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The known members of nearby young associations, with new discoveries in this paper. Quality of membership is as decided in the source paper and has not been re-evaluated here. By virtue of numbers, they will better inform the initial mass function IMF measurements of young associations, which currently appear to be very different from the field IMF Schlieder Our analysis of youth is based on absolute trigonometric parallaxes, Johnson—Kron—Cousins VRI photometry, spectral types, variability, kinematic analyses, and surface gravity estimates. Identifying young stars specifically, pre-main-sequence young stars is a complicated process.
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About Related Links 1. Yet, its effect on stellar evolution and supernova explosions, and by implication on the chemical enrichment of galaxies is of prime importance. It was realized quite some time ago that stellar rotation and the mixing it induces must play a major role in stellar evolution theory e. Ways to test the theoretical descriptions used to represent rotational mixing are scarce and are mainly limited to studies of the chemical composition and projected rotational velocity of stellar atmospheres e. A particularly strong observational diagnostic for mixing is the surface nitrogen abundance of stars that are undergoing hydrogen fusion through the carbon—nitrogen—oxygen cycle in their interior. It turns out that the current theoretical concepts of rotational mixing seemingly fail to explain observations of various massive stars in the Milky Way and in the Magellanic Clouds Hunter et al.
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About Related Links 1. Confronting theoretical predictions with empirical measurements have also identified significant offsets even for isolated field stars: The existence of a correlation between gas giant planet frequency and host-star metallicity is well established for FGK-dwarfs Gonzalez ; Santos et al. This conclusion was reinforced by the work of Bean et al.
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