Fractal analysis of the GRB light curves

AX J1910.7+0917: the slowest X-ray pulsar

“…For the characteristic valuesṀ = 10 14 g s −1 (corresponding to the X-ray luminosity Lx = 10 34 erg s −1 ) and the canonical NS surface magnetic field B = 10 12 G (corresponding to the NS dipole magnetic moment µ = 10 30 G cm 3 µ30), we find (see Shakura & Postnov 2017 for more detail and derivations) that the magnetospheric radius is RA ∼ 3 × 10 9 cm, Z ∼ 5 − 10 and τ ≃ 10 4 years, the latter being only weakly dependent on the mass accretion rateṀ . The solution of Eq.…”

Radiative Processes in High Energy Astrophysics

“…Matter around the hole is attracted by the black hole gravity, it is compressed, heated, and then radiates. This was realized quite soon (Salpeter 1964;Zeldovich 1964;Lynden-Bell 1969;Shakura & Sunjaev 1973) 1 .…”

Supermassive black holes in the EAGLE Universe. Revealing the observables of their growth

“…For Eddington ratios larger than 10 −2 , we assume that the nuclear disc around the SMBH is thin and radiative cooling is efficient. We therefore assume that the luminosity of the disc can be described by the standard Shakura-Sunyaev disc model (Shakura & Syunyaev 1973). Such sources will be highly luminous in X-rays.…”

“…where r is the radiative efficiency and is set to 0.1 as suggested by Shakura & Syunyaev (1973). We use the redshift independent bolometric corrections of Marconi et al (2004) to convert the bolometric luminosity into intrinsic hard (2-10 keV) and soft (0.5-2 keV) X-ray band luminosities.…”