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      The complications of learning from Super Soft Source X-ray spectra

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          Abstract

          Super Soft X-ray Sources (SSS) are powered by nuclear burning on the surface of an accreting white dwarf, they are seen around 0.1-1 keV (thus in the soft X-ray regime), depending on effective temperature and the amount of intervening interstellar neutral hydrogen N_H. The most realistic model to derive physical parameters from observed SSS spectra would be an atmosphere model that simulates the radiation transport processes. However, observed SSS high-resolution grating spectra reveal highly complex details that cast doubts on the feasibility of achieving unique results from atmosphere modeling. In this article, I discuss two independent atmosphere model analyses of the same data set, leading to different results. I then show some of the details that complicate the analysis and conclude that we need to approach the interpretation of high-resolution SSS spectra differently. We need to focus more on the data than the models and to use more phenomenological approaches as is traditionally done with optical spectra.

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          Most cited references 17

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          The retrograde orbit of the HAT-P-6b exoplanet

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            LUMINOUS SUPERSOFT X-RAY SOURCES

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              ROSAT X-Ray Observations of Nova V1974 Cygni: The Rise and Fall of the Brightest Supersoft X-Ray Source

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                Author and article information

                Journal
                20 September 2019
                Article
                10.1016/j.asr.2019.09.002
                1909.09711

                http://arxiv.org/licenses/nonexclusive-distrib/1.0/

                Custom metadata
                Accepted in JASR. 7 pages, 6 figure. arXiv admin note: ... => ... astro-ph.SR
                astro-ph.HE

                High energy astrophysical phenomena

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