Vittorio Castellani

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We use evolutionary calculations presented in a recent paper (Cassisi et al. 1997a: hereinafter Paper I) to predict B, V , I magnitudes for stars in galactic glob-ulars. The eeect of the adopted mixing length on stellar magnitudes and colors is discussed, showing that the uncertainty on such a theoretical parameter prevents the use of MS stars as bona de(More)
This paper present new evolutionary computations extending toward the lower main sequence previous computations given for globular cluster stars. We discuss the physical inputs with particular regard to the limit of the adopted usual treatment of the stellar atmosphere, which allows a tight correlation with actual stellar structures only for selected range(More)
Theoretical expectations concerning stars as neutrino sources are presented according to detailed evaluations of the stellar evolutionary histories for an extended grid of stellar masses. Neutrino fluxes and cumulative neutrino yields are given for both ‘thermo-nuclear’ and ‘cooling’ neutrinos all over the nuclear life of the stars and along the final(More)
After a short survey of the physics of solar neutrinos, giving an overview of hydrogen burning reactions, predictions of standard solar models and results of solar neutrino experiments, we discuss the solar-model-independent indications in favour of non-standard neutrino properties. The experimental results look to be in contradiction with each other, even(More)
We present a theoretical approach to infer information about RR Lyrae variables from the morphology of their light curves. The method, already successfully applied to the field first overtone variable U Comae, is now tested on a RR ab variable in the globular cluster ω Cen. We show that, with this method, it could be possible to give an estimate of the(More)
We make use of a previous well tested Galactic model, but describing the observational behavior of the various stellar components in terms of suitable assumptions on their evolutionary status. In this way we are able to predict the expected distribution of Galactic White Dwarfs (WDs), with results which appear in rather good agreement with recent estimates(More)
We use evolutionary calculations presented in a recent paper (Cassisi et al. 1997a: hereinafter Paper I) to predict B,V,I magnitudes for stars in galactic globulars. The effect of the adopted mixing length on stellar magnitudes and colors is discussed, showing that the uncertainty on such a theoretical parameter prevents the use of MS stars as bona fide(More)