Quantifying irradiation in spider pulsars: the extreme case of PSR J1622−0315

Abstract

ABSTRACT We present the first multiband optical light curves of PSR J1622−0315, among the most compact known redback binary millisecond pulsars, with an orbital period $P_\mathrm{orb}=3.9 \, \text{h}$. We find a flux modulation with two maxima per orbital cycle and a peak-to-peak amplitude ${\simeq} 0.3 \, \text{mag}$, which we attribute to the ellipsoidal shape of the tidally distorted companion star. The optical colours imply a late-F to early-G spectral-type companion and do not show any detectable temperature changes along the orbit. This suggests that the irradiation of the star’s inner face by the pulsar wind is unexpectedly missing despite its short orbital period. To interpret these results, we introduce a new parameter fsd, defined as the ratio between the pulsar wind flux intercepted by the companion star and the companion intrinsic flux. This flux ratio fsd, which depends on the spin-down luminosity of the pulsar, the base temperature of the companion and the orbital period, can be used to quantify the effect of the pulsar wind on the companion star and turns out to be the most important factor in determining whether the companion is irradiated or not. We find that the transition between these two regimes occurs at fsd ≃ 2–4 and that the value for PSR J1622−0315 is fsd = 0.7, placing it firmly in the non-irradiated regime.