528 research outputs found
Hydrodynamic modelling of accretion flows
In the proceedings of this, and of several recent close binary conferences,
there have been several contributions describing smoothed particle
hydrodynamics simulations of accretion disks. It is apposite therefore to
review the numerical scheme itself with emphasis on its advantages for disk
modelling, and the methods used for modelling viscous processes.Comment: 3 pages, to appear in proceedings of IAU Colloquium 194: Compact
binaries in the galaxy and beyon
Comprehensive simulations of superhumps
(Abridged) We use 3D SPH calculations with higher resolution, as well as with
more realistic viscosity and sound-speed prescriptions than previous work to
examine the eccentric instability which underlies the superhump phenomenon in
semi-detached binaries. We illustrate the importance of the two-armed spiral
mode in the generation of superhumps. Differential motions in the fluid disc
cause converging flows which lead to strong spiral shocks once each superhump
cycle. The dissipation associated with these shocks powers the superhump. We
compare 2D and 3D results, and conclude that 3D simulations are necessary to
faithfully simulate the disc dynamics. We ran our simulations for unprecedented
durations, so that an eccentric equilibrium is established except at high mass
ratios where the growth rate of the instability is very low. Our improved
simulations give a closer match to the observed relationship between superhump
period excess and binary mass ratio than previous numerical work. The observed
black hole X-ray transient superhumpers appear to have systematically lower
disc precession rates than the cataclysmic variables. This could be due to
higher disc temperatures and thicknesses. The modulation in total viscous
dissipation on the superhump period is overwhelmingly from the region of the
disc within the 3:1 resonance radius. As the eccentric instability develops,
the viscous torques are enhanced, and the disc consequently adjusts to a new
equilibrium state, as suggested in the thermal-tidal instability model. We
quantify this enhancement in the viscosity, which is ~10 per cent for q=0.08.
We characterise the eccentricity distributions in our accretion discs, and show
that the entire body of the disc partakes in the eccentricity.Comment: 18 pages (mn2e LaTeX), 14 figures, 5 tables, Accepted for publication
in MNRA
Intracavernous Calcitonin-gene Related Peptide Plus Prostaglandin E 1. Possible Alternative to Penile Implants in Selected Patients.
One NASA: Sharing Knowledge Through an Agency-wide Process Asset Library (PAL)
This poster session will cover the key purpose and components behind implementing the NASA PAL website. This session will present the current results, describing the process used to create the website, the current usage measure, and will demonstrate how NASA is truly becoming ONE. The target audience for the poster session includes those currently implementing the CMMI model and looking for PAL adoption techniques. To continue to be the leader in space, science and technology, NASA is using this agency-wide PAL to share knowledge, work products and lessons learned through this website. Many organizations have failed to recognize how the efforts of process improvement fit into overall organizational effort. However, NASA as an agency has adopted the benefits of process improvement by the creation of this website to foster communication between its ten centers. The poster session will cover the following, topics outlined below: 1) Website purpose; 2) Characteristics of the website; 3) User accounts status; 4) Website content size; and 5) Usage percentages
Propeller-activated resonances and the fate of short-period cataclysmic variables
We show that the combination of a weak magnetic propeller and accretion disc resonances can effectively halt accretion in short-period cataclysmic variables (CVs) for large fractions of their lifetimes. This may help to explain the discrepancy between the observed and predicted orbital period distributions of CVs at short periods. Orbital resonances cause the disc to become eccentric, allowing material to fall back on to the donor star or out of the system. A weak magnetic field on a rapidly spinning primary star propels disc material outwards, allowing it to access these resonances. Numerical and analytic calculations show that this state can be long lived (∼1011 yr). This is because the magnetic propeller is required only to maintain access to the resonances, and not to push matter out of the Roche lobe, so that the spin-down time-scale is much longer than that for a classical propeller mode
Role of the nitric oxide donor linsidomine chlorhydrate (SIN-1) in the diagnosis and treatment of erectile dysfunction
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