Neutron Star Crusts With Magnetic Fields

AbstractThe properties of plasma in neutron star crusts with strong magnetic fields B = 1010 − 1013 G are reviewed: thermodynamic properties (equation of state, entropy, specific heat), transport properties (electron thermal and electrical conductivity of degenerate electron gas, radiative thermal conductivity of very surface nondegenerate layers) and neutrino energy losses. Classical effects of electron Larmor rotation in a magnetic field are considered as well as quantum effects of the electron motion (Landau levels). The influence of the magnetic fields on density and temperature profiles in the surface layers of neutron stars and on neutron star cooling is briefly discussed.

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Thermal luminosities of cooling neutron stars

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1871 ◽

2020 ◽

Vol 496 (4) ◽

pp. 5052-5071 ◽

Cited By ~ 3

Author(s):

A Y Potekhin ◽

D A Zyuzin ◽

D G Yakovlev ◽

M V Beznogov ◽

Yu A Shibanov

Keyword(s):

Spectral Analysis ◽

Neutron Star ◽

Magnetic Fields ◽

Neutron Stars ◽

Cooling Curves ◽

Middle Aged ◽

Superdense Matter ◽

Strong Magnetic Fields ◽

Stellar Core ◽

Neutron Star Cooling

ABSTRACT Ages and thermal luminosities of neutron stars, inferred from observations, can be interpreted with the aid of the neutron star cooling theory to gain information on the properties of superdense matter in neutron-star interiors. We present a survey of estimated ages, surface temperatures, and thermal luminosities of middle-aged neutron stars with relatively weak or moderately strong magnetic fields, which can be useful for these purposes. The catalogue includes results selected from the literature, supplemented with new results of spectral analysis of a few cooling neutron stars. The data are compared with the theory. We show that overall agreement of theoretical cooling curves with observations improves substantially for models where neutron superfluidity in stellar core is weak.

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Electromagnetic Polarization in Partially Ionized Plasmas with Strong Magnetic Fields and Neutron Star Atmosphere Models

The Astrophysical Journal ◽

10.1086/422679 ◽

2004 ◽

Vol 612 (2) ◽

pp. 1034-1043 ◽

Cited By ~ 59

Author(s):

Alexander Y. Potekhin ◽

Dong Lai ◽

Gilles Chabrier ◽

Wynn C. G. Ho

Keyword(s):

Neutron Star ◽

Magnetic Fields ◽

Strong Magnetic Fields ◽

Ionized Plasmas ◽

Partially Ionized Plasmas ◽

Partially Ionized

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Delta baryons in neutron-star matter under strong magnetic fields

The European Physical Journal A ◽

10.1140/epja/s10050-021-00532-6 ◽

2021 ◽

Vol 57 (7) ◽

Author(s):

Veronica Dexheimer ◽

Kauan D. Marquez ◽

Débora P. Menezes

Keyword(s):

Neutron Star ◽

Magnetic Fields ◽

Neutron Star Matter ◽

Strong Magnetic Fields

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Onset of superconductivity and retention of magnetic fields in cooling neutron stars

Proceedings of the International Astronomical Union ◽

10.1017/s174392131700970x ◽

2017 ◽

Vol 13 (S337) ◽

pp. 213-216

Author(s):

Wynn C. G. Ho ◽

Nils Andersson ◽

Vanessa Graber

Keyword(s):

Magnetic Field ◽

Neutron Star ◽

Magnetic Fields ◽

Neutron Stars ◽

Minimum Energy ◽

Meissner Effect ◽

Energy Conditions ◽

Field Diffusion ◽

Neutron Star Cooling ◽

Proton Pairing

AbstractA superconductor of paired protons is thought to form in the core of neutron stars soon after their birth. Minimum energy conditions suggest that magnetic flux is expelled from the superconducting region due to the Meissner effect, such that the neutron star core retains or is largely devoid of magnetic fields for some nuclear equation of state and proton pairing models. We show via neutron star cooling simulations that the superconducting region expands faster than flux is expected to be expelled because cooling timescales are much shorter than timescales of magnetic field diffusion. Thus magnetic fields remain in the bulk of the neutron star core for at least 106 − 107yr. We estimate the size of flux free regions at 107yr to be ≲ 100m for a magnetic field of 1011G and possibly smaller for stronger field strengths.

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