Metallicity

Stars with a higher metallicity than the Sun are more likely to have planets, especially giant planets, than stars with lower metallicity. citation Some planets orbit one member of a binary star system, Schwarz, Richard.

A star's metallicity can influence the time the star takes to burn its fuel, and controls the formation of its magnetic fields, citation which affects the strength of its stellar wind.

At moderate to high metallicity, stars near the upper end of that mass range will have lost most of their hydrogen when core collapse occurs and the result will be a Type II-L supernova.

Extremely luminous stars at near solar metallicity will lose all their hydrogen before they reach core collapse and so will not form a type II supernova.

However, Cepheids appear to suffer from a metallicity effect, where Cepheids of different metallicities have different period–luminosity relations.

Low metallicity red dwarfs, however, are rare.

Stars with an initial mass up to about 90 times the sun, or a little less at high metallicity, are expected to result in a type II-P supernova which is the most commonly observed type.

The clusters share other characteristics with globular clusters such as stellar populations and metallicity.

The metallicity is the proportion of elements other than hydrogen or helium, as compared to the Sun.

The metallicity of Vega's photosphere is only about 32% of the abundance of heavy elements in the Sun's atmosphere.

The rate of mass loss for luminous stars depends on the metallicity and luminosity.

Therefore, in today's photosphere the helium fraction is reduced, and the metallicity is only 84% of what it was in the protostellar phase (before nuclear fusion in the core started).

To narrow down the origin of these clouds, a better understanding of their distances and metallicity is needed.

Type Ib/c and II-L, and possibly most type IIn, supernovae are only thought to be produced from stars having near-solar metallicity levels that result in high mass loss from massive stars, hence they are less common in older more distant galaxies.

While it passed through the red giant stage, Sirius B may have enriched the metallicity of its companion.