9,318 research outputs found
Thermally-driven Neutron Star Glitches
We examine the thermal and dynamical response of a neutron star to a sudden
perturbation of the inner crust temperature. During the star's evolution,
starquakes and other processes may deposit \gap 10^{42} ergs, causing
significant internal heating and increased frictional coupling between the
crust and the more rapidly rotating neutron superfluid the star is expected to
contain. Through numerical simulation we study the propagation of the thermal
wave created by the energy deposition, the induced motion of the interior
superfluid, and the resulting spin evolution of the crust. We find that energy
depositions of ergs produce gradual spin-ups above the timing
noise level, while larger energy depositions produce sudden spin jumps
resembling pulsar glitches. For a star with a temperature in the observed range
of the Vela pulsar, an energy deposition of ergs produces a
large spin-up taking place over minutes, similar to the Vela ``Christmas''
glitch. Comparable energy deposition in a younger and hotter ``Crab-like'' star
produces a smaller spin-up taking place over day, similar to that seen
during the partially time-resolved Crab glitch of 1989.Comment: 21 pages plus 17 figures, uuencode compressed Postscript. Accepted
for publication in the Astrophysical Journa
Late-Time Convection in the Collapse of a 23 Solar Mass Star
The results of a 3-dimensional SNSPH simulation of the core collapse of a 23
solar mass star are presented. This simulation did not launch an explosion
until over 600ms after collapse, allowing an ideal opportunity to study the
evolution and structure of the convection below the accretion shock to late
times. This late-time convection allows us to study several of the recent
claims in the literature about the role of convection: is it dominated by an
l=1 mode driven by vortical-acoustic (or other) instability, does it produce
strong neutron star kicks, and, finally, is it the key to a new explosion
mechanism? The convective region buffets the neutron star, imparting a 150-200
km/s kick. Because the l=1 mode does not dominate the convection, the neutron
star does not achieve large (>450 km/s) velocities. Finally, the neutron star
in this simulation moves, but does not develop strong oscillations, the energy
source for a recently proposed supernova engine. We discuss the implications
these results have on supernovae, hypernovae (and gamma-ray bursts), and
stellar-massed black holes.Comment: 31 pages (including 13 figures), submitted to Ap
Solar Carboreduction of Alumina under Vacuum
AbstractMain requirements for successful production of aluminum via carboreduction of alumina using solar vacuum reactors are sufficiently high reaction temperature, suitable low partial pressure of the product gases, fast heating and quenching at temperature low enough to prevent backward reaction. Based on these requests a batch solar reactor was modeled, designed, built and tested. Experimental results of the solar tests under different vacuum levels and temperature conditions will be presented. It will be shown that for reaction temperature, which is above the minimal temperature required for full conversion as predicted by thermodynamic calculations for appropriate pressure, the alumina to aluminum conversion is above 90%. Not reaching the full conversion can be explained by the byproducts formation during the initial preheating. At lower reaction temperatures and higher CO partial pressure by products can also be formed when reaching steady state condition both in the forward and backward reactions. This formation in the forward reaction is confirmed by the discovery of larger amounts of Al4C3, Al4CO4 solids as the residual byproducts in the reactants holder and higher alumina content in the deposits on the cold parts of the reactor that originated from the volatile Al2O produced in the forward reaction which during the deposition converts to alumina and aluminum. Decreasing the reaction temperature is accompanied by decreasing the temperature in the hot zone that causes the increasing of the deposit mass there with higher amount of Al4C3 and Al4CO4 produced in the backward reaction. Nano crystalline and amorphous morphology of the deposits in the cold zone caused by fast cooling will also be discussed
Chemical equilibrium and stable stratification of a multi-component fluid: thermodynamics and application to neutron stars
A general thermodynamic argument shows that multi-component matter in full
chemical equilibrium, with uniform entropy per baryon, is generally stably
stratified. This is particularly relevant for neutron stars, in which the
effects of entropy are negligible compared to those of the equilibrium
composition gradient established by weak interactions. It can therefore be
asserted that, regardless of the uncertainties in the equation of state of
dense matter, neutron stars are stably stratified. This has important,
previously discussed consequences for their oscillation modes, magnetic field
evolution, and internal angular momentum transport.Comment: AASTeX, 8 pages, including 1 PS figure. Accepted for publication in
The Astrophysical Journa
Instability and spatiotemporal rheochaos in a shear-thickening fluid model
We model a shear-thickening fluid that combines a tendency to form
inhomogeneous, shear-banded flows with a slow relaxational dynamics for fluid
microstructure. The interplay between these factors gives rich dynamics, with
periodic regimes (oscillating bands, travelling bands, and more complex
oscillations) and spatiotemporal rheochaos. These phenomena, arising from
constitutive nonlinearity not inertia, can occur even when the steady-state
flow curve is monotonic. Our model also shows rheochaos in a low-dimensional
truncation where sharply defined shear bands cannot form
Limit cycles in the presence of convection, a travelling wave analysis
We consider a diffusion model with limit cycle reaction functions, in the
presence of convection. We select a set of functions derived from a realistic
reaction model: the Schnakenberg equations. This resultant form is
unsymmetrical. We find a transformation which maps the irregular equations into
model form. Next we transform the dependent variables into polar form. From
here, a travelling wave analysis is performed on the radial variable. Results
are complex, but we make some simple estimates.
We carry out numerical experiments to test our analysis. An initial `knock'
starts the propagation of pattern. The speed of the travelling wave is not
quite as expected. We investigate further. The system demonstrates distinctly
different behaviour to the left and the right. We explain how this phenomenon
occurs by examining the underlying behaviour.Comment: 20 pages, 5 figure
Ledoux-Convection in Protoneutron Stars --- a Clue to Supernova Nucleosynthesis?
Two-dimensional hydrodynamical simulations of the deleptonization of a newly
formed neutron star were performed. Driven by negative lepton fraction and
entropy gradients, convection starts near the neutrinosphere about 20-30 ms
after core bounce, but moves deeper into the protoneutron star, and after about
one second the whole protoneutron star is convective. The deleptonization of
the star proceeds much faster than in the corresponding spherically symmetrical
model because the lepton flux and the neutrino luminosities increase by up to a
factor of two. The convection below the neutrinosphere raises the
neutrinospheric temperatures and mean energies of the emitted neutrinos by
10-20%. This can have important implications for the supernova explosion
mechanism and changes the detectable neutrino signal from the Kelvin-Helmholtz
cooling of the protoneutron star. In particular, the enhanced electron neutrino
flux relative to the electron antineutrino flux during the early post-bounce
evolution might solve the overproduction problem of certain elements in the
neutrino-heated ejecta in models of type-II supernova explosions.Comment: 17 pages, LaTeX, 8 postscript figures, uses epsf.sty. To appear in
ApJ 473 (Letters), 1996 December 1
Large area pulse ionization chamber for measurement of extremely heavy cosmic rays
Parallel plate ionization chamber for identifying relativistic cosmic ray nucle
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