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The "metallicity"—or proportion of heavy elements in stars, for instance, seems to increase with stellar age.
These studies have found that velocity dispersion, rather than effective radius or dynamical mass, is the main predictor of a galaxy's stellar age and metallicity.
Rotation can provide a reliable determinant of stellar age if it can be properly calibrated, in particular across a range of stellar masses.
The astrospheric absorption provides a way to empirically estimate the mass loss rates of solar-like stars, leading to the first empirical estimates of how solar-like winds vary with stellar age and activity.
The scientists found that the average field increases with the stellar rotation rate and decreases with stellar age, and that its strength correlates with emission from the stars' hot outer layers, their chromospheres.
On the early Earth, high-energy solar radiation that reached the surface was higher than today, due to the increased rotation of young solar-type stars (which slows down with stellar age) and also the lack of UV-absorbing ozone in the atmosphere (which is produced from atmospheric oxygen).
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Perhaps these stellar ages are wrong.
They find a well-defined relationship between rotation period and stellar mass, and make the case that stellar ages can now be determined with a precision of order 10% for large numbers of cool Galactic field stars.
Independent estimates of stellar ages have yielded values less than this, as would be expected, but other estimates, based on supernova distance measurements, have arrived at values of about 15 billion years, still consistent, within the errors.
The sometimes discrepant results illustrate the difficulties in a reliable determination of stellar ages.
Besides the age-rotation relation stellar ages can be inferred from memberships in moving groups or stellar clusters, isochrones, chromo-spheric activity (CaII HK indices), and astroseismology (e.g., Soderblom, 2010).
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