well it depends on how fat you are.
well it depends on how fat you are.
Anywhere between a few millions and trillions of years, depending mainly on the star's mass.
MASS
The mass of a star affects its location and lifespan on the Hertzsprung-Russell diagram. Generally, more massive stars are hotter, brighter, and have shorter lifespans, while less massive stars are cooler, dimmer, and have longer lifespans. The relationship between mass and time on the diagram is intricately linked to the star's fusion processes and how it evolves over its lifetime.
The lifespan of a star is inversely related to its mass; more massive stars burn through their nuclear fuel much more quickly than less massive ones. While a small star like a red dwarf can live for tens to hundreds of billions of years, a massive star may only last a few million years before exhausting its fuel and undergoing supernova. This relationship is largely due to the rate of nuclear fusion occurring in the star's core, which increases with mass. Thus, heavier stars have shorter lifespans, while lighter stars can exist for much longer periods.
Juvenile star is typically classified as a low mass star, as it is in the early stage of its life cycle. These stars have a mass similar to that of the Sun or less. They are characterized by their long lifespan and relatively stable nature.
The life expectancy of a star (E) depends on its mass (M), roughly following the model of E = M-2.5. For a star with a mass twice that of our sun (enter 2 in place of `M`), then the lifespan will give 0.177. Our suns lifespan is around 10 billion years, so this would equate to 1.77 billion years.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
Yes, there is a relationship between the mass of a planet and its distance from its star. Heavier planets tend to form farther away from their star, while lighter planets form closer. This is due to the way planetary material condenses and accumulates in different parts of a developing solar system.
Main sequence stars best obey the mass-luminosity relation. This empirical relation states that there is a direct relationship between a star's mass and its luminosity. In general, the more massive a main sequence star is, the more luminous it will be.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.
The mass could either be a red giant or a super giant, they both evolve into different ways, after a star runs out of fuel, it becomes a white dwarf, a neutron star, or a black hole.