Results 171 to 180 of about 5,357 (210)
The Wafold: Curvature-Driven Termination and Dimensional Compression in Black Holes. [PDF]
Viaña J.
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A comparative review of time-resolved x-ray and electron scattering to probe structural dynamics. [PDF]
Lee Y, Oang KY, Kim D, Ihee H.
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Optical kicking of liquid droplets for sample delivery in ultrafast soft X-ray experiments. [PDF]
Ebrahimpour Z +3 more
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Multi-messenger dynamic imaging of laser-driven shocks in water using a plasma wakefield accelerator
Balcazar M +31 more
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Deceleration of relativistic jets
New Astronomy Reviews, 2003Abstract There are now good evidences that, on the parsec scale, jets are relativistic also in Fanaroff–Riley I radiogalaxies. On the other hand they are likely to be subrelativistic on larger scale. Here we present preliminary results of numerical simulations of relativistic jets, whose purpose is the analysis of this deceleration process.
G Bodo, P Rossi, A Mignone
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PIC methods in astrophysics: simulations of relativistic jets and kinetic physics in astrophysical systems [PDF]
Ken-Ichi Nishikawa +2 more
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MHD Simulations of Relativistic Jets
Astrophysics and Space Science, 2004In a series of time dependent numerical simulations we have performed a parameter study of magnetised relativistic jets. We have found that the impact of the magnetic field on the morphology of a jet depends strongly on the configuration of the field.
Leismann, T., Aloy, M., Müller, E.
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Relativistic Jets from Active Galactic Nuclei [PDF]
The nuclei of most normal galaxies contain supermassive black holes, which can accrete gas through a disk and become active. These active galactic nuclei (AGNs) can form jets that are observed on scales from astronomical units to megaparsecs and from ...
R D Blandford
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Magnetohydrodynamic Production of Relativistic Jets
Science, 2001A number of astronomical systems have been discovered that generate collimated flows of plasma with velocities close to the speed of light. In all cases, the central object is probably a neutron star or black hole and is either accreting material from other stars or is in the initial violent stages of formation.
D L, Meier, S, Koide, Y, Uchida
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