MAIN-SEQUENCE The average star spends 90% of its life as a hydrogen burning MS star.
On the main sequence.
The main-sequence lifetime is a phase in a star's life when it fuses hydrogen into helium in its core. This phase typically lasts about 90% of a star's total fusion lifetime. After the main sequence, a star may continue to fuse other elements, depending on its mass, which will determine the total duration of its fusion lifetime.
The Sun is located on the main sequence of the H-R diagram, which is where stars like the Sun reside for most of their lifetime. It falls in the middle of the main sequence, representing a stable phase of hydrogen fusion in its core.
stars there called stars
The hottest type of star on the Hertzsprung-Russell (H-R) diagram is typically a blue star, which falls in the top left portion of the diagram. These stars are usually massive and have high surface temperatures, leading to their blue coloration and positioning on the diagram.
On the main sequence.
On the main sequence.
No, it will spend most of it's life as a main sequence star.
The main-sequence lifetime is a phase in a star's life when it fuses hydrogen into helium in its core. This phase typically lasts about 90% of a star's total fusion lifetime. After the main sequence, a star may continue to fuse other elements, depending on its mass, which will determine the total duration of its fusion lifetime.
The Sun is located on the main sequence of the H-R diagram, which is where stars like the Sun reside for most of their lifetime. It falls in the middle of the main sequence, representing a stable phase of hydrogen fusion in its core.
Most stars, for most of their existence, fuse hydrogen into helium.
A Star spends most of its life on the "main sequence" of the Hertzsprung-Russell diagram (see related link below). While here it is called a "main sequence" star and its source of energy during this phase of its life is the fusion of hydrogen into helium in its core.
The main sequence on the Hertzsprung-Russell diagram represents the stage in a star's life when it is undergoing nuclear fusion of hydrogen into helium in its core. Stars spend the majority of their lifetime on the main sequence, where they maintain a stable balance between inward gravitational pressure and outward radiation pressure. The main sequence runs diagonally from high temperature, high luminosity stars (top left) to lower temperature, lower luminosity stars (bottom right).
When a star is at the end of its lifetime its mass increases.
The lifetime of a star varies a lot, depending on its exact mass. The lifetime of a star can be anywhere from just a few million years for the most massive stars, to trillions of years for red dwarves.
Mainly its mass. The most massive stars develop the most quickly.
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.