Integrative Studies 410 Our Place in the Universe
... • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
... • core continues to cool and contract • Size ~ Earth • Density: a million times that of Earth – 1 cubic cm has 1000 kg of mass! ...
Mr - White Plains Public Schools
... diagram, a star like Earth’s Sun will eventually (1) explode in a supernova (2) become a black hole (3) change to a white dwarf (4) become a neutron star 2. Stars like Earth’s Sun most likely formed directly from a (1) nebula (2) supernova (3) red giant (4) black dwarf 3. According to the diagram, t ...
... diagram, a star like Earth’s Sun will eventually (1) explode in a supernova (2) become a black hole (3) change to a white dwarf (4) become a neutron star 2. Stars like Earth’s Sun most likely formed directly from a (1) nebula (2) supernova (3) red giant (4) black dwarf 3. According to the diagram, t ...
Linking Asteroids and Meteorites through Reflectance
... • These lumps tend to condense into stars • That is why stars tend to be found in clusters ...
... • These lumps tend to condense into stars • That is why stars tend to be found in clusters ...
What stars do Summary: Nuclear burning in stars •
... Pauli exclusion principle cannot have two electrons in same place with exactly same energy. ...
... Pauli exclusion principle cannot have two electrons in same place with exactly same energy. ...
Handout 30
... transfers energy into a thin shell of hydrogen surrounding the core. As it gets hotter the outer hydrogen shell will emit more energy causing the star to expand to be a giant. ...
... transfers energy into a thin shell of hydrogen surrounding the core. As it gets hotter the outer hydrogen shell will emit more energy causing the star to expand to be a giant. ...
Life Cycle of a Star notes
... complex life cycle – they are created, live extremely long lives and then expire. By studying different stars in various stages of development, astronomers have now established a detailed process for their life cycle. ...
... complex life cycle – they are created, live extremely long lives and then expire. By studying different stars in various stages of development, astronomers have now established a detailed process for their life cycle. ...
Star Life Cycle Powerpoin
... Supergiant: Massive stars become larger than giants as they leave the main sequence….they can be 100 to 1,000 times larger than the sun. Supernova: the explosion of a supergiant ...
... Supergiant: Massive stars become larger than giants as they leave the main sequence….they can be 100 to 1,000 times larger than the sun. Supernova: the explosion of a supergiant ...
White Dwarf Stars - University of California Observatories
... Neutron Stars • Neutron stars are stellar cores that are more massive than the Chandrasekhar limit (1.44 M☼). • They are held up against their own intense gravity by the tendency for neutrons to be incompressible (neutron degeneracy pressure). • Their gravity is too strong to be supported by electr ...
... Neutron Stars • Neutron stars are stellar cores that are more massive than the Chandrasekhar limit (1.44 M☼). • They are held up against their own intense gravity by the tendency for neutrons to be incompressible (neutron degeneracy pressure). • Their gravity is too strong to be supported by electr ...
Stellar Evolution
... • Stars on the main sequence fuse hydrogen in their core to produce thermal pressure. • Longest phase of a star’s life. ...
... • Stars on the main sequence fuse hydrogen in their core to produce thermal pressure. • Longest phase of a star’s life. ...
What is a Star? - Lisle CUSD 202
... explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. ...
... explosion called a supernova. In a supernova, a massive shockwave is produced that blows away the outer layers of the star. ...
The Death of Stars
... • The Sun will become a carbon/oxygen white dwarf with a mass of 0.6Msun. • Stars up to 8Msun become carbon/oxygen white dwarfs with masses up to ~1.1Msun. • Stars below 0.45Msun aren’t massive enough to burn helium in their core and become helium white dwarfs. • Stars with masses from 8-10Msun have ...
... • The Sun will become a carbon/oxygen white dwarf with a mass of 0.6Msun. • Stars up to 8Msun become carbon/oxygen white dwarfs with masses up to ~1.1Msun. • Stars below 0.45Msun aren’t massive enough to burn helium in their core and become helium white dwarfs. • Stars with masses from 8-10Msun have ...
presentation source
... • Star swells to a cool, extended Red Giant. – 3000K, Radius ~ 1 AU. GENS4001 1999-X1 ...
... • Star swells to a cool, extended Red Giant. – 3000K, Radius ~ 1 AU. GENS4001 1999-X1 ...
LIfe of a Star
... Red giant star that expands and cools once it loses all its hydrogen Center shrinks and atmosphere grows large and cools ...
... Red giant star that expands and cools once it loses all its hydrogen Center shrinks and atmosphere grows large and cools ...
stellar_explosions - UT Austin (Astronomy)
... means of an illustration shown below. You should be able to talk your way through this diagram and it should take at least half an hour. Remember that all stars less massive than about 8 Mo go through these phases (except not the helium flash above about 2 Mo). What is the major reason why the advan ...
... means of an illustration shown below. You should be able to talk your way through this diagram and it should take at least half an hour. Remember that all stars less massive than about 8 Mo go through these phases (except not the helium flash above about 2 Mo). What is the major reason why the advan ...
Life Cycle of Star Flipbook
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
... 6. What is going to happen to our Sun’s magnitude and temperature when it goes to its next stage? 7. What is the final stage of our Sun’s life? 8. What will happen to our Sun’s magnitude and temperature when it goes to its final stage? 9. What determines which star will go supernova? 10. What two fo ...
Linking Asteroids and Meteorites through Reflectance Spectroscopy
... • The temperatures of high-mass stars in its latestage of life can reach temperatures above 600 million Kelvin • Can fuse Carbon and heavier elements • Helium Capture can also occur where Helium can be fused into heavy elements ...
... • The temperatures of high-mass stars in its latestage of life can reach temperatures above 600 million Kelvin • Can fuse Carbon and heavier elements • Helium Capture can also occur where Helium can be fused into heavy elements ...
Homework 5
... 1. What is a stellar association, how big are they, how many stars do they contain, how long do they last? Finally, what is their fate? ...
... 1. What is a stellar association, how big are they, how many stars do they contain, how long do they last? Finally, what is their fate? ...
Integrative Studies 410 Our Place in the Universe
... determine the rate of energy release, and thus rate of fuel consumption • Given the mass (amount of fuel to burn) we can obtain the lifetime • Large hot blue stars: ~ 20 million years • The Sun: 10 billion years • Small cool red dwarfs: trillions of years ...
... determine the rate of energy release, and thus rate of fuel consumption • Given the mass (amount of fuel to burn) we can obtain the lifetime • Large hot blue stars: ~ 20 million years • The Sun: 10 billion years • Small cool red dwarfs: trillions of years ...
Linking Asteroids and Meteorites through Reflectance
... • Temperatures like 10-30 K • Denser than surrounding regions ...
... • Temperatures like 10-30 K • Denser than surrounding regions ...
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.