Exploring jet-launching conditions for supergiant fast X-ray transients

García, Federico; Aguilera, Deborah N.; Romero, Gustavo E.

doi:10.1051/0004-6361/201323157

Cited by 3 publications

(3 citation statements)

References 54 publications

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“…However, in Fig. 2, we show that the magnetic field decay due to the Hall effect plus the Ohmic diffusion is similar to the magnetic field decay due to the Ohmic diffusion only, allowing us to neglect the Hall effect in our calculations, which, in turn, allows us to assume a purely dipolar geometry for the magnetic field (Konar 1997;Sengupta 1998;García et al 2014) as a simplifying case.…”

Section: The Hall Effect and The Geometry Of The Magnetic Fieldmentioning

confidence: 84%

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Magnetic field decay in black widow pulsars

Mendes

Avellar

Horvath

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We study in this work the evolution of the magnetic field in 'redback-black widow' pulsars. Evolutionary calculations of these 'spider' systems suggest that first the accretion operates in the redback stage, and later the companion star ablates matter due to winds from the recycled pulsar. It is generally believed that mass accretion by the pulsar results in a rapid decay of the magnetic field when compared to the rate of an isolated neutron star. We study the evolution of the magnetic field in black widow pulsars by solving numerically the induction equation using the modified Crank-Nicolson method with intermittent episodes of mass accretion on to the neutron star. Our results show that the magnetic field does not fall below a minimum value ('bottom field') in spite of the long evolution time of the black widow systems, extending the previous conclusions for much younger low-mass X-ray binary systems. We find that in this scenario, the magnetic field decay is dominated by the accretion rate, and that the existence of a bottom field is likely related to the fact that the surface temperature of the pulsar does not decay as predicted by the current cooling models. We also observe that the impurity of the pulsar crust is not a dominant factor in the decay of magnetic field for the long evolution time of black widow systems.

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Section: The Hall Effect and The Geometry Of The Magnetic Fieldmentioning

confidence: 84%

“…In this work, we consider that the magnetic field is anchored in the crust of neutron star and does not reach the core. Even if it seems an important restriction, we should remark that the magnetic field decay physics is not sensitive to the unknown exact composition of the core (García, Aguilera & Romero 2014).…”

Section: Density Profilementioning

confidence: 99%

Magnetic field decay in black widow pulsars

Mendes

Avellar

Horvath

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…However, as observed in systems such as Cir X-1 [29], transient jets can be produced upon a sufficiently low ( 10 8 G) magnetic field magnitude at the surface of the NS [30], based on a similar accretion/ejection mechanism as microquasars. In supergiant fast X-ray transients (HMXB composed of a NS and exhibiting rapid hard X-ray flux evolution) magnetic field decay could also allow for relativistic particle injection when large clumps of matter are accreted by the NS [31], producing again a potential correlation between hard X-ray flares and particle acceleration.…”

Section: Selection Of Outburst Periodsmentioning

confidence: 99%

Time-dependent search for neutrino emission from X-ray binaries with the ANTARES telescope

Albert¹,

André²,

Anton³

et al. 2017

J. Cosmol. Astropart. Phys.

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ANTARES is currently the largest neutrino telescope operating in the NorthernHemisphere, aiming at the detection of high-energy neutrinos from astrophysical sources. Neutrino telescopes constantly monitor at least one complete hemisphere of the sky, and are thus well-suited to detect neutrinos produced in transient astrophysical sources. A timedependent search has been applied to a list of 33 X-ray binaries undergoing high flaring activities in satellite data (RXTE/ASM, MAXI and Swift/BAT) and during hardness transition states in the 2008-2012 period. The background originating from interactions of charged cosmic rays in the Earth's atmosphere is drastically reduced by requiring a directional and temporal coincidence with astrophysical phenomena. The results of this search are presented together with comparisons between the neutrino flux upper limits and the neutrino flux predictions from astrophysical models. The neutrino flux upper limits resulting from this search limit the jet parameter space for some astrophysical models.

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Modelling the expected very high energy γ-ray emission from accreting neutron stars in X-ray binaries

Ducci,

Romano,

Vercellone

et al. 2023

Monthly Notices of the Royal Astronomical Society

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The detection of γ −ray emission from accreting pulsars in X-ray binaries (XRBs) has long been sought after. For some high-mass X-ray binaries (HMXBs), marginal detections have recently been reported. Regardless of whether these will be confirmed or not, future telescopes operating in the γ −ray band could offer the sensitivity needed to achieve solid detections and possibly spectra. In view of future observational advances, we explored the expected emission above 10 GeV from XRBs, based on the Cheng & Ruderman model, where γ −ray photons are produced by the decay of π0 originated by protons accelerated in the magnetosphere of an accreting pulsar fed by an accretion disc. We improved this model by considering, through Monte Carlo simulations, the development of cascades inside of and outside the accretion disc, taking into account pair and photon production processes that involve interaction with nuclei, X-ray photons from the accretion disc, and the magnetic field. We produced grids of solutions for different input parameter values of the X-ray luminosity (Lx), magnetic field strength (B), and for different properties of the region where acceleration occurs. We found that the γ −ray luminosity spans more than five orders of magnitude, with a maximum of ∼1035 erg s−1. The γ −ray spectra show a large variety of shapes: some have most of the emission below ∼100 GeV, others are harder (emission up to 10−100 TeV). We compared our results with Fermi/LAT and VERITAS detections and upper-limits of two HMXBs: A0535+26 and GRO J1008−57. More consequential comparisons will be possible when more sensitive instruments will be operational in the coming years.

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Exploring jet-launching conditions for supergiant fast X-ray transients

Cited by 3 publications

References 54 publications

Magnetic field decay in black widow pulsars

Magnetic field decay in black widow pulsars

Time-dependent search for neutrino emission from X-ray binaries with the ANTARES telescope

Modelling the expected very high energy γ-ray emission from accreting neutron stars in X-ray binaries

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