Stellar Evolution
... It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
... It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
Stellar Evolution
... It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
... It glows with infrared light generated from its gravitational contraction like Jupiter does. They don’t “evolve” but stay brown dwarfs and slowly fade over 100s of billions of years ...
the life cycle of stars
... • After a sun-like star forms, it enters the main-sequence. • This is the second and longest stage of its life. • Energy is generated in the core and causes the star to shine. • The size of the star changes very little as long as its supply of hydrogen nuclei fuse into helium nuclei. ...
... • After a sun-like star forms, it enters the main-sequence. • This is the second and longest stage of its life. • Energy is generated in the core and causes the star to shine. • The size of the star changes very little as long as its supply of hydrogen nuclei fuse into helium nuclei. ...
Stellar Evolution
... nebula’s dust and gas into a denser cloud • As a nebula heats up, it contracts • A contracting cloud of dust with enough mass to form a star ...
... nebula’s dust and gas into a denser cloud • As a nebula heats up, it contracts • A contracting cloud of dust with enough mass to form a star ...
How the Universe Works Extreme Stars Name 1. When a star dies
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
... How the Universe Works Extreme Stars Name _______________ 1. When a star dies (gravity) (fusion) wins out. 2. The sun will run out of fuel in about (3) (7) (10) billion years. 3. When the sun runs out of hydrogen fuel, it will become a (red giant) (neutron star) (black hole). 4. Eventually, the heli ...
The Evolutionary Cycle of Stars
... NEBULA(e) that contains gas & dust from the beginnings of a star. Cosmic cloud of gas & dust, basic building blocks of the universe, & the largest objects in the universe. Temperatures rise, driven by gravitational collapse, and a PROTOSTAR forms. It is the early stage in star formation. The star ev ...
... NEBULA(e) that contains gas & dust from the beginnings of a star. Cosmic cloud of gas & dust, basic building blocks of the universe, & the largest objects in the universe. Temperatures rise, driven by gravitational collapse, and a PROTOSTAR forms. It is the early stage in star formation. The star ev ...
Foundation 1 - Discovering Astronomy
... The end states of stars depends upon its mass! The more massive a star, the faster it consumes its fuel, the shorter its lifetime ...
... The end states of stars depends upon its mass! The more massive a star, the faster it consumes its fuel, the shorter its lifetime ...
The Sun Compared to Other Stars
... Core continues to collapse, outer shell expands because of hydrogen fusion, star becomes luminous Core becomes degenerate (sustained by electron pressure), outer shell dumps helium ash onto core Helium flash! Helium fusion (into carbon) begins in core Core helium fusion ends, eventually leading to b ...
... Core continues to collapse, outer shell expands because of hydrogen fusion, star becomes luminous Core becomes degenerate (sustained by electron pressure), outer shell dumps helium ash onto core Helium flash! Helium fusion (into carbon) begins in core Core helium fusion ends, eventually leading to b ...
Lecture 16 - Yet More Evolution of Stars
... variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
... variety of different masses • Using what we know about stellar evolution is there a way to determine the age of the star cluster? ...
Life Cycles of Stars
... The outer layers of gas are ejected while the star's core contracts into a white dwarf. ...
... The outer layers of gas are ejected while the star's core contracts into a white dwarf. ...
PowerPoint File
... through the star, throwing off the outer layers of the star into space. As the outer layers are peeled back, it reveals the extremely hot, ultraviolet-emitting carbon and oxygen core which ionizes the stellar wind ...
... through the star, throwing off the outer layers of the star into space. As the outer layers are peeled back, it reveals the extremely hot, ultraviolet-emitting carbon and oxygen core which ionizes the stellar wind ...
File
... 8-25 X larger than our Sun Consume their fuel very fast – die more quickly and more violently Star expands into a Supergiant which causes the core to collapse and the outer portion to explode creating a Supernova then a Neutron Star ...
... 8-25 X larger than our Sun Consume their fuel very fast – die more quickly and more violently Star expands into a Supergiant which causes the core to collapse and the outer portion to explode creating a Supernova then a Neutron Star ...
Life Cycle of Stars: Chapter 21
... • Becomes a red giant as hydrogen is depleted • Expands and collapses to facilitate helium burning – Becomes helium burning star ...
... • Becomes a red giant as hydrogen is depleted • Expands and collapses to facilitate helium burning – Becomes helium burning star ...
Stellar evolution
Stellar evolution is the process by which a star changes during its lifetime. Depending on the mass of the star, this lifetime ranges 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.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.