By Martinez-Pais I.G., Shahbaz T., Velazquez J.C. (eds.)
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Additional resources for Accretion Processes in Astrophysics (Canary Islands Winter School of Astrophysics)
For an isothermal disk (T independent of z), this is equivalent to taking the viscosity parameter α independent of z. As long as we are not sure what causes the viscosity, this is a reasonable simpliﬁcation. f. 8). 43 is still valid for rotation rates Ω deviating from Keplerian (only the integration over disk thickness must 3 If you prefer a more formal derivation, the fastest way is to consult Landau and Lifshitz (1959), chapter 15 (hereafter LL). Noting that the divergence of the ﬂow vanishes for a thin axisymmetric disk, the viscous stress σ becomes (LL eq.
59. 55, ignoring the factor f ). In practice, this works out to a factor of a few. The surface of the belt is therefore not very hot. The situation is quite diﬀerent if the boundary layer is not optically thick (Pringle and Savonije, 1979). It then heats up to much higher temperatures. Analytical methods to obtain the boundary layer structure have been used by Regev and Hougerat (1988), numerical solutions of the slim disk type by Narayan and Popham (1994) and Popham (1997), and 2-D numerical simulations by Kley (1991).
These simulations show an outburst during which the accretion in the inner disk is enhanced, between two episodes in which mass accumulates in the outer disk. 1 Comparison with LMXB observations: irradiated disks In low-mass X-ray binaries, a complication arises because of the much higher luminosity of the accreting object. Because a neutron star is roughly 1,000 times smaller than a white dwarf, it produces 1,000 times more luminosity for a given accretion rate. 55. 2). If the disk is concave, it will intercept some of this luminosity.
Accretion Processes in Astrophysics (Canary Islands Winter School of Astrophysics) by Martinez-Pais I.G., Shahbaz T., Velazquez J.C. (eds.)