Evolution of Neutron Star Magnetic Fields

Igoshev, Andrei P.; Попов, С. Б.; Hollerbach, Rainer

doi:10.3390/universe7090351

Cited by 67 publications

(45 citation statements)

References 225 publications

(318 reference statements)

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“…Such explanations imply that B0950 is a very peculiar object among other old ordinary pulsars. The required decay timescale is significantly shorter than the Ohmic dissipation timescale of 10 Myr caused by lattice impurities of the nuclear crystal in the NS crust (see Igoshev et al 2021 for a recent review of NS magnetic field evolution). Recent 2D and 3D simulations of magneto-thermal evolution of NSs, performed mainly for super-strong magnetic fields B ∼ 10 14 − 10 15 G typical for magnetars, show that short timescales are possible if the non-linear Hall effect is taken into account and the presence of superstrong toroidal field component inside the crust is assumed (e.g., Geppert & Viganò 2014;Gourgouliatos & Hollerbach 2018).…”

Section: Discussionmentioning

confidence: 99%

Thermal and nonthermal emission in the optical-UV spectrum of PSR B0950+08

Abramkin,

Pavlov,

Shibanov

et al. 2021

Preprint

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Based on recent Hubble Space Telescope (HST) observations in far-UV and groundbased observations in optical bands, Pavlov and colleagues have revealed a thermal component in the spectrum of the old pulsar B0950+08 (spin-down age 17.5 Myr) and estimated a neutron star (NS) surface temperature of (1-3) × 10 5 K. Our new HST observations in the optical have allowed us to resolve the pulsar from a close-by galaxy and measure the optical fluxes more accurately. Using the newly measured fluxes and a new calibration of the HST's far-UV detector, we fit the optical-UV pulsar's spectrum with a model that consists of a nonthermal power-law (f ν ∝ ν α ) and a thermal blackbody components. We obtained the spectral slope α = −0.3 ± 0.3, considerably flatter than found from groundbased observations, and the best-fit temperature in the range of (6-12) × 10 4 K (as seen by a distant observer), depending on interstellar extinction and NS radius. The temperature is lower than reported previously, but still much higher than predicted by NS passive cooling scenarios for such an old pulsar. This means that some heating mechanisms operate in NSs, e.g., caused by interaction of the faster rotating neutron superfluid with the slower rotating normal matter in the inner crust of the NS.

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Section: Discussionmentioning

confidence: 99%

Thermal and nonthermal emission in the optical-UV spectrum of PSR B0950+08

Abramkin,

Pavlov,

Shibanov

et al. 2021

Preprint

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“…Therefore, the surface thermal distribution is strongly affected by magnetic field configuration in the NS crust. The surface temperature distribution is an important ingredient to model the quiescent emission of magnetars and eventually to probe their magnetic fields and emission properties; see for example a recent review [156].…”

Section: Magneto-thermal Evolutionmentioning

confidence: 99%

Magnetic Field Evolution in Neutron Star Crusts: Beyond the Hall Effect

Gourgouliatos

Grandis²,

Igoshev

2022

Symmetry

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Neutron stars host the strongest magnetic fields that we know of in the Universe. Their magnetic fields are the main means of generating their radiation, either magnetospheric or through the crust. Moreover, the evolution of the magnetic field has been intimately related to explosive events of magnetars, which host strong magnetic fields, and their persistent thermal emission. The evolution of the magnetic field in the crusts of neutron stars has been described within the framework of the Hall effect and Ohmic dissipation. Yet, this description is limited by the fact that the Maxwell stresses exerted on the crusts of strongly magnetised neutron stars may lead to failure and temperature variations. In the former case, a failed crust does not completely fulfil the necessary conditions for the Hall effect. In the latter, the variations of temperature are strongly related to the magnetic field evolution. Finally, sharp gradients of the star’s temperature may activate battery terms and alter the magnetic field structure, especially in weakly magnetised neutron stars. In this review, we discuss the recent progress made on these effects. We argue that these phenomena are likely to provide novel insight into our understanding of neutron stars and their observable properties.

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“…Magnetic field decay caused by accretion is usually invoked to explain the low field of NSs in low-mass X-ray binaries (Shibazaki et al 1989;Romani 1990;Konar & Bhattacharya 1997;Mukherjee 2017). Following the review of Igoshev et al (2021), we adopt a simple model of magnetic field decay:…”

Section: A Ns Spun Up By Accretion?mentioning

confidence: 99%

Quasi periodic whispers from a transient ULX in M\,101: signatures of a fast-spinning neutron star?

Urquhart,

Soria,

Di Stefano

et al. 2022

Preprint

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We have studied the unusual time variability of an ultraluminous X-ray source in M 101, 4XMM J140314.2+541806 (henceforth, J1403), using Chandra and XMM-Newton data. Over the last two decades, J1403 has shown short-duration outbursts with an X-ray luminosity ∼1-3 ×10 39 erg s −1 , and longer intervals at luminosities ∼0.5-1 ×10 38 erg s −1 . The bimodal behaviour and fast outburst evolution (sometimes only a few days) are more consistent with an accretor/propeller scenario for a neutron star than with the canonical outburst cycles of stellar-mass black holes. If this scenario is correct, the luminosities in the accretor and propeller states suggest a fast spin (𝑃 ≈ 5 ms) and a low surface magnetic field (𝐵 ∼ 10 10 G), despite our identification of J1403 as a high-mass X-ray binary. The most striking property of J1403 is the presence of strong ∼600-s quasi periodic oscillations (QPOs), mostly around frequencies of ≈1.3-1.8 mHz, found at several epochs during the ultraluminous regime. We illustrate the properties of such QPOs, in particular their frequency and amplitude changes between and within observations, with a variety of techniques (Fast Fourier Transforms, Lomb-Scargle periodograms, weighted wavelet Z-transform analysis). The QPO frequency range <10 mHz is an almost unexplored regime in X-ray binaries and ultraluminous X-ray sources. We compare our findings with the (few) examples of very low frequency variability found in other accreting sources, and discuss possible explanations (Lense-Thirring precession of the inner flow or outflow; radiation pressure limit-cycle instability; marginally stable He burning on the neutron star surface).

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Evolution of Neutron Star Magnetic Fields

Cited by 67 publications

References 225 publications

Thermal and nonthermal emission in the optical-UV spectrum of PSR B0950+08

Thermal and nonthermal emission in the optical-UV spectrum of PSR B0950+08

Magnetic Field Evolution in Neutron Star Crusts: Beyond the Hall Effect

Quasi periodic whispers from a transient ULX in M\,101: signatures of a fast-spinning neutron star?

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