2019ApJ...887..201X

The neutron star (NS) low-mass X-ray binary 2A 1822-371 has an orbital period of 5.57 hr. Mass transfer in such short-period binaries is thought to be driven by magnetic braking with orbital shrinking. However, 2A 1822-371 shows a very rapid orbital expansion, implying that mass transfer occurs rapidly in this system. The accretion rate of the NS is observationally estimated to be higher than the Eddington limit, which is also hard to explain by the standard magnetic braking mechanism. In this work, we construct a model to account for the peculiar properties of 2A 1822-371. We assume that the donor star possesses a relatively strong magnetic field, which is coupled with the stellar winds excited by the X-ray radiation from the NS. This would generate efficient angular momentum loss, leading to a high mass transfer rate and hence orbital expansion. We provide possible evolutionary tracks of 2A 1822-371 and study how the input parameters affect the results. The observational implications of the irradiation-driven mass loss are also briefly discussed in the context of evolution of low-mass X-ray binaries and millisecond pulsars.