29.3 – Stellar Evolution
... •No energy left for fusion •Loses its outer shell, revealing core •Core heats and illuminates expanding gases = planetary nebula •Gravity causes star to collapse inward •Hot, dense core of matter = white dwarf ...
... •No energy left for fusion •Loses its outer shell, revealing core •Core heats and illuminates expanding gases = planetary nebula •Gravity causes star to collapse inward •Hot, dense core of matter = white dwarf ...
Extension worksheet – Topic 6 - Cambridge Resources for the IB
... paths of these two stars with reference to a ...
... paths of these two stars with reference to a ...
Star Cycle [Recovered]
... the sun. This greater internal pressure causes fusion reactions to occur __________. This causes the largest stars to burn their quickly quickly fuel, and eventually run out, much more ______________. lives Larger stars live shorter _____________. Bigger stars are brighter and hotter due to the rapi ...
... the sun. This greater internal pressure causes fusion reactions to occur __________. This causes the largest stars to burn their quickly quickly fuel, and eventually run out, much more ______________. lives Larger stars live shorter _____________. Bigger stars are brighter and hotter due to the rapi ...
Life cycle of Stars Notes
... • White dwarfs, are the carbon and oxygen cores of dead stars. • WD are about the size of earth. • The more massive a WD is, the smaller it is in size. ...
... • White dwarfs, are the carbon and oxygen cores of dead stars. • WD are about the size of earth. • The more massive a WD is, the smaller it is in size. ...
Chapter 13 Notes – The Deaths of Stars
... Expansion to red giant during hydrogen burning ____________ phase Ignition of ___________ burning in the Helium core Formation of a _______________ and oxygen core IV. Mass Loss from Stars Stars like our sun are constantly losing mass in a ______________ wind (solar wind) The more massive ...
... Expansion to red giant during hydrogen burning ____________ phase Ignition of ___________ burning in the Helium core Formation of a _______________ and oxygen core IV. Mass Loss from Stars Stars like our sun are constantly losing mass in a ______________ wind (solar wind) The more massive ...
Ch.10 Stellar old age
... • H fusion is faster because C, N and O act as catalysts • Same net result: 4 H become 1 He. • No total gain or loss of C, N, O Question: How does energy produced by CNO cycle compare to PP chain? ...
... • H fusion is faster because C, N and O act as catalysts • Same net result: 4 H become 1 He. • No total gain or loss of C, N, O Question: How does energy produced by CNO cycle compare to PP chain? ...
THE BIRTH AND DEATH OF A LOW/MEDIUM MASS STAR
... • THE STAGE WHEN A STAR IS IN IT’S “BEST” LIFE CYCLE • OUR SUN IS A MAIN SEQUENCE STAR • MAIN SEQUENCE STARS HAVE MOSTLY HYDROGEN. • THE HYDROGEN EXPLODES, GIVING OFF LIGHT AND HEAT • AS IT EXPLODES, THE HYDROGEN TURNS TO HELIUM. • HELIUM IS LIGHTER THAN HYDROGEN. • OUR SUN IS 4.6 BILLION YEARS OLD. ...
... • THE STAGE WHEN A STAR IS IN IT’S “BEST” LIFE CYCLE • OUR SUN IS A MAIN SEQUENCE STAR • MAIN SEQUENCE STARS HAVE MOSTLY HYDROGEN. • THE HYDROGEN EXPLODES, GIVING OFF LIGHT AND HEAT • AS IT EXPLODES, THE HYDROGEN TURNS TO HELIUM. • HELIUM IS LIGHTER THAN HYDROGEN. • OUR SUN IS 4.6 BILLION YEARS OLD. ...
Slide 1
... • AGB stars are left with the stellar core surrounded by a relatively thin sphere of hot gas which looks like planetary disk, and called Planetary Nebulae (PNe) (nothing to do with planets per se) • PNe cores continue to cool and become White Dwarfs (94% stars end up as WDs) ...
... • AGB stars are left with the stellar core surrounded by a relatively thin sphere of hot gas which looks like planetary disk, and called Planetary Nebulae (PNe) (nothing to do with planets per se) • PNe cores continue to cool and become White Dwarfs (94% stars end up as WDs) ...
PowerPoint Presentation - ASTR498E High energy
... A star leaves the main sequence once it exhausts its supply of hydrogen in the core This lifetime depends upon ...
... A star leaves the main sequence once it exhausts its supply of hydrogen in the core This lifetime depends upon ...
Elements and Isotopes - University of California, Berkeley
... Hundreds to thousands of stars (and brown dwarfs). Relatively young (still containing massive stars). Found in galactic plane. May not even stay together if really young (might be dispersing). Light dominated by hot stars. ...
... Hundreds to thousands of stars (and brown dwarfs). Relatively young (still containing massive stars). Found in galactic plane. May not even stay together if really young (might be dispersing). Light dominated by hot stars. ...
80.BrainPopLifeCycleStars
... 1. Stars __________ throughout their lives just like we do; only they live for ___________ of years. 2. They start out as clouds of gas and dust called __________ nurseries. The force of __________ within these clouds slowly pulls the particles together, causing dense clumps to form. 3. If the clump ...
... 1. Stars __________ throughout their lives just like we do; only they live for ___________ of years. 2. They start out as clouds of gas and dust called __________ nurseries. The force of __________ within these clouds slowly pulls the particles together, causing dense clumps to form. 3. If the clump ...
main sequence star
... • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainter. • When there is no more energy being emitted (released), they are called ...
... • The outer gases are lost, which allows us to see the core of the star. The white dwarf is very dense and hot. The emit (release) less light than they did when they were stars. • As these white dwarfs cool they become fainter. • When there is no more energy being emitted (released), they are called ...
Fusion in the Sun
... 1. Nebula cloud- gas and dust particles held together by gravity. 2. Gravity crushes the center of the cloud until fusion begins and the cloud ignites. 3. Main Sequence- hydrogen atoms fuse into helium atoms in the core of the star 4. Red Giant- hydrogen atoms are almost gone, the outer shell of gas ...
... 1. Nebula cloud- gas and dust particles held together by gravity. 2. Gravity crushes the center of the cloud until fusion begins and the cloud ignites. 3. Main Sequence- hydrogen atoms fuse into helium atoms in the core of the star 4. Red Giant- hydrogen atoms are almost gone, the outer shell of gas ...
Red Giants
... core shrinks. The layers outside the core collapse too, the ones closer to the center collapse quicker than the ones near the surface. As the layers collapses, the gas compresses and heats up. Eventually, the layer just outside the core called the ``shell layer'' gets hot and dense enough for fusion ...
... core shrinks. The layers outside the core collapse too, the ones closer to the center collapse quicker than the ones near the surface. As the layers collapses, the gas compresses and heats up. Eventually, the layer just outside the core called the ``shell layer'' gets hot and dense enough for fusion ...
Physical properties of stars
... The size ranges from stars approximately 10 km across to stars that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widel ...
... The size ranges from stars approximately 10 km across to stars that are 1,000 times larger than our sun. pg. 450 Temperature: Surface temperatures range from 3000K to 30,000K Color is an indication of temperature. Blue hottest White Yellow Orange Red coolest Mass While the size of stars varies widel ...
Supernova
... Stellar Explosion • When gravitational force exceeds the electron repulsion, the core collapses immediately. – Energy in photons and neutrinos ...
... Stellar Explosion • When gravitational force exceeds the electron repulsion, the core collapses immediately. – Energy in photons and neutrinos ...
Use this form to take notes in class about stars
... Stars of Spectral Classes B to M 9. What color is our sun? ___________what class is it in? ...
... Stars of Spectral Classes B to M 9. What color is our sun? ___________what class is it in? ...
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.