Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Debashis Sanyal; Norbert Langer (Bonn); Sung-Chul Yoon; Thomas M. Tauris

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Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Thomas M. Tauris, Debashis Sanyal, Sung-Chul Yoon, Norbert Langer (Bonn)

Solar and Stellar Astrophysics · Submitted 22 Aug 2013

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

The authors' main claim We demonstrate that the final properties of these MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel.

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arXiv ID1308.4887 (version 2)

Pith IDG7Q2X3QX, Pith's permanent record of this paper and its review

CitationDebashis Sanyal, Norbert Langer (Bonn), Sung-Chul Yoon, Thomas M. Tauris. "Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars." arXiv:1308.4887 (2013). https://pith.science/paper/G7Q2X3QX

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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.88 · states limitation 0.51 · human participants 0.01 · controlled comparison 0.68 · randomized assignment 0.01 · states quantitative result 0.59 · compares with prior results 0.91 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; show every role.

Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre- and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. We demonstrate that the final properties of these MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. Finally, we discuss the link between AIC and young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions. [Abridged]

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB).	background 1.00	0.03	0.02	asserted 0.55
s1	In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary.	background 1.00	0.04	0.03	asserted 0.96
s2	Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities.	contribution 0.97	0.55	0.06	unclear 0.64
s3	Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre- and post-AIC evolution of close binaries.	method 0.78	0.91	0.03	asserted 0.99
s4	We investigated the mass transfer onto a massive WD in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars.	method 0.85	0.96	0.02	asserted 0.99
s5	When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit.	method 0.95	0.84	0.03	asserted 0.69
s6	Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end.	method 0.96	0.95	0.03	asserted 0.92
s7	We demonstrate that the final properties of these MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel.	result 0.99	0.93	0.65	asserted 1.00
s8	However, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals.	result 1.00	0.93	0.17	asserted 0.88
s9	Finally, we discuss the link between AIC and young NSs in globular clusters.	contribution 0.44	0.45	0.04	unclear 0.78
s10	Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions. [Abridged]	interpretation 0.67	0.73	0.04	asserted 0.59

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre- and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. We demonstrate that the final properties of these MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. Finally, we discuss the link between AIC and young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions. [Abridged]

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References

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Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

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46 later papers cite it

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By the same authors

Regarding the kinematic effect of the AIC event, we follow the prescription of [ref] (see their section 3.2.1) to study the effects of sudden mass loss and natal kicks of BHs in post-AIC binary systems.

Does Nature allow formation of ultra-compact black hole X-ray binaries via accretion-induced collapse of neutron stars? (2023) (same authors) · Kinematic effects of the AIC event · 1.00

How the literature uses it

7 arXiv papers cite this in 11 sentences

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

Papers citing it · 5 sentences without a confident label

Cites it as background 6 papers

AIC can occur via two main channels: mass transfer from a companion star to a WD in a binary system [ref] or the binary WD merger [ref] .

Distinct neutrino signatures and onset condition of quark deconfinement in accretion-induced collapse of white dwarfs · Introduction · 0.80
An alternative channel for MSP formation is Accretion Induced Collapse (AIC), in which a white dwarf accretes enough material to exceed the Chandrasekhar mass limit of about $1.4$ and collapses to a neutron star [ref] .

The Galactic Millisecond Pulsar Population: Implications for the Galactic Center Excess · Millisecond Pulsars · 0.97
For instance, MSPs may be formed via the accretion induced collapse (AIC) of a massive (close to $M_Chandra$) O-Ne-Mg white dwarf accreting from a (typically low mass) companion in a tight binary [ref] .

Consistency Between the Luminosity Function of Resolved Millisecond Pulsars and the Galactic Center Excess · Introduction · 0.95

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