Name ______KEY Date Core ______ Study Guide Galaxies and the
... happened 14 billion years ago when the universe suddenly began to expand from one merged mass of matter or substance. At that time, all matter was dense and hot and the universe developed in less than a second. 300,000 years later, the first elements formed, then stars, planets and galaxies the next ...
... happened 14 billion years ago when the universe suddenly began to expand from one merged mass of matter or substance. At that time, all matter was dense and hot and the universe developed in less than a second. 300,000 years later, the first elements formed, then stars, planets and galaxies the next ...
Stellar Evolution
... Helium in the core fuses to carbon Core becomes hotter and hotter Helium burns faster and faster Star is now similar to its condition just as it left the Main Sequence, ...
... Helium in the core fuses to carbon Core becomes hotter and hotter Helium burns faster and faster Star is now similar to its condition just as it left the Main Sequence, ...
Fifth - Department of Physics and Astronomy
... sources, all burning outwards through the fresh fuel supply, there is instability. The relative speed at which they burn out can create an instability where the helium shell L increases with no release of pressure, leading to even more L. Eventually the L pushes the envelope out, the H shell extingu ...
... sources, all burning outwards through the fresh fuel supply, there is instability. The relative speed at which they burn out can create an instability where the helium shell L increases with no release of pressure, leading to even more L. Eventually the L pushes the envelope out, the H shell extingu ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Live fast, die young…leave no corpse The simulations revealed that a supermassive star burns hydrogen at a furious rate for under 2 million years—a mere blink of a cosmic eye (the Sun is about 5 billion years old) before beginning to collapse. Then what happens internally depends critically on its m ...
... Live fast, die young…leave no corpse The simulations revealed that a supermassive star burns hydrogen at a furious rate for under 2 million years—a mere blink of a cosmic eye (the Sun is about 5 billion years old) before beginning to collapse. Then what happens internally depends critically on its m ...
Stars in our Galaxy
... – Light travels at 300,000 km/s or about 9.5 trillion km in one year. – The nearest start to Earth other than the sun is Proxima Centauri which is 4.3 light years away or about 40 trillion km!!! ...
... – Light travels at 300,000 km/s or about 9.5 trillion km in one year. – The nearest start to Earth other than the sun is Proxima Centauri which is 4.3 light years away or about 40 trillion km!!! ...
Document
... – How fast you need to go in order to escape the surface. • How dense can something get? • How strong can the force of gravity be? • What if the escape velocity is faster than light? ...
... – How fast you need to go in order to escape the surface. • How dense can something get? • How strong can the force of gravity be? • What if the escape velocity is faster than light? ...
Document
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
Milky Way
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
... • What causes the mass to keep on increasing? • Don’t see anything there. Thus “dark” matter. ...
1)2 A light year is a) about six trillion miles. b) the distance to the star
... By 0.001 seconds after time began, all the protons in my brain were created from the quarks that arose from the energy of the Big Bang. ...
... By 0.001 seconds after time began, all the protons in my brain were created from the quarks that arose from the energy of the Big Bang. ...
Astrophysics and Chemistry Review Guide
... What happened in Air Force One with President Regan and how does it relate to the sun? Why doesn’t all of sun’s electromagnetic energy hit the surface of the Earth? What stops harmful UV rays? Why? ...
... What happened in Air Force One with President Regan and how does it relate to the sun? Why doesn’t all of sun’s electromagnetic energy hit the surface of the Earth? What stops harmful UV rays? Why? ...
chapter6
... very specific radii and energies. • These characteristic electron energies are different for each individual element. ...
... very specific radii and energies. • These characteristic electron energies are different for each individual element. ...
Type 1a Supernovae - RanelaghALevelPhysics
... The white dwarf reaches a larger mass, approaching the Chandrasekhar limit But just before it would collapse into a neutron star (within 1% of the limit), the temperature and density inside the core increase enough to allow the fusion of carbon to take place. ...
... The white dwarf reaches a larger mass, approaching the Chandrasekhar limit But just before it would collapse into a neutron star (within 1% of the limit), the temperature and density inside the core increase enough to allow the fusion of carbon to take place. ...
Stages 7 to 9 - Sun
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
... Off the Main Sequence - The Evolution of a Sun-like Star Stages 7 - 9 While on the main sequence, the star is burning hydrogen. It’s luminosity is determined by the stars mass. The most intense fusion is occurring at the center regions of the core (highest pressure and temperature). ...
Pre-Main Sequence Evolution
... • In general, the timescale for accretion, τ acc ~ M / M! , is shorter than the protostar’s thermal timescale. The protostar cannot thermally adjust to the added energy, and therefore heats up adiabatically. • Eventually, the protostar becomes hot enough to disassociate molecular hydrogen. When th ...
... • In general, the timescale for accretion, τ acc ~ M / M! , is shorter than the protostar’s thermal timescale. The protostar cannot thermally adjust to the added energy, and therefore heats up adiabatically. • Eventually, the protostar becomes hot enough to disassociate molecular hydrogen. When th ...
Earth Science Unit Test Review
... 1. Describe composition of Sun. What type of star is it? How long does it take light from Sun to reach us? 2. Identify the features of the Sun on a diagram. Why do sunspots appear dark? 3. Desc ...
... 1. Describe composition of Sun. What type of star is it? How long does it take light from Sun to reach us? 2. Identify the features of the Sun on a diagram. Why do sunspots appear dark? 3. Desc ...
Section 7.3 - CPO Science
... 7.3 Temperature and color • If you look closely at the stars on a clear night, you might see a slight reddish or bluish tint to some stars. • This is because stars’ surface temperatures are different. ...
... 7.3 Temperature and color • If you look closely at the stars on a clear night, you might see a slight reddish or bluish tint to some stars. • This is because stars’ surface temperatures are different. ...
The Universe
... •As the evolutionist astronomers Clark and Caswell say, ‗Why have the large number of expected remnants not been detected?‘ and these authors refer to ‗The mystery of the missing remnants‘. Clark and Caswell, 1976. Monthly Notices of the Royal Astronomical Society, 174:267; cited in ...
... •As the evolutionist astronomers Clark and Caswell say, ‗Why have the large number of expected remnants not been detected?‘ and these authors refer to ‗The mystery of the missing remnants‘. Clark and Caswell, 1976. Monthly Notices of the Royal Astronomical Society, 174:267; cited in ...
BA Training – XRT software
... reactions in core cease. Drop of pressure in core causes core to contract. Surrounding H is pulled into core region and raised in temperature. Burning occurs in H-shell around He core. Burnt H added to core, whose density increases B-C Core contracts when too much material has been added to it. Ener ...
... reactions in core cease. Drop of pressure in core causes core to contract. Surrounding H is pulled into core region and raised in temperature. Burning occurs in H-shell around He core. Burnt H added to core, whose density increases B-C Core contracts when too much material has been added to it. Ener ...
The Big Bang Theory
... frequency appears to increase and is therefore said to be blueshifted. In contrast, the radiation emitted by an object moving away is stretched or redshifted. Blueshifts and redshifts exhibited by stars, galaxies and gas clouds also indicate their motions with respect to the observer. ...
... frequency appears to increase and is therefore said to be blueshifted. In contrast, the radiation emitted by an object moving away is stretched or redshifted. Blueshifts and redshifts exhibited by stars, galaxies and gas clouds also indicate their motions with respect to the observer. ...
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.