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LMXB and IMXB Evolution: I. The Binary Radio Pulsar PSR J1614-2230

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Jinrong Lin, S. Rappaport, Ph. Podsiadlowski, L. Nelson, B. Paxton, P. Todorov

High Energy Astrophysical Phenomena · Submitted 8 Dec 2010

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

The authors' main claim We show that (i) this system is a cousin to the LMXB Cyg X-2; (ii) for neutron stars of canonical birth mass 1.4 solar masses, the initial donor stars which produce the closest relatives to PSR J1614-2230 have a mass between 3.4-3.8 solar masses; (iii) neutron stars as massive as 1.97 solar masses are not easy to produce in spite of the initially high mass of the donor star, unless they were already born as relatively massive neutron stars; (iv) to successfully produce a system like PSR J1614-2230 requires a minimum initial neutron star mass of at least 1.6+-0.1 solar masses, as well as initial donor masses and orbital period of ~ 4.25+-0.10 solar masses and ~49+-2 hrs, respectively; and (v) the current companion star is largely composed of CO, but should have a surface H abundance of ~10-15%.

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arXiv ID1012.1877 (version 2)
Pith IDWK5H343Q, Pith's permanent record of this paper and its review
CitationB. Paxton, Jinrong Lin, L. Nelson, Ph. Podsiadlowski, P. Todorov, S. Rappaport. "LMXB and IMXB Evolution: I. The Binary Radio Pulsar PSR J1614-2230." arXiv:1012.1877 (2010). https://pith.science/paper/WK5H343Q
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The compiled record

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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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,170 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.21 · states limitation 0.58 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.18 · mentions code or data availability 0.04.

The abstract, sentence by sentence

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

We have computed an extensive grid of binary evolution tracks to represent low- and intermediate mass X-ray binaries (LMXBs and IMXBs). The grid includes 42,000 models which covers 60 initial donor masses over the range of 1-4 solar masses and, for each of these, 700 initial orbital periods over the range of 10-250 hours. These results can be applied to understanding LMXBs and IMXBs: those that evolve analogously to CVs; that form ultracompact binaries with orbital periods in the range of 6-50 minutes; and that lead to wide orbits with giant donors. We also investigate the relic binary recycled radio pulsars into which these systems evolve. To evolve the donor stars in this study, we utilized a newly developed stellar evolution code called "MESA" that was designed, among other things, to be able to handle very low-mass and degenerate donors. This first application of the results is aimed at an understanding of the newly discovered pulsar PSR J1614-2230 which has a 1.97 solar masses neutron star, orbital period = 8.7 days, and a companion star of 0.5 solar mass. We show that (i) this system is a cousin to the LMXB Cyg X-2; (ii) for neutron stars of canonical birth mass 1.4 solar masses, the initial donor stars which produce the closest relatives to PSR J1614-2230 have a mass between 3.4-3.8 solar masses; (iii) neutron stars as massive as 1.97 solar masses are not easy to produce in spite of the initially high mass of the donor star, unless they were already born as relatively massive neutron stars; (iv) to successfully produce a system like PSR J1614-2230 requires a minimum initial neutron star mass of at least 1.6+-0.1 solar masses, as well as initial donor masses and orbital period of ~ 4.25+-0.10 solar masses and ~49+-2 hrs, respectively; and (v) the current companion star is largely composed of CO, but should have a surface H abundance of ~10-15%.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We have computed an extensive grid of binary evolution tracks to represent low- and intermediate mass X-ray binaries (LMXBs and IMXBs). contribution 0.71 0.96 0.04 asserted 1.00
s1 The grid includes 42,000 models which covers 60 initial donor masses over the range of 1-4 solar masses and, for each of these, 700 initial orbital periods over the range of 10-250 hours. method 0.80 0.94 0.03 asserted 1.00
s2 These results can be applied to understanding LMXBs and IMXBs: those that evolve analogously to CVs; that form ultracompact binaries with orbital periods in the range of 6-50 minutes; and that lead to wide orbits with giant donors. interpretation 0.93 0.65 0.09 asserted 0.50
s3 We also investigate the relic binary recycled radio pulsars into which these systems evolve. contribution 0.98 0.83 0.04 asserted 0.69
s4 To evolve the donor stars in this study, we utilized a newly developed stellar evolution code called "MESA" that was designed, among other things, to be able to handle very low-mass and degenerate donors. method 1.00 0.67 0.02 asserted 1.00
s5 This first application of the results is aimed at an understanding of the newly discovered pulsar PSR J1614-2230 which has a 1.97 solar masses neutron star, orbital period = 8.7 days, and a companion star of 0.5 solar mass. contribution 0.68 0.32 0.08 asserted 0.85
s6 We show that (i) this system is a cousin to the LMXB Cyg X-2; (ii) for neutron stars of canonical birth mass 1.4 solar masses, the initial donor stars which produce the closest relatives to PSR J1614-2230 have a mass between 3.4-3.8 solar masses; (iii) neutron stars as massive as 1.97 solar masses are not easy to produce in spite of the initially high mass of the donor star, unless they were already born as relatively massive neutron stars; (iv) to successfully produce a system like PSR J1614-2230 requires a minimum initial neutron star mass of at least 1.6+-0.1 solar masses, as well as initial donor masses and orbital period of ~ 4.25+-0.10 solar masses and ~49+-2 hrs, respectively; and (v) the current companion star is largely composed of CO, but should have a surface H abundance of ~10-15%. result 0.94 0.94 0.67 asserted 1.00

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

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not examined
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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

We have computed an extensive grid of binary evolution tracks to represent low- and intermediate mass X-ray binaries (LMXBs and IMXBs). The grid includes 42,000 models which covers 60 initial donor masses over the range of 1-4 solar masses and, for each of these, 700 initial orbital periods over the range of 10-250 hours. These results can be applied to understanding LMXBs and IMXBs: those that evolve analogously to CVs; that form ultracompact binaries with orbital periods in the range of 6-50 minutes; and that lead to wide orbits with giant donors. We also investigate the relic binary recycled radio pulsars into which these systems evolve. To evolve the donor stars in this study, we utilized a newly developed stellar evolution code called "MESA" that was designed, among other things, to be able to handle very low-mass and degenerate donors. This first application of the results is aimed at an understanding of the newly discovered pulsar PSR J1614-2230 which has a 1.97 solar masses neutron star, orbital period = 8.7 days, and a companion star of 0.5 solar mass. We show that (i) this system is a cousin to the LMXB Cyg X-2; (ii) for neutron stars of canonical birth mass 1.4 solar masses, the initial donor stars which produce the closest relatives to PSR J1614-2230 have a mass between 3.4-3.8 solar masses; (iii) neutron stars as massive as 1.97 solar masses are not easy to produce in spite of the initially high mass of the donor star, unless they were already born as relatively massive neutron stars; (iv) to successfully produce a system like PSR J1614-2230 requires a minimum initial neutron star mass of at least 1.6+-0.1 solar masses, as well as initial donor masses and orbital period of ~ 4.25+-0.10 solar masses and ~49+-2 hrs, respectively; and (v) the current companion star is largely composed of CO, but should have a surface H abundance of ~10-15%.

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