According to a 2005 paper by Fischer et al, this quantity for the host star is a strong predictor of whether gas giants are likely to be detectable using Doppler spectroscopy. In 2022, astronomers discovered that objects in the C-19 stellar stream had an unusually low value for this quantity. (15[2])High values of this quantity inhibit the reduction of outward pressure during pair production, (15[2])thereby preventing pair-instability supernovae. (15[1])Population (*) II stars (10[1])located (10[1])at the halos of (10[1])spiral galaxies are low in this (10[1])quantity, (10[2])while (10[1])Population III stars (10[1]-5[1])have values (10[1])of this quantity near zero. (10[2])This quantity is denoted Z in the equation “X plus Y plus Z equals 1,” (10[1])where X and Y represent the abundances of the two (10[1])lightest (10[1])elements. (10[2]-5[2])For (10[1])10 (10[1])points, (10[1])name this quantity (10[1])which measures the proportion of elements heavier (10[1])than helium (10[1])in (10[1])a star. ■END■ (10[3]0[4])