The Solar System
... systems), outflows and jets. • Disperse their cocoon to become visible. • Typically form in clusters, dominated by light from 1–2 brightest members. GENS4001 Astronomy ...
... systems), outflows and jets. • Disperse their cocoon to become visible. • Typically form in clusters, dominated by light from 1–2 brightest members. GENS4001 Astronomy ...
Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... no more than 8 Solar masses • White Dwarfs can be no more than 1.4 Solar masses and have diameters about the size of the Earth (1/100 the diameter of the Sun). • If a White Dwarf is in a binary system and close enough to its companion A White Dwarf pulling material star it may draw material off off ...
... no more than 8 Solar masses • White Dwarfs can be no more than 1.4 Solar masses and have diameters about the size of the Earth (1/100 the diameter of the Sun). • If a White Dwarf is in a binary system and close enough to its companion A White Dwarf pulling material star it may draw material off off ...
Folie 1
... Evolution of Intermediate Mass Stars He burning occurs in a convective core (inner part of the larger He core). The composition of the inner core is constantly mixed and turns gradually from He to C and O. When He is depleted, convection is quenched. • Once the star has converted all its He to C, i ...
... Evolution of Intermediate Mass Stars He burning occurs in a convective core (inner part of the larger He core). The composition of the inner core is constantly mixed and turns gradually from He to C and O. When He is depleted, convection is quenched. • Once the star has converted all its He to C, i ...
Astronomy
... The mass of a star determines how quickly fusion will occur and therefore how long the star will “live”. ...
... The mass of a star determines how quickly fusion will occur and therefore how long the star will “live”. ...
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! ...
Stars are classified according to their color
... • Stars are classified according to their color temperature: ...
... • Stars are classified according to their color temperature: ...
The Life Cycle of Stars Introduction Stars are huge spheres of very
... Fusion takes place in the core. Fusion combines the nuclei of hydrogen atoms into helium nuclei. When hydrogen nuclei collide, they fuse to form deuterons, which have one proton and one neutron. Another proton collides with a deuteron to form a helium isotope. Each time that two particles fuse, ener ...
... Fusion takes place in the core. Fusion combines the nuclei of hydrogen atoms into helium nuclei. When hydrogen nuclei collide, they fuse to form deuterons, which have one proton and one neutron. Another proton collides with a deuteron to form a helium isotope. Each time that two particles fuse, ener ...
大爆炸---宇宙的起源
... body thermal energy coming from all parts of the sky. The radiation is isotropic to roughly one part in 100,000. As the universe expanded, adiabatic cooling caused the plasma to lose energy until it became favorable for electrons to combine with protons, forming hydrogen atoms. This recombination ev ...
... body thermal energy coming from all parts of the sky. The radiation is isotropic to roughly one part in 100,000. As the universe expanded, adiabatic cooling caused the plasma to lose energy until it became favorable for electrons to combine with protons, forming hydrogen atoms. This recombination ev ...
MBuzaTalk2
... Normal stars are fighting with Hydrodynamic pressure, and radiation pressure. But in by-products we see both electron and neutron degeneracy’s, along with neutrino pressures. Where density is the dominating factor. Mainly, White Dwarfs, Neutron Stars, and Black holes. ...
... Normal stars are fighting with Hydrodynamic pressure, and radiation pressure. But in by-products we see both electron and neutron degeneracy’s, along with neutrino pressures. Where density is the dominating factor. Mainly, White Dwarfs, Neutron Stars, and Black holes. ...
Section 25.2 Stellar Evolution
... When the core of a protostar has reached about 10 million K, pressure within is so great that nuclear fusion of hydrogen begins, and a star is born. Nebula ...
... When the core of a protostar has reached about 10 million K, pressure within is so great that nuclear fusion of hydrogen begins, and a star is born. Nebula ...
Ch. 11 and 12 Study Guide (ANSWERS)
... of the nebula to clump together. As particles begin clumping together, they move faster and become hotter. As the clump contracts even more, it begins to take the shape of a sphere and gets even hotter. That spherical mass begins to spin and become a disk, which is hottest at its center. Then, the t ...
... of the nebula to clump together. As particles begin clumping together, they move faster and become hotter. As the clump contracts even more, it begins to take the shape of a sphere and gets even hotter. That spherical mass begins to spin and become a disk, which is hottest at its center. Then, the t ...
Talk
... carbon and oxygen in a degenerate-electron sea. Stars with masses d 4 MŸ cannot generate the temperate and pressure needed for fusion beyond helium. These are White Dwarf stars, and in most cases this is nearly the end of their evolution. ...
... carbon and oxygen in a degenerate-electron sea. Stars with masses d 4 MŸ cannot generate the temperate and pressure needed for fusion beyond helium. These are White Dwarf stars, and in most cases this is nearly the end of their evolution. ...
投影片 1
... It represents the end state of stellar evolution of stars like the Sun Its progenitor had an original mass about seven times the Sun’s From the death of GD362,it passed two to five billion years based on the cooling rate ...
... It represents the end state of stellar evolution of stars like the Sun Its progenitor had an original mass about seven times the Sun’s From the death of GD362,it passed two to five billion years based on the cooling rate ...
The Life of a Star
... star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. This leaves behind either a neutron star ...
... star 10 times the Sun’s mass. Low-mass stars cool down and swell up into a red giant. Outer layers drift away and the star shrinks to become a white dwarf which will cool and fade away. High-mass stars swells into a red supergiant which undergoes a supernova. This leaves behind either a neutron star ...
Stellar Evolution and the HR Diagram Study Guide
... Which star will appear brighter in the night sky, a star with an apparent magnitude of 0 or a star with an apparent magnitude of +1? Star with apparent magnitude of 0 ...
... Which star will appear brighter in the night sky, a star with an apparent magnitude of 0 or a star with an apparent magnitude of +1? Star with apparent magnitude of 0 ...
Formation of the Universe Test Review Packet
... 2. Nebula 3. Supernova 4. Pulsar 5. Main-Sequence 6. Gravity 7. Red Giant 8. Super Giant 9. White Dwarf 10. Black Hole 11. Geocentric 12. Heliocentric Concept 13. Compare and Contrast how a HIGH Mass, LOW Mass, and a AVERAGE Mass (Sun-like) star evolves through its life cycle. 14. Label the H-R diag ...
... 2. Nebula 3. Supernova 4. Pulsar 5. Main-Sequence 6. Gravity 7. Red Giant 8. Super Giant 9. White Dwarf 10. Black Hole 11. Geocentric 12. Heliocentric Concept 13. Compare and Contrast how a HIGH Mass, LOW Mass, and a AVERAGE Mass (Sun-like) star evolves through its life cycle. 14. Label the H-R diag ...
Galaxies and Stars Questions KEY
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
... Generally, stars with more mass have shorter life spans because they burn their fuel more quickly than smaller stars do. The mass also determines which direction the lifespan goes and ultimately, determines what the star becomes when it dies. 7. What is the outcome of a star that runs out of hydroge ...
Lecture Notes-PPT
... temperature rises to 5 million K Heat and gravity compete between stages 6 and 7 until core reaches about 10 million K; nuclear fusion begins. ...
... temperature rises to 5 million K Heat and gravity compete between stages 6 and 7 until core reaches about 10 million K; nuclear fusion begins. ...
Where Did the Elements Come From?
... • When very massive stars have converted almost all of the hydrogen and helium in its core into heavier elements up to iron, the star collapses, and then blows apart producing the elements heavier than iron. • This explosion is called a supernova. • The contents of the star become part of a newly fo ...
... • When very massive stars have converted almost all of the hydrogen and helium in its core into heavier elements up to iron, the star collapses, and then blows apart producing the elements heavier than iron. • This explosion is called a supernova. • The contents of the star become part of a newly fo ...
Slide 1
... As of February 2012, Kepler has revealed 2321 planets – 281 are Jupiter-sized or larger (6 REarth < R < 22 REarth); – 1118 are Neptune-sized (2 REarth < R < 6 REarth); – 676 are super-Earth (1.25 REarth < R < 2 REarth); – 246 are approximately Earth-sized (R< 1.25 REarth). – 88% are Neptune sized or ...
... As of February 2012, Kepler has revealed 2321 planets – 281 are Jupiter-sized or larger (6 REarth < R < 22 REarth); – 1118 are Neptune-sized (2 REarth < R < 6 REarth); – 676 are super-Earth (1.25 REarth < R < 2 REarth); – 246 are approximately Earth-sized (R< 1.25 REarth). – 88% are Neptune sized or ...
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.