Swift monitoring of IGR J16418-4532
P. Esposito (1), P. Romano (2), V. Mangano (2), L. Ducci (3), S., Vercellone (2) ((1) INAF-IASF Milano, (2) INAF-IASF Palermo, (3) Uni., Tuebingen)
TL;DR
This study presents detailed Swift X-ray observations of the supergiant fast X-ray transient IGR J16418-4532, revealing how its emission can be explained by accretion from a clumpy stellar wind over multiple orbits.
Contribution
It provides the most complete orbital sampling of IGR J16418-4532's X-ray light curve and models the emission through accretion of a structured stellar wind.
Findings
X-ray emission consistent with accretion from a clumpy wind
Clump masses range from ~5x10^16 g to 10^21 g
Most intense and complete orbital sampling to date
Abstract
We report on the Swift observations of the candidate supergiant fast X-ray transient (SFXT) IGR J16418-4532, which has an orbital period of ~3.7 d. Our monitoring, for a total of ~43 ks, spans over three orbits and represents the most intense and complete sampling along the orbital period of the light curve of this source. If one assumes a circular orbit, the X-ray emission from this source can be explained by accretion from a spherically symmetric clumpy wind from a blue supergiant, composed of clumps with different masses, ranging from ~5x10^16 g to 10^21g.
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