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- Volume 93 - Année 2024
- No 3 - 41st Liège International Astrophysical Coll...
- Probing the X-ray Reprocessing Geometry in High-Mass X-ray Binaries with the Chandra High Energy Transmission Grating
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Probing the X-ray Reprocessing Geometry in High-Mass X-ray Binaries with the Chandra High Energy Transmission Grating
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La majorité des étoiles résident dans des systèmes multiples, et la majorité des étoiles massives apparaissent dans des binaires. Un sous-ensemble important passe par une phase binaire à rayons X (BRX), mais la géométrie de leur matière retraitant les rayons X, qui génère ainsi des caractéristiques spectrales proéminentes, telles que les raies d’émission de fer fluorescent, reste mal comprise. La similitude des caractéristiques spectrales des BRX avec celles des noyaux galactiques actifs (NGA) dans les rayons X nous motive à appliquer une modélisation physique similaire pour 10 binaires X de grande masse (BXGM) dans la Galaxie, bien connues et observées avec le spectromètre à réseau de transmission à haute énergie (High Energy Transmission Grating) sur Chandra. En utilisant deux modèles de pointe différents pour le retraitement des rayons X, qui modélisent de manière cohérente l’émission fluorescente Fe Kα en même temps que les continus des rayons X diffusés, nous obtenons des informations uniques sur la géométrie et la cinématique de l’écoulement d’accrétion dans ces systèmes. Nous présentons ici les contraintes sur la forme ainsi que la distance entre le reprocesseur de rayons X et le disque d’accrétion.
Abstract
A majority of stars reside in multiple systems, and a majority of massive stars appear in binaries. An important subset goes through an X-ray binary (XRB) phase, but the geometry of their X-ray reprocessing matter that gives rise to prominent spectral features such iron fluorescent X-ray emission remains not well understood. The similarity of XRB spectral features to those of Active Galactic Nuclei (AGN) in the X-rays motivates us to apply similar physical modeling for 10 well-known Galactic High Mass X-ray Binaries (HMXBs) observed with the Chandra High Energy Transmission Grating (HETG). Using two different state-of-the art models for X-ray reprocessing, that self-consistently model together Fe Kα fluorescent emission and scattered X-ray continua, we obtain unique insights into the geometry and kinematics of the accretion flow in these systems. Here, we present constraints on the shape as well as distance of the X-ray reprocessor from the accretion disk.
This work is distributed under the Creative Commons CC BY 4.0 Licence.
Paper presented at the 41st Liège International Astrophysical Colloquium on “The eventful life of massive star multiples,” University of Liège (Belgium), 15–19 July 2024.
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Om dit artikel te citeren:
Over : Panayiotis Tzanavaris
Center for Research and Exploration in Space Science and Technology, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
The American Physical Society, Hauppauge, NY 11788, USA
email : ptzanava@umbc.edu
Over : Tahir Yaqoob
Center for Research and Exploration in Space Science and Technology, NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA