Radiation pressure, absorption and AGN feedback in the Chandra Deep Fields

These two models are then used to calculate the number of SLSNe-I, in bins of ∆z = 0.5 width, centred on multiples of z = 0.5 up to z = 3.5 which is consistent with the highest

MD simulations in this and previous work has allowed us to propose a relation between the nature of the interactions at the interface and the observed properties of nanofluids:

 The expansionary monetary policy measures have had a negative impact on net interest margins both via the reduction in interest rates and –less powerfully- the flattening of the

Recent observations of the bulge display a gradient of the mean metallicity and of [Ƚ/Fe] with distance from galactic plane.. Bulge regions away from the plane are less

In the previous sections we have shown how astronomical alignments and solar hierophanies – with a common interest in the solstices − were substantiated in the

The model with power-law density profile (Col. 4 in Table 6) gives the best overall fit to the SED, ISO-SWS spectrum and line emission (see Fig. 4), with quite different disc

(hundreds of kHz). Resolution problems are directly related to the resulting accuracy of the computation, as it was seen in [18], so 32-bit floating point may not be appropriate

Even though the 1920s offered new employment opportunities in industries previously closed to women, often the women who took these jobs found themselves exploited.. No matter