The G-dwarf problem is the deficit of low-metallicity long-lived G dwarfs near the Sun relative to the prediction of a constant-yield closed-box model. Prolonged accretion of metal-poor gas is a standard ingredient in its resolution.
A metallicity distribution function gives the number or mass of stars per metallicity interval. Its interpretation depends on sample selection, stellar lifetimes, spatial migration, and whether metallicity means total heavy-element abundance or a particular abundance ratio.
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The G-dwarf problem is a phenomenon in astrophysics and astronomy related to the abundance of certain types of stars, specifically G-type main-sequence stars (often referred to as "G-dwarfs"). These stars are similar to our Sun and are characterized by certain characteristics, such as their temperature and luminosity. The problem arises when astronomers try to account for the number of G-dwarf stars in the Milky Way galaxy.