Mass of Stars
The mass of a star determines how long a star will live. A star with a high mass consumes hydrogen much faster than a star with low mass, resulting in a shorter life cycle.
When a massive star runs out of hydrogen for fusion, it begins to fuse helium in to the carbon. The core becomes so hot that when helium is no longer available for fusion, carbon undergoes fusion. This produces heavier elements, beginning with oxygen and up to iron. Once iron is produced in the core, fusion can no longer occur.
Once fusion stops, the star collapses under its own gravity and the iron core increases in temperature. The inward rush of gas is suddenly halted by the core and the gases bounce back outward with a great force. The outer layers of the star explode outwards in what is called supernova, sending out a series of shock waves.
When a massive star runs out of hydrogen for fusion, it begins to fuse helium in to the carbon. The core becomes so hot that when helium is no longer available for fusion, carbon undergoes fusion. This produces heavier elements, beginning with oxygen and up to iron. Once iron is produced in the core, fusion can no longer occur.
Once fusion stops, the star collapses under its own gravity and the iron core increases in temperature. The inward rush of gas is suddenly halted by the core and the gases bounce back outward with a great force. The outer layers of the star explode outwards in what is called supernova, sending out a series of shock waves.
