
dark matter - Aurora City Schools
... microwave radiation all throughout the universe, but couldn’t explain where it came from • Only possible source is it’s left over from Big Bang • Later shown not to be “evenly spread” ...
... microwave radiation all throughout the universe, but couldn’t explain where it came from • Only possible source is it’s left over from Big Bang • Later shown not to be “evenly spread” ...
File
... • We currently know of 118 different elements. • The 81 stable elements found on Earth make up the bulk of matter in the universe. • 10 radioactive elements also occur naturally on our planet. • 19 radioactive elements have been artificially produced in nuclear laboratories. ...
... • We currently know of 118 different elements. • The 81 stable elements found on Earth make up the bulk of matter in the universe. • 10 radioactive elements also occur naturally on our planet. • 19 radioactive elements have been artificially produced in nuclear laboratories. ...
ppt - Wladimir Lyra
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
... The Helium Flash never happens The star reaches Helium burning temperatures before the core becomes degenerate ...
1_Introduction
... If the universe hadn’t been flattened, it would have long since collapsed in a Big Crunch or fizzled out in a Big Chill. ...
... If the universe hadn’t been flattened, it would have long since collapsed in a Big Crunch or fizzled out in a Big Chill. ...
Origin of the Elements
... the helium begins fusing into carbon (C) at its core, but hydrogen continues to form helium in a thin ...
... the helium begins fusing into carbon (C) at its core, but hydrogen continues to form helium in a thin ...
Name Origins: Back to the Beginning Video Questions http://www
... Origins: Back to the Beginning Video Questions http://www.pbs.org/wgbh/nova/space/origins-series-overview.html#origins-back-beginning 1. The Big Bang theory has been called the greatest discovery in cosmology. Describe it. ...
... Origins: Back to the Beginning Video Questions http://www.pbs.org/wgbh/nova/space/origins-series-overview.html#origins-back-beginning 1. The Big Bang theory has been called the greatest discovery in cosmology. Describe it. ...
Ch. 21
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. • Stars greater than 8 solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues ...
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. • Stars greater than 8 solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues ...
Stellar Explosions
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. • Stars greater than 8 solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues ...
... • A nova is a star that suddenly brightens and gradually fades; it is a white dwarf whose larger partner continually transfers material to it. • Stars greater than 8 solar masses can have fusion in their cores going all the way up to iron, which is stable against further fusion. • The star continues ...
The fantastic journey of that ring on your finger: From
... ultimately leaving a tiny hot residue known as a white dwarf. But, in more massive stars, gravity will exert enough pressure to ignite carbon fusion, forming heavier and heavier elements like neon, oxygen, silicon, and eventually iron; and that’s when the pandemonium begins. Iron has the most stable ...
... ultimately leaving a tiny hot residue known as a white dwarf. But, in more massive stars, gravity will exert enough pressure to ignite carbon fusion, forming heavier and heavier elements like neon, oxygen, silicon, and eventually iron; and that’s when the pandemonium begins. Iron has the most stable ...
Geol. 655 Isotope Geochemistry
... history of the cosmos. Astronomy is a bit like geology in that just as we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. It turns out that old stars (such old stars are most abundant in the globular clusters outs ...
... history of the cosmos. Astronomy is a bit like geology in that just as we learn about the evolution of the Earth by examining old rocks, we can learn about the evolution of the cosmos by looking at old stars. It turns out that old stars (such old stars are most abundant in the globular clusters outs ...
Worksheet
... new fuel sources are depleted at faster and faster rates. Since the heaviest element created in a star by nuclear fusion reactions is iron, a large iron core eventually forms at the center of everything. At this point, gravity becomes overwhelming, the core collapses, and an explosion occurs, during ...
... new fuel sources are depleted at faster and faster rates. Since the heaviest element created in a star by nuclear fusion reactions is iron, a large iron core eventually forms at the center of everything. At this point, gravity becomes overwhelming, the core collapses, and an explosion occurs, during ...
b) Formation of Heavy Elements
... Element Formation and Supernovae Elements heavier than Iron get created during Supernova Explosions. Since there are two types of supernovae (SN I and SN II — the end stage of a low mass binary and the end stage of a high mass single star), the details are a little different, but the general proces ...
... Element Formation and Supernovae Elements heavier than Iron get created during Supernova Explosions. Since there are two types of supernovae (SN I and SN II — the end stage of a low mass binary and the end stage of a high mass single star), the details are a little different, but the general proces ...
nuclear reactions
... repulsion can be overcome by the attractive nuclear force which is stronger at close distances. • If the matter is sufficiently heated (plasma state), the thermonuclear fusion reaction may occur due to collisions between the particles of extreme thermal kinetic energies. • Laboratory fusion of hydro ...
... repulsion can be overcome by the attractive nuclear force which is stronger at close distances. • If the matter is sufficiently heated (plasma state), the thermonuclear fusion reaction may occur due to collisions between the particles of extreme thermal kinetic energies. • Laboratory fusion of hydro ...
lecture18
... This build up of heavy elements takes time, since it waits on a free neutron to wander along and initiate the next reaction. But after time, it allows the formation of elements as heavy as 209Bi (Bismuth) with 83 protons. Beyond that, the slow process (s-process) fails since a new nucleus formed by ...
... This build up of heavy elements takes time, since it waits on a free neutron to wander along and initiate the next reaction. But after time, it allows the formation of elements as heavy as 209Bi (Bismuth) with 83 protons. Beyond that, the slow process (s-process) fails since a new nucleus formed by ...
80.BrainPopLifeCycleStars
... under the pressure of gravity. _____________, it will begin to expand and contract, shedding its outer layers in the process. The remains of those out layers form a big cloud of gas and dust, called a ____________________. 13.At the center of a planetary nebula is a core of ___________, which after ...
... under the pressure of gravity. _____________, it will begin to expand and contract, shedding its outer layers in the process. The remains of those out layers form a big cloud of gas and dust, called a ____________________. 13.At the center of a planetary nebula is a core of ___________, which after ...
Nuclear and Particle Physics - Lecture 26 Nucleosynthesis 1
... K, that neutral atoms could form without immediate reionisation. This turned off electromagnetism as the dominant force between matter particles and allowed gravity to take over. Being purely attractive, this meant any fluctuations in the density of matter would grow, attracting more matter and even ...
... K, that neutral atoms could form without immediate reionisation. This turned off electromagnetism as the dominant force between matter particles and allowed gravity to take over. Being purely attractive, this meant any fluctuations in the density of matter would grow, attracting more matter and even ...
Lesson Plan: Supernova`s
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
... A supernova is when a very big star explodes. This happens when a star totally runs out of energy to make heat and light. When the star explodes, it will be brighter than all other stars. If a supernova explosion happened near the Earth, we could see it in the sky even during the day. Supernova expl ...
Facts - short version
... In the centre of some galaxies is a black hole. Everything nearby gets pulled into a black hole; stars, dust clouds, even light – it all gets sucked in and disappears. ...
... In the centre of some galaxies is a black hole. Everything nearby gets pulled into a black hole; stars, dust clouds, even light – it all gets sucked in and disappears. ...
6 Big Bang Nucleosynthesis - Course Pages of Physics Department
... up a few per cent. The rest, i.e., the major part, is hydrogen. The building blocks of atomic nuclei, the nucleons, or protons and neutrons, formed in the QCD phase transition at T ∼ 150 MeV and t ∼ 20 µs. Elements heavier than lithium, up to iron, cobalt, and nickel, have been made from lighter ele ...
... up a few per cent. The rest, i.e., the major part, is hydrogen. The building blocks of atomic nuclei, the nucleons, or protons and neutrons, formed in the QCD phase transition at T ∼ 150 MeV and t ∼ 20 µs. Elements heavier than lithium, up to iron, cobalt, and nickel, have been made from lighter ele ...
starevolution - Global Change Program
... of H is 1 and its mass is ~1.67E-24 gram; atomic weight is typically expressed as reference mass, and is slightly more than 1 for H (it is 1.0079) because of the presence of other H isotopes. The next element in the periodic system, He, has atomic number 2 (two protons and 2 neutrons) and a mass of ...
... of H is 1 and its mass is ~1.67E-24 gram; atomic weight is typically expressed as reference mass, and is slightly more than 1 for H (it is 1.0079) because of the presence of other H isotopes. The next element in the periodic system, He, has atomic number 2 (two protons and 2 neutrons) and a mass of ...
Equivalent Widths and Chemical abundances Equivalent
... 5) Also note the relative peak of the “iron peak” elements, Fe and Ni. 6) Note that Iron-56 represents the most stable atom in the sense of the greatest binding energy per nucleon, so it is the dividing point between where nuclear reactions yield energy by fusion and where they yield them by fission ...
... 5) Also note the relative peak of the “iron peak” elements, Fe and Ni. 6) Note that Iron-56 represents the most stable atom in the sense of the greatest binding energy per nucleon, so it is the dividing point between where nuclear reactions yield energy by fusion and where they yield them by fission ...
Standard Set 2 - Atascadero High School
... heavier than iron. This type can be carried out only by adding neutrons to a preexisting heavy element that forms a “seed.” Neutrons are available only during a limited portion of a star’s lifetime, particularly during the brief supernova that occurs when a massive star dies. Section D Students know ...
... heavier than iron. This type can be carried out only by adding neutrons to a preexisting heavy element that forms a “seed.” Neutrons are available only during a limited portion of a star’s lifetime, particularly during the brief supernova that occurs when a massive star dies. Section D Students know ...
Lecture 18: Supernovae
... energy in this reaction to make it happen. That energy comes from the kinetic (=energy of motion) of the very hot proton and electron. The neutrino flies out of the star, taking energy with it. Note that electron degeneracy pressure will not be important source of pressure in this situation because ...
... energy in this reaction to make it happen. That energy comes from the kinetic (=energy of motion) of the very hot proton and electron. The neutrino flies out of the star, taking energy with it. Note that electron degeneracy pressure will not be important source of pressure in this situation because ...
Introduction - Assets - Cambridge
... each star record the abundance of metals in the gas from which the star formed. The most metal-poor stars in our Milky Way galaxy of stars have only 1/10 000th of the iron atoms (in comparison with hydrogen) as the Sun. These are also the oldest stars, probably among the first to be born in the infa ...
... each star record the abundance of metals in the gas from which the star formed. The most metal-poor stars in our Milky Way galaxy of stars have only 1/10 000th of the iron atoms (in comparison with hydrogen) as the Sun. These are also the oldest stars, probably among the first to be born in the infa ...
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.