Fe Kα lines from accreting black holes are produced mostly outside 10 gravitational radii due to radial ionization gradients, allowing broad profiles without high spin.
Science with the x-ray imaging and spectroscopy mission (xrism).arXiv preprint arXiv:2003.04962,
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Simulation analysis of 415 clusters reveals two accretion regimes: warm filament gas enters slowly thermalizing at 2-4 R200 while tangential velocity gradients and hot gas ejection appear at 1-2 R200, with no strong filament accretion shocks.
Bayesian fitting of NICER comet X-ray data identifies three spectral families and shows carbon-derived freeze-in temperatures lower than those from nitrogen and oxygen lines, with short-term variability attributed to solar-wind charge-state changes.
DIXE NXB averages 4.46e-2 counts s^-1 cm^-2 keV^-1 at the geomagnetic equator under solar minimum, dominated by cosmic-proton-induced particles, rising to 1.55e-1 at higher latitudes, with SAA delayed background negligible after ~5 minutes.
citing papers explorer
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Simulation-Based Prediction of Black Hole Fe K$\alpha$ Line Profiles
Fe Kα lines from accreting black holes are produced mostly outside 10 gravitational radii due to radial ionization gradients, allowing broad profiles without high spin.
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Cosmic gas accretion from filaments onto galaxy clusters using the IllustrisTNG simulation
Simulation analysis of 415 clusters reveals two accretion regimes: warm filament gas enters slowly thermalizing at 2-4 R200 while tangential velocity gradients and hot gas ejection appear at 1-2 R200, with no strong filament accretion shocks.
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Bayesian Modeling of NICER Cometary X-ray Spectra: A Legacy Survey of Solar-Wind Charge Exchange
Bayesian fitting of NICER comet X-ray data identifies three spectral families and shows carbon-derived freeze-in temperatures lower than those from nitrogen and oxygen lines, with short-term variability attributed to solar-wind charge-state changes.
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Simulation of non X-ray background for the DIffuse X-ray Explorer (DIXE) mission
DIXE NXB averages 4.46e-2 counts s^-1 cm^-2 keV^-1 at the geomagnetic equator under solar minimum, dominated by cosmic-proton-induced particles, rising to 1.55e-1 at higher latitudes, with SAA delayed background negligible after ~5 minutes.