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of wind velocity. All luminosities are taken from the radiative phases of the ULXB at ≈ 2 Myr. For vw = 10−3c, the shocked wind cools efficiently and no significant X - ray emission is observed . Figure 7. Open ...
observations , were obtained from the Swift/XRT online product builder2 (Evans et al. 2009). All X - ray light curves were originally extracted in the 2 –10 keV band. These light curves were then converted from ...
Abstract Electron–positron pair production by collision of photons is investigated in view of application to pulsar physics. We compute the absorption rate of individual gamma- ray photons ...
of the bubbles see Pinto et al. (2020) and references therein. Evidence for such winds was first seen through strong residuals at soft X - ray energies ( ...
. (2013) to show that they could be the WDs postulated in Malheiro, Rueda & Ruffini (2012) to describe the observational properties of soft gamma-repeaters (SGRs) and anomalous X - ray pulsars (AXPs ...
Abstract Supersoft X - ray sources (SSSs) are characterized by their low effective temperatures and high X - ray luminosities. The soft X - ray emission can be explained by hydrogen nuclear burning ...
, to Γ ∼ 2.2, appearing to recover the slope of the soft X - ray to UV portion of the spectrum. For this epoch, the observed αox ∼ 1.76. Figure 1. View largeDownload slide The simultaneous NuSTAR and Swift ...
that the synchrotron radiative processes of relativistic electrons injected into the jet can reproduce the radiation ranging from radio to infrared wavebands. However, the origin of both X - rays and soft γ- rays (e.g ...
for more details on crash. The spectral shape of the sources is discretized into 82 frequency bins, where 72 are in the UV regime below hPν = 200 eV, and the rest are in the soft X - ray regime (0.2– 2 keV ...
plasmas are expected to concentrate right on the edge of the relevant pair- production regions in the compactness–temperature parameter space (see above), this suggests that the shape of the X - ray corona ...
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