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... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
... • As the helium core grows, it compresses. Helium doesn’t fuse to heavier elements for two reasons. (1) with 2 p+ per nucleus, the electric repulsion force is higher than was the case for H-fusion. This means that helium fusion requires a higher temperature than hydrogen fusion -- 100 million K (2) ...
Stellar Remnants White Dwarfs, Neutron Stars & Black Holes
... White Dwarfs • composed mainly of Carbon & Oxygen • formed from stars that are 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 ...
... White Dwarfs • composed mainly of Carbon & Oxygen • formed from stars that are 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 ...
Article 8
... (from all the gas and dust bumping into each other under the great pressure of the surrounding material) reaches 15 million degrees or so. A wondrous event occurs.... nuclear fusion begins and the ball of gas and dust starts to glow. A new star has begun its life in our Universe. So what is this mag ...
... (from all the gas and dust bumping into each other under the great pressure of the surrounding material) reaches 15 million degrees or so. A wondrous event occurs.... nuclear fusion begins and the ball of gas and dust starts to glow. A new star has begun its life in our Universe. So what is this mag ...
ASTR2050 Spring 2005 •
... This is much hotter than the surface of the Sun, but the center of the Sun would be much higher pressure. This is the key to how the Sun and other stars shine! ...
... This is much hotter than the surface of the Sun, but the center of the Sun would be much higher pressure. This is the key to how the Sun and other stars shine! ...
PHYS 2410 General Astronomy Homework 7
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
... The energy emitted from the surface of a main sequence star is _____the energy generated in the core. a. ...
Stars and The Universe
... itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, parts of the massive star fly away into space, where they can form _____________. If the mass remaining in the dead star’s core is 3 times our sun’s mass, it will form a _____ ...
... itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, parts of the massive star fly away into space, where they can form _____________. If the mass remaining in the dead star’s core is 3 times our sun’s mass, it will form a _____ ...
AST101 Lecture 20 The Ecology of the Galaxy
... • The bulge is also old • The disk is youngest The age is correlated with flatness The Sun is in the disk ...
... • The bulge is also old • The disk is youngest The age is correlated with flatness The Sun is in the disk ...
Discussion Activity #13
... least 10 times as much matter as we see in the Milky Way disk, suggesting that the halo is full of dark matter. B. The orbital speeds of stars far from the galactic center are surprisingly high, suggesting that these stars are feeling gravitational effects from unseen matter in the halo. C. Our view ...
... least 10 times as much matter as we see in the Milky Way disk, suggesting that the halo is full of dark matter. B. The orbital speeds of stars far from the galactic center are surprisingly high, suggesting that these stars are feeling gravitational effects from unseen matter in the halo. C. Our view ...
0802 - thephysicsteacher.ie
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean 'water-forming'. Hydrogen atoms were made in the Big Bang, when the universe is be ...
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean 'water-forming'. Hydrogen atoms were made in the Big Bang, when the universe is be ...
CBradleyLoutl
... hydrogen fusion at all, the star passes through the main sequence and becomes a white dwarf, slowly cooling. . ~.08 - .3 Solar Masses, the the hydrogen burning can only produce Helium 3. . .3 - 1.2 Solar Masses: It will expand into a red giant, then fall back down into a white dwarf. If the star’s m ...
... hydrogen fusion at all, the star passes through the main sequence and becomes a white dwarf, slowly cooling. . ~.08 - .3 Solar Masses, the the hydrogen burning can only produce Helium 3. . .3 - 1.2 Solar Masses: It will expand into a red giant, then fall back down into a white dwarf. If the star’s m ...
Overview Evolution of massive stars Evolution of massive stars
... The shock from the supernova is traveling outward at about 10% the speed of light. The ejecta carrys the newly synthesized elements with it into the interstellar medium, ready to become the next generation of stars. When the shock encounters a stable gas cloud it mixes metals into the gas cloud, and ...
... The shock from the supernova is traveling outward at about 10% the speed of light. The ejecta carrys the newly synthesized elements with it into the interstellar medium, ready to become the next generation of stars. When the shock encounters a stable gas cloud it mixes metals into the gas cloud, and ...
29.3-stellar-evolution
... The core heats up to much higher temps. Star will expand to a supergiant. Iron forms in the core and becomes too massive to be supported. The core collapses in on itself in a violent explosion. This is called a supernova. A supernova can go in two directions. 1. Neutron star When the c ...
... The core heats up to much higher temps. Star will expand to a supergiant. Iron forms in the core and becomes too massive to be supported. The core collapses in on itself in a violent explosion. This is called a supernova. A supernova can go in two directions. 1. Neutron star When the c ...
0802c - Thephysicsteacher
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean ‘water-forming’. Hydrogen atoms were made in the Big Bang, when the universe is be ...
... Hydrogen is the most common element in the universe. 88% of all atoms are hydrogen atoms so there is more hydrogen than any other substance. The name comes from the two Greek words hydro and genes, which together mean ‘water-forming’. Hydrogen atoms were made in the Big Bang, when the universe is be ...
Stars: from Adolescence to Old Age
... planets in early telescopes • Now known to be formed when old, low-mass stars are unable to fuse heavier elements, and their cores collapse – The outer layer of the star is ejected by wind ...
... planets in early telescopes • Now known to be formed when old, low-mass stars are unable to fuse heavier elements, and their cores collapse – The outer layer of the star is ejected by wind ...
Stars and The Universe
... a supernova. 17. The temperature change of #16 will cause the volume of the star to ________. shrink 18. When a massive star runs out of fuel and collapses on itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, the outside laye ...
... a supernova. 17. The temperature change of #16 will cause the volume of the star to ________. shrink 18. When a massive star runs out of fuel and collapses on itself, its mass collides at its core and bounces back in an explosion called a ____________. As a result of this explosion, the outside laye ...
Chapter 13 Practice Questions
... 10. Each successive stage of core nuclear reactions in a massive star lasts for considerably less time than the previous stage (e.g., for a 25-solar-mass star, carbon fusion lasts for 600 years, while neon fusion lasts for only 1 year). One reason for this is that A) the later the stage of fusion, t ...
... 10. Each successive stage of core nuclear reactions in a massive star lasts for considerably less time than the previous stage (e.g., for a 25-solar-mass star, carbon fusion lasts for 600 years, while neon fusion lasts for only 1 year). One reason for this is that A) the later the stage of fusion, t ...
Helium Production in Big Bang Weighing a Galaxy12 Nov 11/12/2010
... 2. At 5s, T=10GK, and kT=0.9MeV. Same question. • At 5s, 10BK, and kT=0.9MeV. n/p=0.2. • When T is between 10BK and 3BK, the density drops so that – number of collisions falls & neutrons and protons are no longer in ...
... 2. At 5s, T=10GK, and kT=0.9MeV. Same question. • At 5s, 10BK, and kT=0.9MeV. n/p=0.2. • When T is between 10BK and 3BK, the density drops so that – number of collisions falls & neutrons and protons are no longer in ...
Quarter 1 Review of Transfer of Learning
... 1.) An important piece of evidence supporting the Big Bang Theory is that all galaxies are moving away from the Earth. We know that this is true because of the Doppler Effect things moving away from us would have a longer wavelength (whether it be wavelengths of sound or light), and the faster somet ...
... 1.) An important piece of evidence supporting the Big Bang Theory is that all galaxies are moving away from the Earth. We know that this is true because of the Doppler Effect things moving away from us would have a longer wavelength (whether it be wavelengths of sound or light), and the faster somet ...
3_Ocean126_2006
... Cloud that lies just beyond the Milky Way. The star, known in modern times as Sanduleak 69-202, is a blue supergiant 25 times more massive than our Sun. Such explosions distribute all the common elements such as Oxygen, Carbon, Nitrogen, Calcium and Iron into interstellar space where they enrich clo ...
... Cloud that lies just beyond the Milky Way. The star, known in modern times as Sanduleak 69-202, is a blue supergiant 25 times more massive than our Sun. Such explosions distribute all the common elements such as Oxygen, Carbon, Nitrogen, Calcium and Iron into interstellar space where they enrich clo ...
Parallax
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
... layers to expand and cool Star becomes a giant Helium nuclei fuse to form a core of Carbon ...
The Sun - www .alexandria .k12 .mn .us
... Sunspots expand and contract as they move round the Sun and can be as large as 80000 km in diameter making them clearly visible from Earth. ...
... Sunspots expand and contract as they move round the Sun and can be as large as 80000 km in diameter making them clearly visible from Earth. ...
The Life Cycles of Stars
... The core of a massive star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive s ...
... The core of a massive star that is 1.5 to 4 times as massive as our Sun ends up as a neutron star after the supernova. Neutron stars spin rapidly giving off radio waves. If the radio waves are emitted in pulses (due to the star’s spin), these neutron stars are called pulsars. The core of a massive s ...
Nucleosynthesis
Nucleosynthesis is the process that creates new atomic nuclei from pre-existing nucleons, primarily protons and neutrons. The first nuclei were formed about three minutes after the Big Bang, through the process called Big Bang nucleosynthesis. It was then that hydrogen and helium formed to become the content of the first stars, and this primeval process is responsible for the present hydrogen/helium ratio of the cosmos.With the formation of stars, heavier nuclei were created from hydrogen and helium by stellar nucleosynthesis, a process that continues today. Some of these elements, particularly those lighter than iron, continue to be delivered to the interstellar medium when low mass stars eject their outer envelope before they collapse to form white dwarfs. The remains of their ejected mass form the planetary nebulae observable throughout our galaxy.Supernova nucleosynthesis within exploding stars by fusing carbon and oxygen is responsible for the abundances of elements between magnesium (atomic number 12) and nickel (atomic number 28). Supernova nucleosynthesis is also thought to be responsible for the creation of rarer elements heavier than iron and nickel, in the last few seconds of a type II supernova event. The synthesis of these heavier elements absorbs energy (endothermic) as they are created, from the energy produced during the supernova explosion. Some of those elements are created from the absorption of multiple neutrons (the R process) in the period of a few seconds during the explosion. The elements formed in supernovas include the heaviest elements known, such as the long-lived elements uranium and thorium.Cosmic ray spallation, caused when cosmic rays impact the interstellar medium and fragment larger atomic species, is a significant source of the lighter nuclei, particularly 3He, 9Be and 10,11B, that are not created by stellar nucleosynthesis.In addition to the fusion processes responsible for the growing abundances of elements in the universe, a few minor natural processes continue to produce very small numbers of new nuclides on Earth. These nuclides contribute little to their abundances, but may account for the presence of specific new nuclei. These nuclides are produced via radiogenesis (decay) of long-lived, heavy, primordial radionuclides such as uranium and thorium. Cosmic ray bombardment of elements on Earth also contribute to the presence of rare, short-lived atomic species called cosmogenic nuclides.