We used the standard geometrical thin accretion theory to obtain the accretion rates in Seyfert 1 galaxies and quasars. Combining accretion rates with the bolometric luminosity, we obtained the accretion efficiency. We found most of Seyfert 1 galaxies and radio quiet quasars have lower accretion efficiencies while most of the radio loud quasars possess higher accretion efficiencies. This findin...

We present a novel method to measure the accretion rate of radio emitting X-ray binaries (XRBs) and active galactic nuclei (AGN) independently of the X-ray luminosity. The radio emission of the jet is used as a tracer for the accretion rate and is normalised using sources of known accretion rates: island state neutron stars and efficiently radiating black holes close to a state transition. We s...

The polars VV Pup and V393 Pav were observed with XMM-Newton during states of low accretion rate with peak X-ray luminosities of ∼1 × 10 and ∼1 × 10 erg s, respectively. In both polars, accretion onto the white dwarf was extremely irregular, and the accretion rate varied by more than 1 order of magnitude on timescales of ∼1 hr. Our observations suggest that this type of irregular accretion is a...

The appearance and time variability of accreting millisecond X-ray pulsars (hereafter AMXPs, e.g. Wijnands & van der Klis 1998) depends strongly on the accretion rate, the effective viscosity and the effective magnetic diffusivity of the disk-magnetosphere boundary. The accretion rate is the main parameter which determines the location of the magnetospheric radius of the star for a given stella...

We investigate the physics of gas accretion in young stellar clusters. Accretion in clusters is a dynamic phenomenon as both the stars and the gas respond to the same gravitational potential. Accretion rates are highly non-uniform with stars nearer the centre of the cluster, where gas densities are higher, accreting more than others. This competitive accretion naturally results in both initial ...

We present results of 3D simulations of MHD instabilities at the accretion diskmagnetosphere boundary. The instability is Rayleigh-Taylor, and develops for a fairly broad range of accretion rates and stellar rotation rates and magnetic fields. It produces tall, thin tongues of plasma that penetrate the magnetosphere in the equatorial plane. The shape and number of the tongues changes with time ...

The transition of a standard thin disk to a radiatively inefficient accretion flow (RIAF) is expected to occur, when ṁ ∼ ṁcrit (ṁ = Ṁ/ṀEdd). The radiative efficiencies of accretion flows accreting at rates lower than the critical accretion rate ṁcrit become significantly lower than that of standard thin disks. It is believed that the initial transition radius is small just after the accretion m...

Accretion rates of order 10 M⊙yr −1 are observed in young pre–main– sequence (PMS) stars of approximately a solar mass with evidence of circumstellar disks. The accretion rate is significantly lower for PMS stars of smaller mass, approximately proportional to the second power of the stellar mass, Ṁaccr ∝ M . The traditional view is that the observed accretion is the consequence of the angular m...

Chemical composition of the empty body was determined in 159 animals slaughtered at weights ranging from 121 to 706 kilograms. Holstein and Angus bulls, steers and heifers were fed at two energy levels: ad libitum and 65 to 70% ad libitum. The allometric equation, Y = aXb, was used to determine the effect of energy intake and the influence of breed and sex on the accretion rates of the chemical...

and Implications The dietary bioavailable riboflavin needs for body maintenance and body protein and fat accretion were estimated in pigs. The riboflavin required to support body protein accretion was higher than that for body maintenance or fat accretion. Specifically, the riboflavin required to support protein accretion was six times higher than the riboflavin required to support fat accretio...