Full stars

The reduced characteristic frequencies Q(Q)/Q3, as obtained from NSE measurements, are plotted vs. Q for both systems in Fig. 54. The minimum, which occurs for the full stars, does not occur in the system, where the... 

For the single labelled arm the limiting behavior of Q(Q)/Q3 at small and large Q(z 1 and z > 1) agrees with that of the full star. Thereby, the crossover of Q from Q3- to the Q2-dependence is much more gentle than that observed for unattached linear PDMS chains [128] or in the case of the 4-arm PIP stars [150] (see Fig. 52). 

This is different for the star core. Figure 57 provides a comparison of the spectra at two Q-values with those from an equivalent full star (sample 3). Over short periods of time, both sets of spectra nearly coincide. However, over longer periods of time, the relaxation of the star core is strongly retarded and seems to reach a plateau level. This effect may be explained by the occurrence of interarm entanglements as recently proposed by scaling arguments [135]. 

The absolute values of the reduced relaxation rates at Q1/2 > 1 are smaller at the core than at the shell of the stars. The corresponding values for the full stars are the arithmetic mean of the core and the shell value... 

The NSE spectra from full stars are well described by the scattering law of the Zimm model in the whole experimental time window (20 ns)... 

Figure 10 Mg/Si versus Al/Si for chondritic meteorites and the Earth s mantle. Carbonaceous chondrites are on the right side of the solar ratio (full star), ordinary and enstatite chondrites are on the left side, reflecting depletion of refractory elements. The Earth s mantle plots above Cl-chondrites. Putting 5% Si into the core of the Earth leads to a PM composition compatible with CV-chondrites (after O Neill and Palme, 1998).

Figwe 9 Phase diagram of the system DMAc/SAN/PS at 20 °C modeled on the basis of the Flory-Huggins theory, treating SAN as a single component. Squares, experimental cloud points empty star, experimental critical point full star, calculated critical point full lines, calculated tie lines dotted curve, calculated spinodal line. Reprinted with permission from Loske, S. Schneider, A. Wolf, B. A. Macromolecules 2003, 36, 5008. Copyright 2003 American Chemical Society. 

During a run, if the supply voltage to a motor terminal drops to 85% of its rated value, then the full load torque of the motor will decrease to 72.25%. Since the load and its torque requirement will remain the same, the motor will star to drop speed until the torque available on its speed-torque curve has a value as high as 100/0.7225 or 138.4% of T to sustain this situation. The motor will now operate at a higher slip, increasing the rotor slip losses also in the same proportion. See equation (1.9) and Figure 1.7. 

Star contactor C and A/Tcontactor Ci must be rated for the square of the percentage lapping. For a tapping of 80%., for instance, the rating of the contactors C and Ci will be (0.8) or 64% of the full-load current of the motor. The main contactor Ct, however, will be rated for the full-load current. 

The presence of a single polarization function (either a full set of the six Cartesian Gaussians dxx, d z, dyy, dyz and dzz, or five spherical harmonic ones) on each first row atom in a molecule is denoted by the addition of a. Thus, STO/3G means the STO/3G basis set with a set of six Cartesian Gaussians per heavy atom. A second star as in STO/3G implies the presence of 2p polarization functions on each hydrogen atom. Details of these polarization functions are usually stored internally within the software package. 

Using this very strict criterion of remission, the STAR D researchers reported that 37 per cent of the patients in the trial recovered from depression on the first medication they were given. Another 19 per cent of the full group of patients recovered on the second medication, 6 per cent on the third and 5 per cent on the fourth. Altogether, 67 per cent of the patients recovered. However, the remission of symptoms turned out to be only temporary for many - approximately half of the patients who recovered relapsed within a year. 

Note that, again, three different types of variables were combined chain length, component ratio, and absolute component level. Thus, a "standard" constrained mixture design was not appropriate. In this case a full factorial, central composite design was used, with a total of 20 data points. The star points were... 

Figure 19 Schematic effect of the STAR operator on 2JCH and 3,/CH couplings. The vicinal component of magnetization in the long-range response that is two-bond coupled to a protonated carbon experiences modulation, which serves as a pseudo-evolution for this coupling. In contrast, the vicinal component of magnetization in the long-range response that is three-bond coupled to a protonated carbon does not exhibit a F, skew. Homonuclear modulation during the evolution period f, is still present, as the full experiment is not a constant-time experiment.

Fig. 1. Left panel. Spectroscopic observations of [Cu/Fe] versus [Fe/H] for thick-disk (open symbols) and thin-disk stars (full symbols). Right panel. The same for [Zn/Fe],...

Abstract. Coronal abundances have been a subject of debate in the last years due to the availability of high-quality X-ray spectra of many cool stars. Coronal abundance determinations have generally been compared to solar photospheric abundances from this a number of general properties have been inferred, such as the presence of a coronal metal depletion with an inverse First Ionization Potential dependence, with a functional form dependent on the activity level. We report a detailed analysis of the coronal abundance of 4 stars with various levels of activity and with accurately known photospheric abundances. The coronal abundance is determined using a line flux analysis and a full determination of the differential emission measure. We show that, when coronal abundances are compared with real photospheric values for the individual stars, the resulting pattern can be very different some active stars with apparent Metal Abundance Deficiency in the corona have coronal abundances that are actually consistent with their photospheric counterparts. 

Fig. 4. left [C/Fe] versus [Fe/H] for the full sample. The scatter on [C/Fe] is very large, right same for the non-mixed stars. All stars with [C/Fe] < 0 have gone... 

The difference in the Li abundances in the G-stars of the Pleiades and the Sun, combined with the probable similarities in their overall chemical composition tell us that PMS Li depletion cannot be the whole story. Another mechanism, additional to convective mixing, must be responsible for Li depletion whilst solar-type stars are on the main-sequence. Recent PMS models that have their convective treatments tuned to match the structure of the Sun reproduce the mass dependence of Li depletion, but deplete too much Li compared with the Pleiades, and can even explain the solar A (Li) in the case of full spectrum turbulence models [9]. The over-depletion with respect to the Pleiades gets worse at lower masses. Better fits to the Pleiades data are achieved with PMS models that feature relatively inefficient convection with smaller mixing lengths. 

Massive stars play an important role in numerous astrophysical contexts that range from the understanding of starburst environments to the chemical evolution in the early Universe. It is therefore crucial that their evolution be fully and consistently understood. A variety of observations of hot stars reveal discrepancies with the standard evolutionary models (see [1] for review) He and N excesses have been observed in O and B main sequence stars and large depletions of B accompanied by N enhancements are seen in B stars and A-F supergiants [2,3,4,5], All of these suggest the presence of excess-mixing, and have led to the development of a new generation of evolutionary models which incorporate rotation (full reviews in [1], [6], [7]). 

Abstract. We present metallicities for 487 red giants in the Carina dwarf spheroidal (dSph) galaxy that were obtained from FLAMES low-resolution Ca triplet (CaT) spectroscopy. We find a mean [Fe/H] of —1.91dex with an intrinsic dispersion of 0.25 dex, whereas the full spread in metallicities is at least one dex. The analysis of the radial distribution of metallicities reveals that an excess of metal poor stars resides in a region of larger axis distances. These results can constrain evolutionary models and are discussed in the context of chemical evolution in the Carina dSph. 

The accretion history of a parent galaxy is constructed using a semi-analytical code. The full phase-space evolution during each accretion event is then followed separately with numerical simulations [2]. Star-formation and chemical evolution models are implemented within each satellite. The star formation prescription matches the number and luminosity of present-day galaxies in the Local Group, whereas the chemical evolution model takes into account the metal enrichment of successive stellar populations as well as feedback processes. Below we present results of a sample of four such simulated galaxy halos, denoted as Halos HI, H2, H3 and H4. 

While this theory has been shown to be very successful in the case of massive stars (Maeder and Meynet, this volume) and Population 1 low-mass stars (Charbonnel, this volume), full and self-consistent application in the case of globular... 

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