Landau Quantisation of Electron Motion in the Crust of Highly Magnetised Neutron Stars

Chamel, Nicolas; Mutafchieva, Y. D.; Stoyanov, Zh. K.; Mihailov, L.M.; Pavlov, R. L.

doi:10.1007/978-3-319-50255-7_11

Cited by 3 publications

(4 citation statements)

References 36 publications

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“…We have previously shown that the composition and the equation of state of the outer crust of a neutron star can be drastically modified by such high magnetic fields due to Rabi quantization of electron motion [11,12,13,14]. In this paper, we present new results using updated experimental atomic mass data.…”

Section: Introductionmentioning

confidence: 87%

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Towards a unified description of magnetar crusts

Mutafchieva¹,

Stoyanov²,

Chamel³

2019

AIP Conference Proceedings

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The properties of the crust of a neutron star can be significantly altered by the presence of a high magnetic field. The effects of Rabi quantization of electron motion on the equation of state and on the composition of the crust are studied. Both the outer and inner regions are described in a unified and consistent way by extending the neutron-star crust models developed by the Brussels-Montreal collaboration. The first numerical results obtained for different magnetic field strengths are presented.

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Section: Introductionmentioning

confidence: 87%

“…Determining the equilibrium state in the weakly quantizing regime can be numerically tricky due to the occurrence of quantum oscillations (see, e.g., Ref. [14]).…”

Section: Inner Crustmentioning

confidence: 99%

Towards a unified description of magnetar crusts

Mutafchieva¹,

Stoyanov²,

Chamel³

2019

AIP Conference Proceedings

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“…B < B rel where B rel ≡ (m 2 e c 3 )/(e ) 4.41 × 10 13 G, the internal constitution of their outer crust is essentially the same as in the absence of magnetic fields except near the stellar surface. For higher magnetic fields, B B rel as measured in SGRs, AXPs, and some radio pulsars, the composition changes depending on the magnetic field strength [6,7,8,9]. In particular, the maximum baryon number densityn max 1 up to which a nuclide (A 1 , Z 1 ) is present exhibit universal quantum oscillations as a function of the magnetic field strength, and increases almost linearly in the strongly quantizing regime [9,10,11].…”

Section: Model Of the Outer Crustmentioning

confidence: 97%

“…For higher magnetic fields, B B rel as measured in SGRs, AXPs, and some radio pulsars, the composition changes depending on the magnetic field strength [6,7,8,9]. In particular, the maximum baryon number densityn max 1 up to which a nuclide (A 1 , Z 1 ) is present exhibit universal quantum oscillations as a function of the magnetic field strength, and increases almost linearly in the strongly quantizing regime [9,10,11]. For comparison, we shall thus consider two extreme situations: i) unmagnetized neutron stars with B ≡ B/B rel = 0, and ii) highlymagnetized neutron stars with a strongly quantizing field B = 2000 (in any region of the outer crust, electrons are confined to the lowest energy level).…”

Section: Model Of the Outer Crustmentioning

confidence: 99%

Stratification of the outer crust of magnetars and nuclear abundances

Stoyanov¹,

Mutafchieva²,

Chamel³

2019

AIP Conference Proceedings

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The r-process triggered by the decompression of ejected crustal materials from binary neutron star mergers has been recently confirmed by observations of the kilonova following the detection of gravitational waves from GW170817. Isolated neutron stars endowed with very high magnetic fields, so called magnetars, might be also at the origin of r-process nucleosynthesis since some material is ejected during giant flares. The final abundance distribution depends on the crustal composition. Making use of the latest experimental nuclear mass data supplemented with microscopic models, we show that the presence of a high magnetic field can have a significant influence on the stratification of neutron-star crusts and on the nuclear abundances of the different layers.

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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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Landau Quantisation of Electron Motion in the Crust of Highly Magnetised Neutron Stars

Cited by 3 publications

References 36 publications

Towards a unified description of magnetar crusts

Towards a unified description of magnetar crusts

Stratification of the outer crust of magnetars and nuclear abundances

Phases of Dense Matter in Compact Stars

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