Possible new astrophysics-relevant experiments with high
... References: 1) D.D. Ryutov. “Destabilizing effect of thermal conductivity on the Rayleigh-Taylor instability in a plasma,” Phys. Plasmas, 7, 4797, 2000. 2) D.D. Ryutov, J.Kane, M. Pound, and B. Remington.”Instability of the ablatively accelerated slab for the case of non-normal irradiation.” Plasma ...
... References: 1) D.D. Ryutov. “Destabilizing effect of thermal conductivity on the Rayleigh-Taylor instability in a plasma,” Phys. Plasmas, 7, 4797, 2000. 2) D.D. Ryutov, J.Kane, M. Pound, and B. Remington.”Instability of the ablatively accelerated slab for the case of non-normal irradiation.” Plasma ...
Regions of atoms that have the same magnetic polarity (N/S
... The magnitude of F is F = q·v·B·sinθ where θ is the angle between v and B. In our case the v and B vectors are parallel, so sinθ = 0. In conclusion F = 0. 2. In the figure below, a magnetic field of .01 T is applied locally to a wire carrying a current of intensity I = 10A. What is the magnitude of ...
... The magnitude of F is F = q·v·B·sinθ where θ is the angle between v and B. In our case the v and B vectors are parallel, so sinθ = 0. In conclusion F = 0. 2. In the figure below, a magnetic field of .01 T is applied locally to a wire carrying a current of intensity I = 10A. What is the magnitude of ...
The End of the Dark Ages
... The effects of a top-heavy IMF on the ionization of the surrounding gas and intergalactic medium are spectacular. Fig. 1 shows a comparison between the final stages (100 Myr after the source turn on) of the I-front evolution for a Larson (upper panel) and a Salpeter (bottom) IMF. The source stellar ...
... The effects of a top-heavy IMF on the ionization of the surrounding gas and intergalactic medium are spectacular. Fig. 1 shows a comparison between the final stages (100 Myr after the source turn on) of the I-front evolution for a Larson (upper panel) and a Salpeter (bottom) IMF. The source stellar ...
Planetesimal collisions in binary systems
... as particles at an eccentricity maximum can collide with particles at an eccentricity minimum the resulting encounter velocities are too high for accretion to occur. The presence of a gas disc and the associated aerodynamic gas drag on the particles can effectively damp the oscillations leading to a ...
... as particles at an eccentricity maximum can collide with particles at an eccentricity minimum the resulting encounter velocities are too high for accretion to occur. The presence of a gas disc and the associated aerodynamic gas drag on the particles can effectively damp the oscillations leading to a ...
Morphology and kinematics of the gas envelope of the variable AGB
... This suggests a smooth variation of the expansion velocity from the star equator, where the disk stands, to the star poles on the star axis perpendicular to the disk rather than a bipolar jet confined around the star axis. This had been already remarked by C2006 who proposed an explanation in terms ...
... This suggests a smooth variation of the expansion velocity from the star equator, where the disk stands, to the star poles on the star axis perpendicular to the disk rather than a bipolar jet confined around the star axis. This had been already remarked by C2006 who proposed an explanation in terms ...
Jets and Outflows From Star to Cloud: Observations Confront Theory
... measured on larger scales which then allow mechanisms working on smaller scales to be inferred. That said, we note however that interferometric studies are beginning to resolve the smaller scales directly (see § 2.5). We first consider the ratio of jet mass-flux to accretion rate. Measuring the mass ...
... measured on larger scales which then allow mechanisms working on smaller scales to be inferred. That said, we note however that interferometric studies are beginning to resolve the smaller scales directly (see § 2.5). We first consider the ratio of jet mass-flux to accretion rate. Measuring the mass ...
Spiral Arms - Harry Kroto
... In the disk the density of stars in the spiral arms in only about 5% greater than the density of stars in the rest of the disk. So why are they so much brighter? Newborn clusters are all in the spiral arms. These clusters contain the most luminous and blue stars. So even though the density contrast ...
... In the disk the density of stars in the spiral arms in only about 5% greater than the density of stars in the rest of the disk. So why are they so much brighter? Newborn clusters are all in the spiral arms. These clusters contain the most luminous and blue stars. So even though the density contrast ...
