556 research outputs found
Otra tertulia de Navidad
Copia digital. Valladolid : Junta de Castilla y León. Consejería de Cultura y Turismo, 2009-2010Contiene: No hay posada ; Eleazar / (J. M. Saj). Los deseo
VLT-UVES abundance analysis of four giants in NGC 6553
Metal-rich globular clusters trace the formation of bulges. Abundance ratios
in the metal-rich globular clusters such as NGC 6553 can constrain the
formation timescale of the Galactic bulge. The purpose of this study is
determine the metallicity and elemental ratios in individual stars of the
metal-rich bulge globular cluster NGC 6553. A detailed abundance analysis of
four giants in NGC 6553 is carried out, based on optical high-resolution
echelle spectra obtained with UVES at the ESO VLT-UT2 Kueyen telescope. A
metallicity [Fe/H]= -0.20 dex is derived, together with -element
enhancement of Mg and Si ([Mg/Fe]=+0.28, [Si/Fe]=+0.21), solar Ca and Ti
([Ca/Fe]=+0.05, [Ti/Fe]=-0.01), and a mild enhancement of the r-process element
Eu with [Eu/Fe] = +0.10. A mean heliocentric radial velocity of -1.86 km
s is measured. We compare our results with previous investigations of
the cluster.Comment: 15 pages, 8 figures, A&A, in pres
OBSERVACIONES PRELIMINARES SOBRE LA ECOLOGIA DE Speothos venaticus (CANIDAE: CARNIVORA) EN SU HABITAT NATURAL
Se presenta información sobre el tamaño, composición, componentes alimenticios y posibles depredadores de Speothos venaticus. También se incluye una breve descripción del hábitat y aspectos del comportamiento, así como de las interrelaciones del uso de "carne de monte" con el hombre
The radius and mass of the close solar twin 18 Sco derived from asteroseismology and interferometry
The growing interest in solar twins is motivated by the possibility of
comparing them directly to the Sun. To carry on this kind of analysis, we need
to know their physical characteristics with precision. Our first objective is
to use asteroseismology and interferometry on the brightest of them: 18 Sco. We
observed the star during 12 nights with HARPS for seismology and used the PAVO
beam-combiner at CHARA for interferometry. An average large frequency
separation Hz and angular and linear radiuses of mas and R were estimated. We used these
values to derive the mass of the star, M.Comment: 5 pages, 5 figure
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