Homework 1
... on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the temperature to increase. Seeing as the mass of the protostar is larger it can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and tempera ...
... on the outside shell becomes larger causing it to become more dense. This increase in density in turn causes the temperature to increase. Seeing as the mass of the protostar is larger it can pull in more dust from the surrounding cloud, and this cycle continues. At some point the density and tempera ...
EMR, Telescopes, Stars, Solar System study guide `14-15
... 9. The distance that light travels in a year is known as a _________________________. 10. The time it takes light from a star 100 light years away to reach Earth is ___________________. 11. Parallax is used to find the ____________________________ to nearby stars. 12. Astronomers use a _____________ ...
... 9. The distance that light travels in a year is known as a _________________________. 10. The time it takes light from a star 100 light years away to reach Earth is ___________________. 11. Parallax is used to find the ____________________________ to nearby stars. 12. Astronomers use a _____________ ...
1. The distances to the most remote galaxies can be
... b) Have only their high mass stars on the main sequence while the low-mass protostars are still contracting (and hence are not on the main sequence yet). c) Have only their low mass stars on the main sequence while the high-mass protostars are still contracting (and hence are not on the main sequenc ...
... b) Have only their high mass stars on the main sequence while the low-mass protostars are still contracting (and hence are not on the main sequence yet). c) Have only their low mass stars on the main sequence while the high-mass protostars are still contracting (and hence are not on the main sequenc ...
Luminosity - UCF Physics
... 0.1 times as much fuel, uses it 0.01 times as fast 100 billion years ~ 10 billion years x 0.1 / 0.01 ...
... 0.1 times as much fuel, uses it 0.01 times as fast 100 billion years ~ 10 billion years x 0.1 / 0.01 ...
Evolution of a Star
... We have a theory of how stars evolve, what makes them different from one another and what happens when they die. Teachers - Stars begin as a large cloud of dust and gas called a nebula. The particles of dust and gas exert a gravitational force on each other causing the nebula to contract. As the par ...
... We have a theory of how stars evolve, what makes them different from one another and what happens when they die. Teachers - Stars begin as a large cloud of dust and gas called a nebula. The particles of dust and gas exert a gravitational force on each other causing the nebula to contract. As the par ...
GLY 1001 Earth Science Name:__Answers
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
... Red giant – A large, cool star of high luminosity, a star occupying the upper-right portion of the Hertzsprung-Russell Diagram. Reflection nebula – A relatively dense dust cloud in interstellar space that is illuminated by starlight. Spiral galaxy – A flattened, rotating galaxy with pinwheel-like ar ...
High School Science Proficiency Review #2 Earth Science
... Demonstrate the general relationship between the color and temperature of stars. E.12.B.2 Students know stars are powered by nuclear fusion of lighter elements into heavier elements, which results in the release of large ...
... Demonstrate the general relationship between the color and temperature of stars. E.12.B.2 Students know stars are powered by nuclear fusion of lighter elements into heavier elements, which results in the release of large ...
Stars, Galaxies & Universe
... most of their lives. • After all the hydrogen has been fused into helium, the star fuses helium into carbon, carbon into oxygen and then oxygen into iron. ...
... most of their lives. • After all the hydrogen has been fused into helium, the star fuses helium into carbon, carbon into oxygen and then oxygen into iron. ...
Teaching ideas for Option E, Astrophysics
... knowledge of the nuclear fusion reactions taking place inside the star or any other details about the structure of the star. All we have to assume is that the star is in equilibrium under the action of the force of gravitation that tends to collapse the star and the outward force due to the pressure ...
... knowledge of the nuclear fusion reactions taking place inside the star or any other details about the structure of the star. All we have to assume is that the star is in equilibrium under the action of the force of gravitation that tends to collapse the star and the outward force due to the pressure ...
![HR DIAGRAM[1] Star Human Comparison Are all stars the same](http://s1.studyres.com/store/data/010665051_1-e4f26b4aee29f3f3aaab891d368963d6-300x300.png)
HR DIAGRAM[1] Star Human Comparison Are all stars the same
... fuel to burn once the core of a star has been converted to iron. Iron cannot fuse and lose energy at the same time. Therefore, once the carbon is gone the temperature of the star’s core will drop. This causes the gas pressure to decrease. Then gravity has the upper hand, and the star will collapse u ...
... fuel to burn once the core of a star has been converted to iron. Iron cannot fuse and lose energy at the same time. Therefore, once the carbon is gone the temperature of the star’s core will drop. This causes the gas pressure to decrease. Then gravity has the upper hand, and the star will collapse u ...
Analyzing Spectra
... star's atmosphere. As light emitted from a star passes through the star's atmosphere, some of it is absorbed by elements in the atmosphere. The wavelengths of the light that are absorbed appear as dark lines in the spectrum. Each element absorbs certain wavelengths, producing a certain pattern of da ...
... star's atmosphere. As light emitted from a star passes through the star's atmosphere, some of it is absorbed by elements in the atmosphere. The wavelengths of the light that are absorbed appear as dark lines in the spectrum. Each element absorbs certain wavelengths, producing a certain pattern of da ...
Stars, Stellar classification, H
... H-R diagram depicts: Temperature Color Spectral Type Luminosity Radius *Mass *Lifespan ...
... H-R diagram depicts: Temperature Color Spectral Type Luminosity Radius *Mass *Lifespan ...
The IC 348 surface density in the Perseus molecular cloud L. Cambrésy Observatoire de Strasbourg, France
... Embedded clusters toward the North America Nebula ...
... Embedded clusters toward the North America Nebula ...
Stars: Part 2
... • This red giant begins to lose some of its layers. • Eventually it enters the Cepheid stage. • This is the final phase of the star's life. • It then becomes a white dwarf. • In a white dwarf, the core of the star is left, some fires still burn, but there is very little fuel left. ...
... • This red giant begins to lose some of its layers. • Eventually it enters the Cepheid stage. • This is the final phase of the star's life. • It then becomes a white dwarf. • In a white dwarf, the core of the star is left, some fires still burn, but there is very little fuel left. ...
Lecture 9: Hydrostatic Equilibrium
... Note that in most cases of interest in stellar structure, the radiation pressure is much less than the gas pressure and can often be neglected. The exception is the atmospheres of very hot stars, where the gas density is so low and the temperature so high that radiation pressure becomes important. A ...
... Note that in most cases of interest in stellar structure, the radiation pressure is much less than the gas pressure and can often be neglected. The exception is the atmospheres of very hot stars, where the gas density is so low and the temperature so high that radiation pressure becomes important. A ...
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.