Life Cycle of a Star
... Step Five Stars bigger than our sun will collapse so quickly they explode into a __________________. The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its ...
... Step Five Stars bigger than our sun will collapse so quickly they explode into a __________________. The core that is leftover after a supernova may form a ______________ star. If the leftover core was above a certain mass, it will continue to collapse in on itself and form a _______ _________. Its ...
On my webpage, find the link Star Life Cycle and use it to answer the
... Click the “brown dwarf” link in Option 1 6. How many solar masses are brown dwarfs on average? ...
... Click the “brown dwarf” link in Option 1 6. How many solar masses are brown dwarfs on average? ...
Star Game Cards
... In the cores of extremely hot red giants, nuclear reactions fuse elements down to ____ on the periodic table. ...
... In the cores of extremely hot red giants, nuclear reactions fuse elements down to ____ on the periodic table. ...
Document
... The Main Sequence • A star is a delicate balance between the force of gravity pulling in, and pressure pushing out. • Stars on the main ...
... The Main Sequence • A star is a delicate balance between the force of gravity pulling in, and pressure pushing out. • Stars on the main ...
Lesson 3 Power Notes Outline
... Giant stars shine brightly because of their large surface areas. ...
... Giant stars shine brightly because of their large surface areas. ...
Stellar Evolution II
... Larger clouds of gas (GMCs) tend to fragment into smaller ones before collapsing to form stars – very massive stars are rare • Stars with masses above 50 MSUN are unstable – nuclear reactions in their core produce energy at such a fast rate that they blow off their outer layers, losing mass. ...
... Larger clouds of gas (GMCs) tend to fragment into smaller ones before collapsing to form stars – very massive stars are rare • Stars with masses above 50 MSUN are unstable – nuclear reactions in their core produce energy at such a fast rate that they blow off their outer layers, losing mass. ...
Death of sun
... A white dwarf star forms at the center of a planetary nebula. White dwarfs are very hot because they have been condensed into a very small area, about the size of the Earth. This heating process is adiabatic heating. ...
... A white dwarf star forms at the center of a planetary nebula. White dwarfs are very hot because they have been condensed into a very small area, about the size of the Earth. This heating process is adiabatic heating. ...
Stellar Evolution
... small, but extremely dense, object that remains is called a black hole because its gravity is so immense ...
... small, but extremely dense, object that remains is called a black hole because its gravity is so immense ...
Chapter 28 Vocabulary
... Astronomical Unit – the average distance between Earth and the sun, about 150 million kilometers. ...
... Astronomical Unit – the average distance between Earth and the sun, about 150 million kilometers. ...
Chapter 15 (Star Lives)
... A. They have different spectral classes. B. They have different luminosity classes. C. They have different masses. D. We can directly see them evolve. 5. Which of these is NOT a major difference between the evolution of a one and a five solar mass star? A. The more massive star has a shorter lifetim ...
... A. They have different spectral classes. B. They have different luminosity classes. C. They have different masses. D. We can directly see them evolve. 5. Which of these is NOT a major difference between the evolution of a one and a five solar mass star? A. The more massive star has a shorter lifetim ...
The Life Cycles of Stars
... blown away to form a ring around the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage ...
... blown away to form a ring around the core. This ring is called a planetary nebula. When the last of the helium atoms in the core are fused into carbon atoms, the medium size star begins to die. Gravity causes the last of the star’s matter to collapse inward and compact. This is the white dwarf stage ...
The Hertzsprung-Russell Diagram
... Another Exception to the Rule • Some stars are very hot and shine intensely but are small so they don’t radiate much energy (appear dim) white dwarf stars ...
... Another Exception to the Rule • Some stars are very hot and shine intensely but are small so they don’t radiate much energy (appear dim) white dwarf stars ...
Life Cycle of the Stars
... • How a star ends its life depends on its mass or how much matter it was born with. • Low and medium mass stars will end up as white dwarfs. • Stars that started with a lot of mass may end their lives as black holes or neutron stars. ...
... • How a star ends its life depends on its mass or how much matter it was born with. • Low and medium mass stars will end up as white dwarfs. • Stars that started with a lot of mass may end their lives as black holes or neutron stars. ...
Document
... – We observe stars at various stages of evolution, and can piece together a description of the evolution of stars in general – Computer models provide a “fast-forward” look at the evolution of stars. ...
... – We observe stars at various stages of evolution, and can piece together a description of the evolution of stars in general – Computer models provide a “fast-forward” look at the evolution of stars. ...
Recap: High Mass Stars
... • 90% of stars spend life here • Nuclear fusion = Hydrogen into Helium • Mass of star determines location on main sequence • Ranges in size from ½ Sun to 20 times the Sun’s size • Color depends on the surface temperature ...
... • 90% of stars spend life here • Nuclear fusion = Hydrogen into Helium • Mass of star determines location on main sequence • Ranges in size from ½ Sun to 20 times the Sun’s size • Color depends on the surface temperature ...
Neutron star - SharpSchool
... large stars, so they have much longer lives Small stars can live up to 200 billion years Medium stars (like the sun) can live for about ...
... large stars, so they have much longer lives Small stars can live up to 200 billion years Medium stars (like the sun) can live for about ...
Parallax
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
The Life of a Star
... together into a sphere. • The sphere becomes dense and hot. • Nuclear fusion changes hydrogen to helium. ...
... together into a sphere. • The sphere becomes dense and hot. • Nuclear fusion changes hydrogen to helium. ...
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.