Probing clumpy stellar winds with a neutron-star

TL;DR

This paper investigates the variability of super-giant high-mass X-ray binaries caused by clumpy stellar winds, using X-ray observations to constrain wind properties and improve understanding of stellar mass loss.

Contribution

It provides quantitative constraints on wind clumping in massive stars through analysis of X-ray flares in SFXT systems, supporting macro-clumping models.

Findings

X-ray flares have a typical duration of 3 ks and occur every 7 days.

Clump densities are 10^22-23 g, with a density ratio of 100-10,000 compared to inter-clump medium.

Results align with macro-clumping scenarios and line-driven instability simulations.

Abstract

INTEGRAL tripled the number of super-giant high-mass X-ray binaries (sgHMXB) known in the Galaxy by revealing absorbed and fast transient (SFXT) systems. Quantitative constraints on the wind clumping of massive stars can be obtained from the study of the hard X-ray variability of SFXT. A large fraction of the hard X-ray emission is emitted in the form of flares with a typical duration of 3 ksec, frequency of 7 days and luminosity of 1E36 ergs/s. Such flares are most probably emitted by the interaction of a compact object orbiting at ~ 10 R* with wind clumps (1E(22-23) g) representing a large fraction of the stellar mass-loss rate. The density ratio between the clumps and the inter-clump medium is 1E(2-4) . The parameters of the clumps and of the inter-clump medium, derived from the SFXT flaring behavior, are in good agreement with macro-clumping scenario and line-driven instability simulations. SFXT are likely to have larger orbital radius than classical sgHMXB.