The accretion environment in Vela X-1 during a flaring period using XMM-Newton

Creators: Martínez-Núñez, S.; Torrejón, J. M.; Kühnel, M.; Kretschmar, P.; Stuhlinger, M.; Rodes-Roca, J. J.; Fürst, F.; Kreykenbohm, I.; Martin-Carillo, A.; Pollock, A. M. T.; Wilms, J.

Abstract

We present analysis of 100 ks contiguous XMM-Newton data of the prototypical wind accretor Vela X-1. The observation covered eclipse egress between orbital phases 0.134 and 0.265, during which a giant flare took place, enabling us to study the spectral properties both outside and during the flare. This giant flare with a peak luminosity of 3.92^(+0.42)_(-0.09) × 10^(37) erg s^(-1) allows estimates of the physical parameters of the accreted structure with a mass of ~10^(21) g. We have been able to model several contributions to the observed spectrum with a phenomenological model formed by three absorbed power laws plus three emission lines. After analysing the variations with orbital phase of the column density of each component, as well as those in the Fe and Ni fluorescence lines, we provide a physical interpretation for each spectral component. Meanwhile, the first two components are two aspects of the principal accretion component from the surface of the neutron star, the third component seems to be the X-ray light echo formed in the stellar wind of the companion.

Additional Information

© 2014 ESO. Received: 30 July 2013; Accepted: 26 December 2013. This work was supported by the Spanish Ministerio de Ciencia e Innovación through the projects AYA2010-15431 and AIB2010DE-00054. It was partly supported by the Bundesministerium für Wirtschaft und Technologie under Deutsches Zentrum für Luft- und Raumfahrt grant 50OR1113. This research was made possible in part by a travel grant from the Deutscher Akademischer Austauschdienst. JJRR acknowledges the support by the Vicerectorat d'Investigació, Desenvolupament i Innovació de la Universitat d'Alacant under grant GRE12-35. The authors acknowledge the help of the International Space Science Institute at Bern, Switzerland and support by the Faculty of the European Space Astronomy Centre. The SLXfig package, developed by John E. Davis, was used to produce some of the figures within in this paper. We thank the anonymous referee whose comments allowed us to improve this paper.

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