Im no astrophysicist but an older star would consume more of its hydrogen over time in comparison to helium through its fusion process. Over time concetrations would change resulting in a higher helium to hydrogen ratio.
mostly hydrogen and helium
HydrogenAnswered By Nick Branham
Stars fuse hydrogen into helium during the main sequence. After the main sequence, helium, oxygen, silicon and carbon are fused.
hydrogen and helium plasmas. This is really helpful
25%
All of them, that's how a star gets to be "old" ... it converts its hydrogen into helium.
A star's nuclear fusion reaction converts hydrogen into helium, and generates energy through this process. A "new" star has a fairly low percentage of helium, but over the course of billions of years, it fuses the hydrogen "fuel" into helium "ash".
The sun in composed of 25 percent helium. The other 75 percent is hydrogen. The sun also has small amounts of other elements such as neon, oxygen, carbon, and magnesium.
Helium atoms.
mostly hydrogen and helium
Helium.
Cecilia Payne discovered that stars in the main sequence of development are composed almost entirely of the elements hydrogen and helium, which contradicted the current beliefs of the time.
HydrogenAnswered By Nick Branham
Stars fuse hydrogen into helium during the main sequence. After the main sequence, helium, oxygen, silicon and carbon are fused.
Jupiter is composed mainly of gases (hydrogen and helium).
Most stars - and specifically main-sequence stars - get their energy from converting hydrogen-1 to helium-4, so you would expect that the percentage of hydrogen will decrease over time, while the percentage of helium would increase over time. Please note that the rate of fusion depends a LOT on the mass of the star; so you might have a very massive star that's only a few million years old and has already burned up most of its fuel (hydrogen), and another star, a red dwarf, that's 10 billion years old and has only used a small percentage of its fuel.
There is no Oxygen on Uranus. Uranus is primarily composed of Hydrogen and Helium