2025/01/27 by М. Д. Афонина, Marina Afonina, Afonina, Marina +3 · 1 voice · 1 citation
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #Geophysics and Sensor Technology #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.2501.15918
openalex publication_date 2025/01/27 · arxiv published 2025/01/27 · arxiv updated 2025/01/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Precise astrometric measurement with Gaia satellite resulted in the discovery of tens of wide binary systems consisting of a Sun-like star and an invisible component. The latter can be a white dwarf, a neutron star, or a black hole. In this paper, we model magneto-rotational evolution of neutron stars in wide low-mass binaries accounting for the orbital eccentricity. We aim to calculate when neutron stars in such systems can start to accrete matter from the stellar wind of the companion. We show that the transition from the ejector to the propeller stage occurs earlier in more eccentric systems, thus increasing the time that neutron stars can spend accreting matter. Our calculations show that in the case of efficient spin-down at the propeller stage, a neutron star in an eccentric orbit with e\gtrsim0.6 and a standard magnetic field B=1012 G can start accreting within a few Gyr. For neutron stars with B=1013 G the onset of accretion occurs earlier regardless of the orbital eccentricity. Otherwise, with a lower spin-down rate, such a neutron star will remain at the propeller stage for most of its life.