Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI

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Título: Orbital phase-resolved spectroscopy of 4U 1538−52 with MAXI
Autor/es: Rodes Roca, José Joaquín | Mihara, T. | Nakahira, S. | Torrejon, Jose M. | Giménez García, Ángel | Bernabeu, Guillermo
Grupo/s de investigación o GITE: Astronomía y Astrofísica
Centro, Departamento o Servicio: Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal
Palabras clave: X-rays: binaries | Pulsars: individual: 4U 1538-52 | Stars: mass-loss
Área/s de conocimiento: Física Aplicada
Fecha de publicación: 21-ago-2015
Editor: EDP Sciences
Cita bibliográfica: Astronomy & Astrophysics. 2015, 580: A140. doi:10.1051/0004-6361/201425323
Resumen: Context. 4U 1538−52, an absorbed high mass X-ray binary with an orbital period of ~3.73 days, shows moderate orbital intensity modulations with a low level of counts during the eclipse. Several models have been proposed to explain the accretion at different orbital phases by a spherically symmetric stellar wind from the companion. Aims. The aim of this work is to study both the light curve and orbital phase spectroscopy of this source in the long term. In particular, we study the folded light curve and the changes in the spectral parameters with orbital phase to analyse the stellar wind of QV Nor, the mass donor of this binary system. Methods. We used all the observations made from the Gas Slit Camera on board MAXI of 4U 1538−52 covering many orbits continuously. We obtained the good interval times for all orbital phase ranges, which were the input for extracting our data. We estimated the orbital period of the system and then folded the light curves, and we fitted the X-ray spectra with the same model for every orbital phase spectrum. We also extracted the averaged spectrum of all the MAXI data available. Results. The MAXI spectra in the 2–20 keV energy range were fitted with an absorbed Comptonisation of cool photons on hot electrons. We found a strong orbital dependence of the absorption column density but neither the fluorescence iron emission line nor low energy excess were needed to fit the MAXI spectra. The variation in the spectral parameters over the binary orbit were used to examine the mode of accretion onto the neutron star in 4U 1538−52. We deduce a best value of Ṁ/v∞ = 0.65 × 10-9M⊙ yr-1/ (km s-1) for QV Nor.
Patrocinador/es: Part of this work was supported by the Spanish Ministry of Economy and Competitiveness project numbers ESP2013-48637-C2-2P, and ESP2014-53672-C3-3-P, by the Vicerectorat d’Investigació, Desenvolupament i Innovació de la Universitat d’Alacant project number GRE12-35, and by the Generalitat Valenciana project number GV2014/088. This research made use of MAXI data provided by RIKEN, JAXA, and the MAXI team. J.J.R.R. acknowledges the support by the Matsumae International Foundation Research Fellowship No14G04, and also thanks the entire MAXI team for the collaboration and hospitality in RIKEN. The work of A.G.G. has been supported by the Spanish MICINN under FPI Fellowship BES-2011-050874 associated to the project AYA2010-15431. T.M. acknowledges the grant by the Vicerectorat d’Investigació, Desenvolupament i Innovació de la Universitat d’Alacant under visiting researcher programme INV14-11.
URI: http://hdl.handle.net/10045/49045
ISSN: 0004-6361 (Print) | 1432-0746 (Online)
DOI: 10.1051/0004-6361/201425323
Idioma: eng
Tipo: info:eu-repo/semantics/article
Derechos: © ESO 2015
Revisión científica: si
Versión del editor: http://dx.doi.org/10.1051/0004-6361/201425323
Aparece en las colecciones:INV - Astronomía y Astrofísica - Artículos de Revistas

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