Hard X-ray flares in IGR J08408-4503 unveil clumpy stellar winds

TL;DR

This study analyzes a hard X-ray flare from IGR J08408-4503, revealing it as a supergiant fast X-ray transient system where stellar wind clumps cause X-ray flares, providing insights into massive star winds.

Contribution

The paper identifies IGR J08408-4503 as a supergiant fast X-ray transient and links its X-ray flares to wind clumps, advancing understanding of stellar wind structures.

Findings

IGR J08408-4503 is a supergiant fast X-ray transient.

X-ray flares are caused by wind clumps accreting onto a compact object.

Stellar wind clump mass loss rate is approximately 1E-6 solar masses per year.

Abstract

Context : A 1000-s flare from a new hard X-ray transient, IGR J08408-4503, was observed by INTEGRAL on May 15, 2006 during the real-time routine monitoring of IBIS/ISGRI images performed at the INTEGRAL Science Data Centre. The flare, detected during a single one-hour long pointing, peaked at 250 mCrab in the 20-40 keV energy range. Aims : Multi-wavelength observations, combining high-energy and optical data, were used to unveil the nature of IGR J08408-4503. Methods : A search in all INTEGRAL public data for other bursts from IGR J08408-4503 was performed, and the detailed analysis of another major flare is presented. The results of two Swift Target of Opportunity observations are also described. Finally, a study of the likely optical counterpart, HD 74194, is provided. Results : IGR J08408-4503 is very likely a supergiant fast X-ray transient (SFXT) system. The system parameters indicate that the X-ray flares are probably related to the accretion of wind clumps on a compact object orbiting about 1E13 cm from the supergiant HD 74194. The clump mass loss rate is of the order of 1E-6 solar mass/yr. Conclusions : Hard X-ray flares from SFXTs allow to probe the stellar winds of massive stars, and could possibly be associated with wind perturbations due to line-driven instabilities.