How does the lifecycle of a low-mass star differ from a high-mass star?

The lifecycle of a low-mass star differs from a high-mass star due to their varying internal processes.

Low-mass stars, like our Sun, begin as a cloud of gas and dust that collapses under its own gravity. As the core temperature reaches 15 million degrees Celsius, hydrogen fusion begins, and the star enters the main sequence phase. This phase lasts for billions of years, during which the star fuses hydrogen into helium in its core. As the hydrogen supply dwindles, the star expands into a red giant, fusing helium into heavier elements. Eventually, the outer layers are expelled, and the core becomes a white dwarf.

High-mass stars, on the other hand, undergo a more violent lifecycle. They begin in the same way as low-mass stars, but their greater mass causes them to burn through their fuel much faster. They also have higher core temperatures, allowing them to fuse heavier elements. As the star runs out of fuel, it undergoes a series of explosive reactions, creating heavier and heavier elements until it reaches iron. At this point, the star collapses in on itself, creating a supernova explosion. The core may then become a neutron star or a black hole.

In summary, the lifecycle of a low-mass star is relatively calm and predictable, while a high-mass star undergoes violent explosions and creates heavier elements.