Accretion Power in Astrophysics

Reconciling the spectrum of Sagittarius A* with a two-temperature plasma model

“…The cell envelope of M. tuberculosis, a Gram-positive bacterium with a G + C-rich genome, contains an additional layer beyond the peptidoglycan that is exceptionally rich in unusual lipids, glycoli-pids and polysaccharides 4,5 . Novel biosynthetic pathways generate cell-wall components such as mycolic acids, mycocerosic acid, phenolthiocerol, lipoarabinomannan and arabinogalactan, and several of these may contribute to mycobacterial longevity, trigger inflammatory host reactions and act in pathogenesis.…”

Magnetic Dipole Equilibrium Solution at Finite Plasma Pressure

“…As a result, the constant c surfaces become more extended and localized about the symmetry plane as b 0 increases. The resulting large b 0 equilibrium resembles the accretion disk associated with star formation [11].…”

The Formation and Disruption of Black Hole Jets

“…We classify them by their normalized luminosity, or the Eddington ratio, D L=L Edd , where L is accretion luminosity and L Edd 1:2 10 38 M BH =Mˇ.erg s 1 / is the Eddington luminosity at which the outward radiation force on the electrons balances the inward gravitational force on the ions (see e.g. Frank et al 2002).…”

“…This keeps the disk cool and geometricallythin, h=r 1. The radiative efficiency of the disk, defined as D L= P M c 2 , is between 0:05 for non-spinning BHs and ' 0:3 for nearly maximally-spinning BHs (Novikov and Thorne 1973) (see also Shapiro and Teukolsky 1986;Frank et al 2002). In many observational applications, authors often set disk radiative efficiency to a characteristic value d D 0:1 and define Eddington mass accretion rate P M Edd D L Edd = d c 2 D 10L Edd =c 2 .…”