The XMM-Newton View of GRS1915 105Report as inadecuate

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1 OAS - Observatoire astronomique de Strasbourg 2 CESR - Centre d-étude spatiale des rayonnements 3 Dipartimento di Fisica 4 Osservatorio Astronomico di Brera 5 IASF, Area di Ricerca di Tor Vergata 6 Astronomical Institute 7 Institute of Astronomy

Abstract : abridged Two XMM-Newton observations of the black-hole binary GRS1915+105 were triggered in 2004, during a long -plateau- state of the source.

. While the light curves show just small amplitude variations a few percent at timescales longer than a few seconds, a QPO is seen at about 0.6 Hz

The pn spectrum is well fitted without invoking thermal disk emission, on the base of four main components: a primary one

., absorbed by cold matter with abundances different than those of standard ISM; reprocessing from an ionized disk; emission and absorption lines; and a soft X-ray excess around 1 keV. However, the latter is not confirmed by the RGS spectra, whose difference from the EPIC-pn ones actually lacks of a fully satisfactory explanation. If real, the soft X-ray excess may be due to reflection from an optically thin, photoionized disk wind; in this case it may yield a way to disentangle intrinsic from interstellar absorption.

Keywords : Black hole physics Line: formation Accretion accretion disks X-rays: binaries X-rays: individuals: GRS1915+105

Author: Andrea Martocchia - Giorgio Matt - Tomaso Belloni - Marco Feroci - Vladimir Karas - Gabriele Ponti -



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