The maximum accreted mass of recycled pulsars

Hai-Liang Chen; Xuefei Chen; Zhanwen Han; Zhenwei Li

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The maximum accreted mass of recycled pulsars

Zhenwei Li, Xuefei Chen, Hai-Liang Chen, Zhanwen Han

High Energy Astrophysical Phenomena · Submitted 5 Aug 2021

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Our results show that the NSs can accrete relatively more material for binary systems with the donor masses in the range of $1.8\sim 2.4M_\odot$, the NSs accrete relatively more mass when the remnant WD mass is in the range of $\sim 0.25-0.30M_\odot$, and the maximum accreted mass is positively correlated with the initial NS mass.

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What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.39 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.06 · mentions code or data availability 0.02.

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The maximum mass of neutron stars (NSs) is of great importance for constraining equations of state of NSs and understanding the mass gap between NSs and stellar-mass black holes. NSs in X-ray binaries would increase in mass by accreting material from their companions (known as recycling process), and the uncertainties in the accretion process give challenge to study the NS mass at birth. {In this work, we investigate the NS accreted mass with considering the effect of NS spin evolution and give the maximum accreted mass for NSs in the recycling process. By exploring a series of binary evolution calculations, we obtain the final NS mass and the maximum accreted mass for a given birth mass of NS and a mass transfer efficiency. Our results show that the NSs can accrete relatively more material for binary systems with the donor masses in the range of $1.8\sim 2.4M_\odot$, the NSs accrete relatively more mass when the remnant WD mass is in the range of $\sim 0.25-0.30M_\odot$, and the maximum accreted mass is positively correlated with the initial NS mass. For a $1.4M_\odot$ NS at birth with a moderate mass transfer efficiency of 0.3, the maximum accreted mass could be $0.27M_\odot$. The results can be used to estimate the minimum birth mass for systems with massive NSs in observations.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	The maximum mass of neutron stars (NSs) is of great importance for constraining equations of state of NSs and understanding the mass gap between NSs and stellar-mass black holes.	background 1.00	0.04	0.03	asserted 1.00
s1	NSs in X-ray binaries would increase in mass by accreting material from their companions (known as recycling process), and the uncertainties in the accretion process give challenge to study the NS mass at birth. {In this work, we investigate the NS accreted mass with considering the effect of NS spin evolution and give the maximum accreted mass for NSs in the recycling process.	contribution 0.86	0.73	0.13	asserted 0.97
s2	By exploring a series of binary evolution calculations, we obtain the final NS mass and the maximum accreted mass for a given birth mass of NS and a mass transfer efficiency.	method 0.97	0.96	0.07	asserted 1.00
s3	Our results show that the NSs can accrete relatively more material for binary systems with the donor masses in the range of $1.8\sim 2.4M_\odot$, the NSs accrete relatively more mass when the remnant WD mass is in the range of $\sim 0.25-0.30M_\odot$, and the maximum accreted mass is positively correlated with the initial NS mass.	result 1.00	0.95	0.62	asserted 1.00
s4	For a $1.4M_\odot$ NS at birth with a moderate mass transfer efficiency of 0.3, the maximum accreted mass could be $0.27M_\odot$.	result 1.00	0.93	0.17	hedged possibility 1.00
s5	The results can be used to estimate the minimum birth mass for systems with massive NSs in observations.	interpretation 0.92	0.48	0.09	asserted 0.61

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Original abstract

The maximum mass of neutron stars (NSs) is of great importance for constraining equations of state of NSs and understanding the mass gap between NSs and stellar-mass black holes. NSs in X-ray binaries would increase in mass by accreting material from their companions (known as recycling process), and the uncertainties in the accretion process give challenge to study the NS mass at birth. {In this work, we investigate the NS accreted mass with considering the effect of NS spin evolution and give the maximum accreted mass for NSs in the recycling process. By exploring a series of binary evolution calculations, we obtain the final NS mass and the maximum accreted mass for a given birth mass of NS and a mass transfer efficiency. Our results show that the NSs can accrete relatively more material for binary systems with the donor masses in the range of $1.8\sim 2.4M_\odot$, the NSs accrete relatively more mass when the remnant WD mass is in the range of $\sim 0.25-0.30M_\odot$, and the maximum accreted mass is positively correlated with the initial NS mass. For a $1.4M_\odot$ NS at birth with a moderate mass transfer efficiency of 0.3, the maximum accreted mass could be $0.27M_\odot$. The results can be used to estimate the minimum birth mass for systems with massive NSs in observations.

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Cited by 2 Pith papers

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Effect of quark-hadron phase transitions on the neutron star mass distribution
astro-ph.HE 2026-10 conditional novelty 7.0 of 10

Neutron stars formed through quark-hadron phase-transition explosions cluster around 1.55 to 1.70 solar masses, creating a single-star path to the observed high-mass peak.
Gaia neutron stars: demographics, birth rates, and connections to other neutron star populations
astro-ph.SR 2026-09 conditional novelty 6.0 of 10

Selection-corrected inference on the 27 Gaia neutron star candidates yields an intrinsic local density near 120 kpc^-3, a decreasing period distribution, and a forecast of 300 to 650 detections in Gaia DR4.

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1 arXiv paper cite this in 1 sentence

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

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Cites it as background 1 paper

A neutron star in a tight binary systems can accrete substantial amounts of matter from its companion star [ref] .

Electron and Muon Dynamics in Neutron Stars Beyond Chemical Equilibrium · Electrons and Muons in Neutron Stars. · 0.90

What it cites · 3 sentences without a confident label

Uses data or values from 1 paper

Recent pulsar radio timing and X-ray observations found several NSs with mass beyond $∼2M_⊙$, e.g. PSR J1600-3053 with a NS mass of $2.3^+0.17_-0.15M_⊙$ [ref] , PSR J2215+5135 with a NS mass of $2.28^+0.10_-0.09M_⊙$ [ref] , PSR J1959+2048 with a NS mass of $2.18±0.09M_⊙$ [ref] , PSR J0740+6620 (hereafter J0740) with a NS mass of $2.072^+0.067_-0.066M_⊙$ [ref] , and PSR J0348+0432 (hereafter J0348) with a NS mass of $2.01±0.04M_⊙$ [ref] .

A NICER View of the Massive Pulsar PSR J0740+6620 Informed by Radio Timing and XMM-Newton Spectroscopy · Introduction · 0.86

Compares with 1 paper

Due to the existences of Eddington limit and inefficient accretion, even if a high mass transfer efficiency is adopted, the value of average accretion efficiency is comparable with that in [ref] .

The millisecond pulsar mass distribution: Evidence for bimodality and constraints on the maximum neutron star mass · Binary evolution code · 0.92

Cites as background 1 paper

There are many uncertainties on the recycling phase, e.g. accretion efficiency (ratio of NS accreted mass to the transferred mass from donor), accretion disk instability, propeller effect [ref] , etc.

The millisecond pulsar mass distribution: Evidence for bimodality and constraints on the maximum neutron star mass · Introduction · 0.82

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