Clumpy stellar winds and the obscuration of active galactic nuclei

(Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs)..

Each model is defined by a set of parameters: effective temperature, surface gravity and stellar radius (all these quantities are defined at τ Ross = 2/3), the exponent of the

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

Figure 6 shows the same normalized intensity as Figure 5 but only for the horizontal segment edges, with measurements of the phasing subaperture on the segment center and shift left

In each panel, we show two MDFs derived from the simulations: one based upon the use of all star particles belonging to the bulge, after ap- plication of the kinematic

Figure 5 shows that the underlying stellar populations of the local H ii galaxies are compatible with the evolution of LCBGs in the sense that their B
R colors were the same at

2 we present the available observations and discuss the influence of the stellar ac- tivity on the radial velocity (RV) variation measurements. Sec- tion 3 shows the results of

An example of projected stellar mass density for the disk, spheroid, and galaxy stellar particles is given in Figure 2 for G-1536, as well as the position of the radial cut we use