Wigner crystallization in quantum electron bilayers

The phase diagram of quantum electron bilayers in zero magnetic field is obtained using density functional theory. For large electron densities the system is in the liquid phase, while for smaller densities the liquid may freeze (Wigner crystallization) into four different crystalline phases; the lattice symmetry and the critical density depend on the the inter-layer distance. The phase boundaries between different Wigner crystals consist of both first and second order transitions, depending on the phases involved, and join the freezing curve at three different triple points.Comment: To appear in Europhys. Lett. (11 pages in REVTEX + 2 figures in postscript

TCP over High Speed Variable Capacity Links: A Simulation Study for Bandwidth Allocation

New optical network technologies provide opportunities for fast, controllable bandwidth management. These technologies can now explicitly provide resources to data paths, creating demand driven bandwidth reservation across networks where an applications bandwidth needs can be meet almost exactly. Dynamic synchronous Transfer Mode (DTM) is a gigabit network technology that provides channels with dynamically adjustable capacity. TCP is a reliable end-to-end transport protocol that adapts its rate to the available capacity. Both TCP and the DTM bandwidth can react to changes in the network load, creating a complex system with inter-dependent feedback mechanisms. The contribution of this work is an assessment of a bandwidth allocation scheme for TCP flows on variable capacity technologies. We have created a simulation environment using ns-2 and our results indicate that the allocation of bandwidth maximises TCP throughput for most flows, thus saving valuable capacity when compared to a scheme such as link over-provisioning. We highlight one situation where the allocation scheme might have some deficiencies against the static reservation of resources, and describe its causes. This type of situation warrants further investigation to understand how the algorithm can be modified to achieve performance similar to that of the fixed bandwidth case

Glaciotectonic Structures in Central Sweden and their Significance for Glacial Theory

Various glaciotectonic structures and landforms created by ice pushing are common in drift and interstadial sediments in a narrow belt of central Sweden. Described examples from the Lake Storsjôn vicinity demonstrate that glaciotectonic deformation took place while the area was deeply covered by the last Fennoscandian Ice Sheet. Deformation was controlled by pressure gradients related to position of the ice divide and ice movement away from the divide. As the position of the divide shifted during the last glaciation, so did the orientation of glaciotectonic structures. The regional distribution of glaciotectonic features in Fennoscandia falls into three zones: (1) inner zone of widespread, small- to moderate-sized features in older drift, (2) intermediate zone of small, isolated features in drift of the last glaciation, and (3) outer zone with all manner of large and small features in drift and soft bedrock. These zones are the cumulative results of multiple glaciations and reflect the overall distribution of deformable sediment and bedrock within the continental substratum.Diverses structures glaciotectoniques et formes engendrées par la poussée des glaces sont courantes dans les dépôts glaciaires et les sédiments interstadiaires d'une étroite zone du centre de la Suède. La description de certains exemples observés dans les environs du lac Storsjôn démontre que des déformations glaciotectoniques se sont produites pendant que la région était profondément enfouie sous le dernier inlandsis finnoscandien. Les déformations étaient commandées par le gradient de pression en relation avec la position de la ligne de partage glaciaire et le mouvement des glaces en direction opposée de cette ligne. Au cours de la dernière glaciation, l'orientation des structures glaciotectoniques s'est déplacée en même temps que la ligne de partage des glaces. En Finnoscandinavie, les structures glaciotectoniques se répartissent en trois zones: 1) une zone interne où les éléments de petite à moyenne tailles abondent dans des dépôts anciens; 2) une zone intermédiaire où de petits éléments sont isolés dans les dépôts de la dernière glaciation; et 3) une zone externe où des éléments de toutes tailles se trouvent dans les dépôts et le substratum sédimentaire. Ces zones sont le résultat du cumul des multiples glaciations et reflètent la répartition totale des sédiments et du substratum non résistant à l'intérieur du socle continental.Glacialtektoniska strukturer i Mellan-Sverige och deras betydelse for glaciationsteorin. Glacialtektoniska strukturer och landformer uppkomna genom istryck âr vanliga i glaciala och interstadiala sediment i ett smalt stràk genom mellersta Sverige. De beskrivna exemplen fran Storsjôtrakten visar att glacialtektonisk deformation skedde medan omràdet ànnu var tâckt av mâktig inlandsis. Deformationen uppkom genom ett tryck, vars riktning bestamdes av lâget i fôrhallande till isdelaren och isytans lutning fran deanna. Dà isdelarens lâge àndrades under loppet av den senaste glaciationen, àndrades ocksà orienteringen av de glacialtektoniska strukturerna. De glacialtektoniska fenomenen i Fennoskandia fôrdelar sig regionalt pà tre zoner: (1)en inre zon med vitt utbredda sma till medelstora strukturer i àldre glaciala bildningar, (2) en mellanzon med smâ, isolerade strukturer i glaciala bildningar fràn den senaste glaciationen, och (3) en yttre zon med alla typer av stora och sma former och strukturer i de glaciala bildningarna och deras berggrundsunderlag. Dessa zoner utgôr det samlade resultatet av inverkan fràn upprepade glaciationer och àterspeglar utvecklingen under lang tid av de stora inlandsisarnas underlag

Nickel Mixing in the Outer Layers of SN 1987A

Supernova 1987A remains the most well-observed and well-studied supernova to date. Observations produced excellent broad-band photometric and spectroscopic coverage over a wide wavelength range at all epochs. Here, we focus on the very early spectroscopic observations. Only recently have numerical models been of sufficient detail to accurately explain the observed spectra. In SN 1987A, good agreement has been found between observed and synthetic spectra for day one, but by day four, the predicted Balmer lines become much weaker than the observed lines. We present the results of work based on a radiation-hydrodynamic model by Blinnikov and collaborators. Synthetic non-LTE spectra generated from this model by the general radiation transfer code PHOENIX strongly support the theory that significant mixing of nickel into the outer envelope is required to maintain strong Balmer lines. Preliminary results suggest a lower limit to the average nickel mass of 1.0 \times 10^{-5} solar masses is required above 5000 \kmps by day four. PHOENIX models thus have the potential to be a sensitive probe for nickel mixing in the outer layers of a supernova.Comment: 16 pages, 7 figures, ApJ, v556 2001 (in press

Observations of the Crab Nebula and its pulsar in the far-ultraviolet and in the optical

We present HST/STIS far-UV observations of the Crab nebula and its pulsar. Broad, blueshifted absorption arising in the nebula is seen in C IV 1550, reaching about 2500 km/s. This can be interpreted as evidence for a fast outer shell, and we adopt a spherically symmetric model to constrain the properties of this. We find that the density appears to decrease outward in the shell. A lower limit to the mass is 0.3 solar masses with an accompanying kinetic energy of 1.5EE{49} ergs. A massive 10^{51} erg shell cannot be excluded, but is less likely if the density profile is much steeper than R^{-4} and the velocity is <6000 km/s. The observations cover the region 1140-1720 A. With the time-tag mode of the spectrograph we obtain the pulse profile. It is similar to that in the near-UV, although the primary peak is marginally narrower. Together with the near-UV data, and new optical data from NOT, our spectrum of the pulsar covers the entire region from 1140-9250 A. Dereddening the spectrum gives a flat spectrum for E(B-V)=0.52, R=3.1. This dereddened spectrum of the Crab pulsar can be fitted by a power law with spectral index alpha_{\nu} = 0.11 +/- 0.04. The main uncertainty is the amount and characteristics of the interstel- lar reddening, and we have investigated the dependence of \alpha_{\nu} on E(B-V) and R. In the extended emission covered by our 25" x 0.5" slit in the far-UV, we detect C IV 1550 and He II 1640 emission lines from the Crab nebula. Several interstellar absorption lines are detected toward the pulsar. The Ly alpha absorption indicates a column density of 3.0+/-0.5\EE{21} cm^{-2} of neutral hydrogen, which agrees well with our estimate of E(B-V)=0.52 mag. Other lines show no evidence of severe depletion of metals in atomic gas.Comment: 18 pages emulateapj style, including 10 figures. ApJ, accepte