2019

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We discuss the effect of a strong magnetic field on neutron 3 P2 superfluidity. Based on the attraction in the 3 P2 pair of two neutrons, we derive the Ginzburg-Landau equation in the pathintegral formalism by adopting the bosonization technique and leave the next-to-leading order in the expansion of the magnetic field B. We determine the (T, B) phase diagram with temperature T , comprising three phases: the uniaxial nematic (UN) phase for B = 0, D2-biaxial nematic (BN) and D4-BN phases in finite B and strong B such as magnetars, respectively, where D2 and D4 are dihedral groups. We find that, compared with the leading order in the magnetic field known before, the region of the D2-BN phase in the (T, B) plane is extended by the effect of the nextto-leading-order terms of the magnetic field. We also present the thermodynamic properties, such as heat capacities and spin susceptibility, and find that the spin susceptibility exhibits anisotropies in the UN, D2-BN, and D4-BN phases. This information will be useful to understand the internal structures of magnetars. I. INTRODUCTIONNeutron stars are interesting astrophysical objects whose phenomena are induced by combinations of fundamental forces, i.e., strong interaction, weak interaction, electromagnetic interaction and gravitation (see Refs. [1,2] for recent reviews). Studying neutron stars by several different signals can open a new approach to unveil the interiors in neutron stars. It was epoch-making that gravitational waves from neutron star merger were observed directly [3]. One of the most important properties of neutron stars is accompanied by a strong magnetic field. It is known that the magnitude of the magnetic field is around 10 12 G in standard neutron stars, and, in magnetars, it can reach about 10 15 G at the surface and may reach even larger values in the inside (see Refs. [4,5] for reviews on magnetars). As for the origin of the strong magnetic fields, researchers have studied several mechanisms such as spin-dependent interactions between neutrons [6-9], 1 the pion domain wall [11,12], the spin polarization in quark-matter core [13][14][15] and so on. In neutron matter, the influence of the magnetic field on a neutron is provided by a finite magnetic moment, µ n = −(γ n /2)σ with the gyromagnetic ratio of a neutron, γ n = 1.2 × 10 −13 MeV/T (in natural units, = c = 1), and the Pauli matrices for the neutron spin σ. The interaction between the neutron and the magnetic field (B) supplies the energy splitting between the spin-up state and the spin-down state for a neutron, −µ n ·B. For example, the strong magnetic field |B| ∼ 10 15 G in magnetars gives the mass splitting about O(10) keV (notice the unit relation, 1 T = 10 4 G).The dominant ingredient in neutron stars is the neutron matter, and it exists as superfluidity with a small admixture of superconducting protons and normal electrons (see Refs. [16,17] for recent reviews). In relation to the observations of neutron stars, it is considered that the neutron superfluidity affects relaxation time afte...

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Neutron stars in the laboratory

Cited by 60 publications

References 462 publications

Phases of Dense Matter in Compact Stars

Phases of Dense Matter in Compact Stars

Glitch Rises as a Test for Rapid Superfluid Coupling in Neutron Stars

Phase structure of neutron P23 superfluids in strong magnetic fields in neutron stars

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