2013/03/25 by Wen-Cong Chen, Wen‐Cong Chen, Wei-Min Liu · 13 citations
Physics and Astronomy · #Angular momentum #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Binary star #Classical mechanics #Compact star #Gamma-ray bursts and supernovae #Neutron star #Orbital period #Physics #Pulsar #Pulsars and Gravitational Waves Research #Star (game theory) #Stars #Stellar evolution #White dwarf #X-ray binary #X-ray pulsar #astro-ph.SR
paper · pdf · doi:10.1093/mnrasl/slt043
published in Monthly Notices of the Royal Astronomical Society Letters 432(1), L75-L79 (Oxford University Press) · 5 pages, 4 figures, accepted for publication in MNRAS letters
arxiv created 2013/03/25 · openalex publication_date 2013/04/20 · arxiv updated 2015/06/15 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract It is difficult for intermediate-mass X-ray binaries to form compact intermediate-mass binary pulsars (IMBPs) with a short orbital-period ( ≲ 3 d), which have heavy ( ≳ 0.4 M⊙) CO or ONeMg white dwarf (WD) companions. Since neutron star + He star binaries may experience common-envelope evolution, they have some advantage to account for the formation of short orbital-period IMBPs. In this work, we explore the probability of IMBPs formed by this evolutionary channel. Using Eggleton's stellar evolution code, considering that the dead pulsars were spun up by the accreting material and angular momentum from the He star companions, we have calculated the evolution of a large number of neutron star + He star binaries. Our simulated results indicate that the NS + He star evolutionary channel can produce IMBPs with a WD of ∼ 0.5-1.1 M⊙ and an orbital period of 0.03–20 d, in which pulsars have a spin period of 1.4–200 ms. Comparing the calculated results with the observational parameters (spin period and orbital period) of nine compact IMBPs, the NS + He star evolutionary channel can account for the formation of four sources. Therefore, NS + He star binaries offer an alternative evolutionary channel to compact IMBPs.