We measure and analyze the sizes of 82 massive (M ≥ 1011 M &sun;) galaxies at 1. 7 ≤ z ≤ 3 utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our sample provides the first statistical study of massive galaxy sizes at z > 2. We split our sample into disk-like (Sérsic index n ≤ 2) and spheroid-like (Sérsic index n > 2) galaxies

In order to explore the possibilities to synthesize the new superheavy elements with Z=120, 122, 124, 126 some hot-fusion (mass asymmetric) reactions and cold-fusion (less mass asymmetric) reactions are studied. The dynamics of reaction with massive nuclei and the formation probability of heavy and superheavy elements with Z=90-126 in the

It is developed a new approach to analyze the induced fission of heavy nuclei, which takes into account the nuclear dissipation phenomenon and the shell structure of nuclei in determination of fission barriers. The approach is based on the combined dynamical and statistical simulations. In the framework of this approach the method of calculation

The dynamic model is proposed for description of the angular distributions of quasifission fragments. The model is able to describe experimental anisotropy of the angular distributions of fissionlike fragments for the 32S, 28Si+208Pb reactions. It is also shown that the new model allows the description of the experimental mass-angular correlations

We have studied the spatial structure of the three dimensional large-scale pattern of the Galactic Magnetic Field using the polarization maps obtained by the WMAP satellite at 22 GHz. By using different models of the large-scale magnetic field of the Milky Way and a certain model for the cosmic rays electron distribution, we predict the expected

We present a study that links the Number Counts (NCs) to the rest-frame luminosity functions (LFs) at the passbands probed by the observed K-band at different epochs. Making use of a large K-band selected sample in the Groth Field, HDFN and CDFS ( ˜ 0. 27 deg2), we have derived highly reliable photometric redshift estimates that allow us to