2009/04/17 by R. C. Reis, A. C. Fabian, A. J. Young
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Emission spectrum #Line (geometry) #Neutron star #RADIUS #Spectral line #astro-ph.HE
paper · pdf · doi:10.1111/j.1745-3933.2009.00675.x
Accepted for publication in MNRAS, 5 pages, 3 figures
arxiv created 2009/04/17 · openalex publication_date 2009/08/28 · arxiv updated 2015/05/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract The X-ray spectra of accreting compact objects often exhibit discrete emission features associated with fluorescent emission in the accretion disc, the strongest of which is the Fe Kα fluorescence line at 6.4–6.97keV. These reflection features are amongst the best tools in the study of the inner region of accretion flow around a compact object. Here, we report on three Suzaku observations of the neutron star X-ray binary 4U 1705−44 where a broad, skewed Fe Kα emission line is clearly visible above the continuum. By using a relativistically blurred reflection model, we find that in 4U 1705−44 the inner disc radius extends down to rin= 10.5+1.0−1.7GM/c2 and is at an angle of 29.8+1.1−1.0 deg to the line of sight. Furthermore, we find that the level of ionization in the surface layers of the accretion disc changes by two orders of magnitude between the three observations, however the inner radius obtained from the line profile remains stable.