2019MNRAS.490..752T

Intermediate-mass binary pulsars (IMBPs) are composed of neutron stars (NSs) and CO/ONe white dwarfs (WDs). It is generally suggested that IMBPs evolve from intermediate-mass X-ray binaries (IMXBs). However, this scenario is difficult to explain the formation of IMBPs with orbital periods (P_orb) less than 3 d. It has recently been proposed that a system consisting of an NS and a helium (He) star can form IMBPs with P_orb less than 3 d (known as the NS+He star scenario), but previous works can only cover a few observed sources with short orbital periods. We aim to investigate the NS+He star scenario by adopting different descriptions of the Eddington accretion rate ({dot}M_ Edd_) for NSs and different NS masses (M_NS) varying from 1.10 to 1.80 M_☉. Our results can cover most of the observed IMBPs with short orbital periods and almost half of the observed IMBPs with long orbital periods. We found that {dot}M_ Edd_ ∝ M_NS^–1/3 could match the observations better than a specific value for all NSs. We also found that the final spin periods of NSs slightly decrease with the initial M_NS. The observed parameters of PSR J0621+1002, which is one of the well-observed IMBPs whose pulsar mass has been precisely measured, can be reproduced by this work.