Observation of a short-lived pattern in the solar chromosphere

In this work we investigate the dynamic behavior of inter-network regions of the solar chromosphere. We observed the chromosphere of the quiet Sun using a narrow-band Lyot filter centered at the Ca II K 2v emission peak with a bandpass of 0.3A. We achieved a spatial resolution of on average 0.7" at a cadence of 10s. In the inter-network we find a mesh-like pattern that features bright grains at the vertices. The pattern has a typical spatial scale of 1.95" and a mean evolution time scale of 53s with a standard deviation of 10s. A comparison of our results with a recent three-dimensional radiation hydrodynamical model implies that the observed pattern is of chromospheric origin. The measured time scales are not compatible with those of reversed granulation in the photosphere although the appearance is similar. A direct comparison between network and inter-network structure shows that their typical time scales differ by at least a factor of two. The existence of a rapidly evolving small-scale pattern in the inter-network regions supports the picture of the lower chromosphere as a highly dynamical and intermittent phenomenon.Comment: Letter A&A 4 pages 5 figure

On The Evolution of Magnetic White Dwarfs

We present the first radiation magnetohydrodynamics simulations of the atmosphere of white dwarf stars. We demonstrate that convective energy transfer is seriously impeded by magnetic fields when the plasma-beta parameter, the thermal to magnetic pressure ratio, becomes smaller than unity. The critical field strength that inhibits convection in the photosphere of white dwarfs is in the range B = 1-50 kG, which is much smaller than the typical 1-1000 MG field strengths observed in magnetic white dwarfs, implying that these objects have radiative atmospheres. We have then employed evolutionary models to study the cooling process of high-field magnetic white dwarfs, where convection is entirely suppressed during the full evolution (B > 10 MG). We find that the inhibition of convection has no effect on cooling rates until the effective temperature (Teff) reaches a value of around 5500 K. In this regime, the standard convective sequences start to deviate from the ones without convection owing to the convective coupling between the outer layers and the degenerate reservoir of thermal energy. Since no magnetic white dwarfs are currently known at the low temperatures where this coupling significantly changes the evolution, effects of magnetism on cooling rates are not expected to be observed. This result contrasts with a recent suggestion that magnetic white dwarfs with Teff < 10,000 K cool significantly slower than non-magnetic degenerates.Comment: 11 pages, 12 figures, accepted for publication in the Astrophysical Journa

Development of a tritium permeation barrier on F82H-mod. Sheets and on MANET tubes by hot dip aluminising and subsequent heat treatment

Entwicklung von Tritiumpermeationshemmenden Schichten auf F82H-mod. Blechen und MANET Rohren nach dem Hot-Dip Aluminierverfahren mit anschließender Wärmebehandlung In der vorliegenden Arbeit werden die Ergebnisse von tauchaluminierten Blechproben aus F82H-mod. und Rohrproben aus MANET diskutiert. Die anschließende Wärmebehandlung an den getauchten Proben (1040°C, 0.5 h / 750°C, 1 h bzw. 1075°C, 0.5 h / 750°C, 2 h) entspricht der Vergütungsvorschrift für F82H-mod. bzw. der für MANET. Das Hot-Dip Aluminierverfahren mit anschließender Wärmebehandlung eignet sich als Beschichtungsmethode sowohl für Blechproben als auch für die Innen- und Außenbeschichtung von Rohren. Die Zusammensetzung und Dicke der hergestellten Schichten ist unabhängig vom eingesetzten Stahl. Des weiteren wird gezeigt, daß die hergestellten Aluminidschichten in Pb-17Li beständig sind, der PRF genügend hoch ist und die einzelnen Prozeßschritte mit der ITM Geometrie und der Fabrikationssequenz vereinbar sind