Stellar evolution | Wikipedia audio article
Channel: wikipedia tts
Date: 2018-12-08

This is an audio version of the Wikipedia Article:
Stellar evolution


00:02:04 1 Birth of a star
00:02:13 1.1 Protostar
00:03:36 1.2 Brown dwarfs and sub-stellar objects
00:04:33 1.3 Main sequence
00:05:58 2 Mature stars
00:06:33 2.1 Low-mass stars
00:08:04 2.2 Mid-sized stars
00:09:07 2.2.1 Subgiant phase
00:09:58 2.2.2 Red-giant-branch phase
00:11:23 2.2.3 Horizontal branch
00:13:18 2.2.4 Asymptotic-giant-branch phase
00:15:32 2.2.5 Post-AGB
00:16:56 2.3 Massive stars
00:20:25 2.3.1 Supernova
00:23:54 3 Stellar remnants
00:24:12 3.1 White and black dwarfs
00:27:40 3.2 Neutron stars
00:29:19 3.3 Black holes
00:30:37 4 Models



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SUMMARY
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Stellar evolution is the process by which a star changes over the course of time. Depending on the mass of the star, its lifetime can range from a few million years for the most massive to trillions of years for the least massive, which is considerably longer than the age of the universe. The table shows the lifetimes of stars as a function of their masses. All stars are born from collapsing clouds of gas and dust, often called nebulae or molecular clouds. Over the course of millions of years, these protostars settle down into a state of equilibrium, becoming what is known as a main-sequence star.
Nuclear fusion powers a star for most of its life. Initially the energy is generated by the fusion of hydrogen atoms at the core of the main-sequence star. Later, as the preponderance of atoms at the core becomes helium, stars like the Sun begin to fuse hydrogen along a spherical shell surrounding the core. This process causes the star to gradually grow in size, passing through the subgiant stage until it reaches the red giant phase. Stars with at least half the mass of the Sun can also begin to generate energy through the fusion of helium at their core, whereas more-massive stars can fuse heavier elements along a series of concentric shells. Once a star like the Sun has exhausted its nuclear fuel, its core collapses into a dense white dwarf and the outer layers are expelled as a planetary nebula. Stars with around ten or more times the mass of the Sun can explode in a supernova as their inert iron cores collapse into an extremely dense neutron star or black hole. Although the universe is not old enough for any of the smallest red dwarfs to have reached the end of their lives, stellar models suggest they will slowly become brighter and hotter before running out of hydrogen fuel and becoming low-mass white dwarfs.Stellar evolution is not studied by observing the life of a single star, as most stellar changes occur too slowly to be detected, even over many centuries. Instead, astrophysicists come to understand how stars evolve by observing numerous stars at various points in their lifetime, and by simulating stellar structure using computer models.