Testing the accretion-induced field-decay and spin-up model for recycled pulsars

Wang, J.; Zhang, Chengmin; Chang, Hsiang-Kuang

doi:10.1051/0004-6361/201116524

Cited by 3 publications

(3 citation statements)

References 44 publications

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“…Old NSs in low mass X-ray binaries have magnetic fields ∼ 10 9 G which is three orders of magnitude smaller than fields inferred for young NSs in high mass X-ray binaries and young isolated radio pulsars. The magnetic moments of NSs in binary systems is inversely correlated with accretion history (Taam & Three distinct mechanisms have been suggested for the reduction of the magnetic field: (i) accretion induced heating decreases the conductivity of the star thus leading to the accelerated ohmic decay (Konar & Bhattacharya 1997;Geppert & Urpin 1994;Urpin & Konenkov 1997); (ii) vortex-fluxoid interactions in the superconducting core (Muslimov & Tsygan 1985;Srinivasan et al 1990); and (iii) magnetic screening or burial (Bisnovatyi-Kogan & Komberg 1974;Cheng & Zhang 1998;Konar & Bhattacharya 1997;Payne & Melatos 2004;Wang et al 2012). A well known problem with the field burial scenario is that the buried magnetic field will be prone to instabilities that rapidly will overturn the field (Litwin et al 2001;Vigelius & Melatos 2008;Mukherjee & Bhattacharya 2012).…”

Section: A Relation Between Space Velocity and Field Growth Timescalementioning

confidence: 99%

Relating the kick velocities of young pulsars with magnetic field growth time-scales inferred from braking indices

Güneydaş

Ekşi

2013

Monthly Notices of the Royal Astronomical Society: Letters

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A nascent neutron star may be exposed to fallback accretion soon after the proto-neutron star stage. This high accretion episode can submerge the magnetic field deep in the crust. The diffusion of the magnetic field back to the surface will take hundreds to millions of years depending on the amount of mass accreted and the consequent depth the field is buried. Neutron stars with large kick velocities will accrete less amount of fallback material leading to shallower submergence of their fields and shorter time-scales for the growth of their fields. We obtain the relation τ Ohm ∝ v −1 between the space velocity of the neutron star and Ohmic time-scale for the growth of the magnetic field. We compare this with the relation between the measured transverse velocities, v ⊥ and the field growth time-scales, µ/μ, inferred from the measured braking indices. We find that the observational data is consistent with the theoretical prediction though the small number of data precludes a strong conclusion. Measurement of the transverse velocities of pulsars B1509−58, J1846−0258, J1119−6127 and J1734−3333 would increase the number of the data and strongly contribute to understanding whether pulsar fields grow following fallback accretion.

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Section: A Relation Between Space Velocity and Field Growth Timescalementioning

confidence: 99%

Relating the kick velocities of young pulsars with magnetic field growth time-scales inferred from braking indices

Güneydaş

Ekşi

2013

Monthly Notices of the Royal Astronomical Society: Letters

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“…Several theoretical mechanisms exist to explain the trend, such as accelerated Ohmic decay (Urpin & Geppert 1995), interactions between superfluid vortices and superconductor flux tubes within the stellar interior (Srinivasan et al 1990), or the process of magnetic burial (Blondin & Freese 1986;Shibazaki et al 1989). In magnetic burial, the focus of this paper, matter is guided onto the polar cap by the magnetic field to form a mountain-like density profile supported by the compressed equatorial magnetic field ('magnetic mountain') Melatos & Phinney 2001;Payne & Melatos 2004;Mukherjee & Bhattacharya 2012;Wang et al 2012). The resulting mass quadrupole moment emits gravitational E-mail:suvorovarthur@gmail.com radiation (Ushomirsky et al 2000;Melatos & Payne 2005;Vigelius & Melatos 2009c;Priymak et al 2011;Lasky 2015).…”

Section: Introductionmentioning

confidence: 97%

Relaxation by thermal conduction of a magnetically confined mountain on an accreting neutron star

Suvorov

Melatos

2018

Monthly Notices of the Royal Astronomical Society

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A magnetically confined mountain on the surface of an accreting neutron star simultaneously reduces the global magnetic dipole moment through magnetic burial and generates a mass quadrupole moment, which emits gravitational radiation. Previous mountain models have been calculated for idealized isothermal and adiabatic equations of state. Here these models are generalised to include non-zero, finite thermal conduction. Grad-Shafranov equilibria for three representative, polytropic equations of state are evolved over many conduction time-scales with the magnetohydrodynamic solver PLUTO. It is shown that conduction facilitates the flow of matter towards the pole. Consequently the buried magnetic field is partially resurrected starting from an initially polytropic Grad-Shafranov equilibrium. The poleward mass current makes the star more prolate, marginally increasing its detectability as a gravitational wave source, though to an extent which is likely to be subordinate to other mountain physics. Thermal currents also generate filamentary hot spots ( 10 8 K) in the mountain, especially near the pole where the heat flux is largest, with implications for type I X-ray bursts.

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“…The minimum spin period and bottom field are independent of the initial values of magnetic field and spin period; see Figure 3 [72]. The bottom fields mildly vary with the accretion rates and the accreted mass (Figure 4), while the minimum period is insensitive to them ( Figure 5) [72,73].…”

Section: Accretion-induced Field Decay and Spin-upmentioning

confidence: 95%

Physical Environment of Accreting Neutron Stars

Wang

2016

Advances in Astronomy

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Neutron stars (NSs) powered by accretion, which are known as accretion-powered NSs, always are located in binary systems and manifest themselves as X-ray sources. Physical processes taking place during the accretion of material from their companions form a challenging and appealing topic, because of the strong magnetic field of NSs. In this paper, we review the physical process of accretion onto magnetized NS in X-ray binary systems. We, firstly, give an introduction to accretion-powered NSs and review the accretion mechanism in X-ray binaries. This review is mostly focused on accretion-induced evolution of NSs, which includes scenario of NSs both in high-mass binaries and in low-mass systems.

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Testing the accretion-induced field-decay and spin-up model for recycled pulsars

Cited by 3 publications

References 44 publications

Relating the kick velocities of young pulsars with magnetic field growth time-scales inferred from braking indices

Relating the kick velocities of young pulsars with magnetic field growth time-scales inferred from braking indices

Relaxation by thermal conduction of a magnetically confined mountain on an accreting neutron star

Physical Environment of Accreting Neutron Stars

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