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- W4224256058 abstract "ABSTRACT In this paper, we use an RXTE library of spectral models from 10 black hole and 9 pulsar X-ray binaries, as well as model spectra available in the literature from 13 extra-galactic ultra-luminous X-ray sources (ULXs). We compute average bolometric corrections (BC = Lband/Lbol) for our sample as a function of different accretion rates. We notice the same behaviour between black hole and pulsar BCs only when ULX pulsars are included. These measurements provide a picture of the energetics of the accretion flow for an X-ray binary based solely on its observed luminosity in a given band. Moreover, it can be a powerful tool in X-ray binary population synthesis models. Furthermore, we calculate the X-ray (2–10 keV) to optical (V band) flux ratios originating from the disc/corona at different Eddington ratios for the black hole X-ray binaries in our sample. This provides a metric of the maximum contribution of the disc to the optical emission of a binary system and better constraints on its nature (donor type, etc.). We find that the optical to X-ray flux ratio shows very little variation as a function of accretion rate, but testing for different disc geometry scenarios we find that the optical contribution of the disc increases as the p value decreases [T(r) ∼ r−p]. Moreover, observational data are in agreement with a thicker disc scenario (p < 0.65), which could also possibly explain the lack of observed high-inclination systems." @default.
- W4224256058 created "2022-04-26" @default.
- W4224256058 creator A5015315882 @default.
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- W4224256058 creator A5024407299 @default.
- W4224256058 creator A5086945831 @default.
- W4224256058 date "2022-04-07" @default.
- W4224256058 modified "2023-10-11" @default.
- W4224256058 title "Average bolometric corrections and optical to X-ray flux measurements as a function of accretion rate for X-ray binaries" @default.
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- W4224256058 doi "https://doi.org/10.1093/mnras/stac940" @default.
- W4224256058 hasPublicationYear "2022" @default.
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