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Implications of the measured parameters of PSR J1903+0327 for its progenitor neutron star
Solar and Stellar Astrophysics · Submitted 13 Jun 2011
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We conclude that the influence of magnetic field in the "recycling" process is crucial - it leads to a significant decrease of spin-up rate and larger accreted masses, in comparison to the B=0 model.
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The abstract, sentence by sentence
Using the intrinsic PSR J1903+0327 parameters evaluated from radio observations (mass, rotation period and dipole magnetic field deduced from the timing properties) we calculate the mass of its neutron star progenitor, M_i, at the onset of accretion. Simultaneously, we derive constraints on average accretion rate Mdot and the pre-accretion magnetic field B_i. Spin-up is modelled by accretion from a thin disk, using the magnetic-torque disk-pulsar coupling model proposed by Kluzniak and Rappaport (2007), improved for the existence of relativistic marginally-stable circular orbit. Orbital parameters in the disk are obtained using the space-time generated by a rotating neutron star in the framework of General Relativity. We employ an observationally motivated model of the surface magnetic field decay. We also seek for the imprint of the poorly known equation of state of dense matter on the spin-up tracks - three equations of state of dense matter, consistent with the existence of 2 Msun neutron star, are considered. We find that the minimum average accretion rate should be larger than 2-8 10^(-10) Msun/yr, the highest lower bound corresponding to the stiffest equation of state. We conclude that the influence of magnetic field in the "recycling" process is crucial - it leads to a significant decrease of spin-up rate and larger accreted masses, in comparison to the B=0 model. Allowed B_i-dependent values of M_i are within 1.0-1.4 Msun, i.e., much lower than an oversimplified but widely used B=0 result, where one gets M_i>1.55 Msun. Estimated initial neutron-star mass depends on the assumed dense-matter equation of state.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Using the intrinsic PSR J1903+0327 parameters evaluated from radio observations (mass, rotation period and dipole magnetic field deduced from the timing properties) we calculate the mass of its neutron star progenitor, M_i, at the onset of accretion. | contribution 0.62 | 0.85 | 0.03 | asserted 0.98 |
| s1 | Simultaneously, we derive constraints on average accretion rate Mdot and the pre-accretion magnetic field B_i. | contribution 0.77 | 0.96 | 0.03 | asserted 0.99 |
| s2 | Spin-up is modelled by accretion from a thin disk, using the magnetic-torque disk-pulsar coupling model proposed by Kluzniak and Rappaport (2007), improved for the existence of relativistic marginally-stable circular orbit. | method 1.00 | 0.49 | 0.03 | asserted 0.98 |
| s3 | Orbital parameters in the disk are obtained using the space-time generated by a rotating neutron star in the framework of General Relativity. | method 1.00 | 0.60 | 0.02 | asserted 0.98 |
| s4 | We employ an observationally motivated model of the surface magnetic field decay. | method 0.99 | 0.69 | 0.02 | asserted 0.95 |
| s5 | We also seek for the imprint of the poorly known equation of state of dense matter on the spin-up tracks - three equations of state of dense matter, consistent with the existence of 2 Msun neutron star, are considered. | method 0.79 | 0.87 | 0.03 | hedged possibility 0.42 |
| s6 | We find that the minimum average accretion rate should be larger than 2-8 10^(-10) Msun/yr, the highest lower bound corresponding to the stiffest equation of state. | result 1.00 | 0.96 | 0.11 | asserted 1.00 |
| s7 | We conclude that the influence of magnetic field in the "recycling" process is crucial - it leads to a significant decrease of spin-up rate and larger accreted masses, in comparison to the B=0 model. | interpretation 0.90 | 0.89 | 0.70 | asserted 1.00 |
| s8 | Allowed B_i-dependent values of M_i are within 1.0-1.4 Msun, i.e., much lower than an oversimplified but widely used B=0 result, where one gets M_i>1.55 Msun. | result 0.99 | 0.91 | 0.30 | asserted 1.00 |
| s9 | Estimated initial neutron-star mass depends on the assumed dense-matter equation of state. | result 0.90 | 0.85 | 0.11 | asserted 0.99 |
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Original abstract
Using the intrinsic PSR J1903+0327 parameters evaluated from radio observations (mass, rotation period and dipole magnetic field deduced from the timing properties) we calculate the mass of its neutron star progenitor, M_i, at the onset of accretion. Simultaneously, we derive constraints on average accretion rate Mdot and the pre-accretion magnetic field B_i. Spin-up is modelled by accretion from a thin disk, using the magnetic-torque disk-pulsar coupling model proposed by Kluzniak and Rappaport (2007), improved for the existence of relativistic marginally-stable circular orbit. Orbital parameters in the disk are obtained using the space-time generated by a rotating neutron star in the framework of General Relativity. We employ an observationally motivated model of the surface magnetic field decay. We also seek for the imprint of the poorly known equation of state of dense matter on the spin-up tracks - three equations of state of dense matter, consistent with the existence of 2 Msun neutron star, are considered. We find that the minimum average accretion rate should be larger than 2-8 10^(-10) Msun/yr, the highest lower bound corresponding to the stiffest equation of state. We conclude that the influence of magnetic field in the "recycling" process is crucial - it leads to a significant decrease of spin-up rate and larger accreted masses, in comparison to the B=0 model. Allowed B_i-dependent values of M_i are within 1.0-1.4 Msun, i.e., much lower than an oversimplified but widely used B=0 result, where one gets M_i>1.55 Msun. Estimated initial neutron-star mass depends on the assumed dense-matter equation of state.
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References
How the literature uses it
2 arXiv papers cite this in 8 sentences
Papers citing it · 4 sentences without a confident label
Uses its method or tool 1 paper
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Function $f_ms$ introduced by [ref] ( [ref] ; reducing to $f_ms≡1$ in the Eq. 17 of [ref] ) ensures a proper behavior of the torque near $r_ms$ [equation] with $α=Jc/(√(2)GM^2)$, $r̅=r_0/r_s$ and $r_s = 2GM/c^2$ denoting the Schwarzschild radius.
Compression of matter in the center of accreting neutron stars · Calculation of the inner-boundary radius of the accretion disk · 0.91
Cites it as background 1 paper
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The details of magnetic-field decay during the accretion-driven evolution phase of an NS' life are still far from being understood in spite of theoretical and observational efforts in recent years (see Sect. 4 of [ref] for a brief summary).
Compression of matter in the center of accreting neutron stars · Introduction · 0.87
What it cites · 7 sentences without a confident label
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This scenario was proposed by [ref] and [ref] .
The formation of the eccentric-orbit millisecond pulsar J1903+0327 and the origin of single millisecond pulsars · IV. Pulsar in a triple (tertiary) system with two MS stars of different masses, the pulsar being spun-up by accretion fr · 0.92
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