The FT-IR spectra of the fullerenes C60 and C70 have been recorded in the temperature range between 523 K (+250 degrees C) and 93 K (-180 degrees C). As a general rule, it has been observed a shift of the infrared absorption bands toward higher frequencies at lower temperatures. As expected, at 93 K the infrared spectra appear better resolved with

Light elements are important tracers of the internal stellar structure and kinematics. Li and Be are both burned in the stellar interiors but Be requires much higher temperatures and thus we can expect to measure Be abundances in stars which have no detectable Li in their atmospheres. The study of these elements can give us information about

Not Available

Not Available

Recent observational work by Israelian et al. has shown that sun-like planet host stars in the temperature range 700 K Teff 5850 K have lithium abundances that are significantly lower than those observed for “single” field stars. In this letter we use stellar evolutionary models to show that differences in stellar mass and age are not responsible

We have computed seismic images of magnetic activity on the far surface of the Sun by using a seismic-holography technique. As in previous works, the method is based on the comparison of waves going in and out of a particular point in the Sun, but we have computed here Green's functions from a spherical polar expansion of the adiabatic wave