On the Apparent Lack of Be X-ray Binaries with Black Holes

TL;DR

The paper explains the absence of observed Be X-ray binaries with black holes by evolutionary models predicting a high neutron star to black hole ratio, which aligns with the current observational data.

Contribution

It demonstrates that stellar evolution and binary formation processes naturally lead to a scarcity of Be black hole binaries, explaining their non-detection.

Findings

Expected number of Be black hole binaries is 0-2.

The neutron star to black hole ratio is predicted to be 10-50.

Current observations are consistent with evolutionary predictions.

Abstract

In the Galaxy there are 64 Be X-ray binaries known to-date. Out of those, 42 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. There seems to be no apparent mechanism that would prevent formation or detection of Be stars with black holes. This disparity is referred to as a missing Be -- black hole X-ray binary problem. We point out that current evolutionary scenarios that lead to the formation of Be X-ray binaries predict that the ratio of these binaries with neutron stars to the ones with black holes is rather high F_NStoBH=10-50, with the more likely formation models providing the values at the high end. The ratio is a natural outcome of (i) the stellar initial mass function that produces more neutron stars than black holes and (ii) common envelope evolution (i.e. a major mechanism involved in the formation of interacting binaries) that naturally selects progenitors of Be X-ray binaries with neutron stars (binaries with comparable mass components have more likely survival probabilities) over ones with black holes (which are much more likely to be common envelope mergers). A comparison of this ratio (i.e. F_NStoBH=30) with the number of confirmed Be -- neutron star X-ray binaries (42) indicates that the expected number of Be -- black hole X-ray binaries is of the order of only 0-2. This is entirely consistent with the observed Galactic sample.