The minimum magnetic field of millisecond pulsars calculated according to accretion: application to the X-ray neutron star SAX J1808.4–3658 in a low-mass X-ray binary

Pan, Y. Y.; Zhang, Chengmin; Song, Liming; Wang, Na; Li, Di; Yang, Yanji

doi:10.1093/mnras/sty1851

Cited by 10 publications

(5 citation statements)

References 51 publications

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“…Using the R in value found in FB, we obtained a magnetic field strength of B ࣠ 1.8 × 10 8 G, where the upper bound considers both the FB and the NB. This result is consistent with the magnetic field strengths of other accreting NS-LMXBs (Cackett et al 2009 ;Mukherjee et al 2015 ;Ludlam et al 2017Ludlam et al , 2019Ludlam et al , 2020Ludlam et al , 2021Pan et al 2018 ;Sharma et al 2020 ;Mondal et al 2022 ).…”

Section: Inner Disc Radii and Magnetic Field Strengthsupporting

confidence: 90%

Relativistic X-ray reflection and photoionized absorption in the neutron star low-mass X-ray binary GX 13+1

Saavedra

García

Fogantini

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We analysed a dedicated NuSTAR observation of the neutron-star low-mass X-ray binary Z-source GX 13+1 to study the timing and spectral properties of the source. From the colour-colour diagram, we conclude that during that observation the source transitioned from the normal branch to the flaring branch. We fitted the spectra of the source in each branch with a model consisting of an accretion disc, a Comptonised blackbody, relativistic reflection (relxillNS), and photo-ionised absorption (warmabs). Thanks to the combination of the large effective area and good energy resolution of NuSTAR at high energies, we found evidence of relativistic reflection in both the Fe K line profile, and the Compton hump present in the 10–25 keV energy range. The inner disc radius is Rin ≲ 9.6 rg, which allowed us to further constrain the magnetic field strength to B ≲ 1.8 × 108 G. We also found evidence for the presence of a hot wind leading to photo-ionised absorption of Fe and Ni, with a Ni overabundance of ∼6 times solar. From the spectral fits, we find that the distance between the ionising source and the slab of ionised absorbing material is ∼4 − 40 × 105 km. We also found that the width of the boundary layer extends ∼3 km above the surface of a neutron star, which yielded a neutron-star radius RNS ≲ 16 km. The scenario inferred from the spectral modelling becomes self-consistent only for high electron densities in the accretion disk, ne ∼ 1022 − 1023 cm−3, as expected for a Shakura-Sunyaev disc, and significantly above the densities provided by relxillNS models. These results have implications for our understanding of the physical conditions in GX 13+1.

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Section: Inner Disc Radii and Magnetic Field Strengthsupporting

confidence: 90%

Relativistic X-ray reflection and photoionized absorption in the neutron star low-mass X-ray binary GX 13+1

Saavedra

García

Fogantini

et al. 2023

Monthly Notices of the Royal Astronomical Society

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“…Nevertheless high accretion rates lead to a rapid decrease of the magnetic field strength and for low magnetic field strengths the angular momentum transfer is slower (Bonanno & Urpin 2015). In order to spin up to millisecond periods a limiting magnetic field strength and accretion rate can be set as a result of the amount of time a neutron star can spend accreting matter being limited by the age of the universe (Pan et al 2018). For a neutron star with a mass of 1.4 M , a radius of 10 km and a minimum accretion rate of 7.26 × 10 −11 M yr −1 we get a minimum magnetic field strength of B surf 3.3 × 10 7 G, which is consistent with the observed pulsar population.…”

Section: Discussionmentioning

confidence: 99%

Detection and Timing of Gamma-Ray Pulsations from the 707 Hz Pulsar J0952−0607

Nieder

Clark

Bassa

et al. 2019

ApJ

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The Low-Frequency Array radio telescope discovered the 707 Hz binary millisecond pulsar (MSP) J0952−0607 in a targeted radio pulsation search of an unidentified Fermi gamma-ray source. This source shows a weak energy flux of F γ = 2.6 × 10 −12 erg cm −2 s −1 in the energy range between 100 MeV and 100 GeV. Here we report the detection of pulsed gamma-ray emission from PSR J0952−0607 in a very sensitive gamma-ray pulsation search. The pulsar's rotational, binary, and astrometric properties are measured over seven years of Fermi-Large Area Telescope data. For this we take into account the uncertainty on the shape of the gamma-ray pulse profile. We present an updated radio-timing solution now spanning more than two years and show results from optical modeling of the black-widow-type companion based on new multi-band photometric data taken with HiPERCAM on the Gran Telescopio Canarias on La Palma and ULTRACAM on the New Technology Telescope at ESO La Silla a) . PSR J0952−0607 is now the fastest-spinning pulsar for which the intrinsic spindown rate has been reliably constrained (Ṗ int 4.6 × 10 −21 s s −1 ). The inferred surface magnetic field strength of B surf 8.2 × 10 7 G is among the ten lowest of all known pulsars. This discovery is another example of an extremely fast spinning black-widow pulsar hiding within an unidentified Fermi gamma-ray source. In the future such systems might help to pin down the maximum spin frequency and the minimum surface magnetic field strength of MSPs.

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“…And the accretion rate is with two limitations: the maximum value corresponds to its ultra luminosity X = 4.7 × 10 39 erg s −1 . And the minimum value is min ≃ 4.6 × 10 15 g s −1 , which is also the minimum accretion rate required for a MSP forming in the binary system (Pan et al 2018). The corresponding bottom magnetic fields are f,max ≃ 1.73×10 9 G and f,min ≃ 2.34 × 10 7 G, respectively.…”

Section: The Evolved Resultsmentioning

confidence: 94%

Study on the magnetic field strength of NGC 300 ULX1

Pan,

Li,

Zhang

et al. 2022

Preprint

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NGC 300 ULX1 is a pulsating ultraluminous X-ray source (PULX) with the longest spin period of ≃ 31.6 s and a high spin-up rate of ≃ −5.56 × 10 −7 s s −1 that is ever seen in the confirmed PULXs. In this paper, the inferred magnetic field of NGC 300 ULX1 is ∼ 3.0 × 10 14 G using the recent observed parameters after its first detection of pulsations. According to the evolved simulation of the magnetic field and the spin period, it will become a recycled pulsar or a millisecond pulsar under the conditions of the companion mass and the accretion rate limitation. We suggest that NGC 300 ULX1 is an accreting magnetar accounting for its super Eddington luminosity. We also propose that there might be other accreting magnetars in the confirmed PULXs. Such PULXs will be helpful for understanding the magnetar evolution and the millisecond pulsar formation whose magnetic field is stronger than ∼ 10 9 G.

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The minimum magnetic field of millisecond pulsars calculated according to accretion: application to the X-ray neutron star SAX J1808.4–3658 in a low-mass X-ray binary

Cited by 10 publications

References 51 publications

Relativistic X-ray reflection and photoionized absorption in the neutron star low-mass X-ray binary GX 13+1

Relativistic X-ray reflection and photoionized absorption in the neutron star low-mass X-ray binary GX 13+1

Detection and Timing of Gamma-Ray Pulsations from the 707 Hz Pulsar J0952−0607

Study on the magnetic field strength of NGC 300 ULX1

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