High-resolution X-ray spectroscopy of supergiant HMXB 4U 1700−37 during the compact object eclipse
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Título: | High-resolution X-ray spectroscopy of supergiant HMXB 4U 1700−37 during the compact object eclipse |
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Autor/es: | Martinez-Chicharro, Maria | Grinberg, Victoria | Torrejon, Jose M. | Schulz, Norbert S. | Oskinova, Lidia M. | Nowak, Michael A. | Fürst, Felix | Hell, Natalie | Hainich, Rainer |
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: | Stars: individual 4U 1700−37 | Stars: massive | X-rays: binaries |
Área/s de conocimiento: | Astronomía y Astrofísica |
Fecha de publicación: | mar-2021 |
Editor: | Oxford University Press |
Cita bibliográfica: | Monthly Notices of the Royal Astronomical Society. 2021, 501(4): 5646-5658. https://doi.org/10.1093/mnras/staa3956 |
Resumen: | We present an analysis of the first observation of the iconic high-mass X-ray binary 4U 1700−37 with the Chandra High-Energy Transmission Gratings (HETGs) during an X-ray eclipse. The goal of the observation was to study the structure/physical conditions in the clumpy stellar wind through high-resolution spectroscopy. We find the following: (a) Emission-line brightness from K-shell transitions, corresponding to near-neutral species, directly correlates with continuum illumination. However, these lines do not greatly diminish during eclipse. This is readily explained if fluorescence K α emission comes from the bulk of the wind. (b) The highly ionized Fe xxv and Fe xxvi Ly α diminish during eclipse. Thus, they must be produced in the vicinity of the compact object where log ξ > 3. (c) To describe the emission-line spectrum, the sum of two self-consistent photoionization models with low ionization (log ξ ∼ −1) and high ionization (log ξ ∼ 2.4) is required. From their emission measures, the clump-to-interclump density ratio can be estimated to be nc/ni ∼ 300. To fit the complex He-like Si xiii profile, the plasma requires a broadening with vbulk ∼ 840 km s−1. Reproducing the observed r ≈ f line fluxes requires the addition of a third collisionally ionized plasma. (d) Emission-line widths appear unresolved at the HETG resolution with the exception of silicon. There is no clear radial segregation between (quasi-)neutral and ionized species, consistent with cold wind clumps interspersed in a hot rarefied interclump medium. |
Patrocinador/es: | This research has been funded under the project ESP2017-85691-P. The research leading to these results has received funding from the European Union’s Horizon 2020 Programme under the Activities for the High-Energy Astrophysiscs Domain (AHEAD) project (grant agreement no. 654215). Victoria Grinberg (VG) was supported through the Margarete von Wrangell fellowship by the ESF and the Ministry of Science, Research and the Arts of Baden-Württemberg. Work at LLNL was performed under the auspices of the U.S. Department of Energy under contract no. DE-AC52-07NA27344 and supported through National Aeronautics and Space Administration (NASA) grants to Lawrence Livermore National Laboratory (LLNL). Lida M. Oskinova acknowledges Deutsches Zentrum für Luft und Raumfahrt (DLR) grant FKZ 50 OR 1508 and partial support by the Russian Government Program of Competitive Growth of Kazan Federal University. |
URI: | http://hdl.handle.net/10045/112398 |
ISSN: | 0035-8711 (Print) | 1365-2966 (Online) |
DOI: | 10.1093/mnras/staa3956 |
Idioma: | eng |
Tipo: | info:eu-repo/semantics/article |
Derechos: | © 2020 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society |
Revisión científica: | si |
Versión del editor: | https://doi.org/10.1093/mnras/staa3956 |
Aparece en las colecciones: | INV - Astronomía y Astrofísica - Artículos de Revistas Investigaciones financiadas por la UE |
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