Uncovering the nuclear atom
... 5. Using complete sentences, describe what the isotopes of an element have in common and how they are different. ...
... 5. Using complete sentences, describe what the isotopes of an element have in common and how they are different. ...
LECTURE 6 NUCLEAR PHENOMENOLOGY, MASS SPECTROSCOPY PHY492 Nuclear and Elementary Particle Physics
... key observable for nuclear structure d n ...
... key observable for nuclear structure d n ...
The Evolution and Explosion of Massive Stars
... • Originated from SN 1987A in the Large Magellanic Cloud about 55 kpc from here – first signal from the supernova though the optical light was detected first (about 6 hr later) and the neutrino signal only discovered by processing data about a week later ...
... • Originated from SN 1987A in the Large Magellanic Cloud about 55 kpc from here – first signal from the supernova though the optical light was detected first (about 6 hr later) and the neutrino signal only discovered by processing data about a week later ...
Age of our galaxy - Purdue Physics
... Age of the earth The best age for the Earth comes not from dating individual rocks but by considering the Earth and meteorites as part of the same evolving system in which the isotopic composition of lead, specifically the ratio of lead-207 to lead-206 changes over time owing to the decay of radioa ...
... Age of the earth The best age for the Earth comes not from dating individual rocks but by considering the Earth and meteorites as part of the same evolving system in which the isotopic composition of lead, specifically the ratio of lead-207 to lead-206 changes over time owing to the decay of radioa ...
MTH 231 - Shelton State
... Sets • A set is a collection of objects. • An object that belongs to a particular set is called an element, or member. • Sets must be well-defined: 1. there must be a universe of objects that are allowed into consideration; 2. each object either is or is not an element of the set. ...
... Sets • A set is a collection of objects. • An object that belongs to a particular set is called an element, or member. • Sets must be well-defined: 1. there must be a universe of objects that are allowed into consideration; 2. each object either is or is not an element of the set. ...
(Star Stuff) ( 11-9-10)
... 3. High mass star (M > 4 solar masses) •Fusion of He,C,O,…..but not Fe (Iron) fusion Faster and faster Core collapses Supernova Produces all elements heavier than Fe and blows envelope apart ejecting to interstellar space most of its mass ...
... 3. High mass star (M > 4 solar masses) •Fusion of He,C,O,…..but not Fe (Iron) fusion Faster and faster Core collapses Supernova Produces all elements heavier than Fe and blows envelope apart ejecting to interstellar space most of its mass ...
The Earth and Beyond
... thrown away by the explosion and the remaining core turns into a NEUTRON STAR. If the star is big enough it could become a BLACK HOLE. ...
... thrown away by the explosion and the remaining core turns into a NEUTRON STAR. If the star is big enough it could become a BLACK HOLE. ...
Lesson 4: Stellar Explosions and Neutron Stars
... Co has too many neutrons to be stable and radioactively decays: ν e> + γ • 61Co → 61Ni + e- + <ν • This continues, making the rest of the elements through bismuth-209 (83 protons + 126 neutrons), including such famous elements as copper, silver, lead, gold, etc. • Rapid neutron capture (r-process): ...
... Co has too many neutrons to be stable and radioactively decays: ν e> + γ • 61Co → 61Ni + e- + <ν • This continues, making the rest of the elements through bismuth-209 (83 protons + 126 neutrons), including such famous elements as copper, silver, lead, gold, etc. • Rapid neutron capture (r-process): ...
here
... 11: CNO cycle. Stars more massive than about 1.2 M⊙ burn H on the main sequence via the CNO cycle, whereas stars less massive than this burn H on the main sequence via the pp chain. 12: Residual heat. Neutron stars are born when the cores of massive stars collapse at the end of their evolution. Afte ...
... 11: CNO cycle. Stars more massive than about 1.2 M⊙ burn H on the main sequence via the CNO cycle, whereas stars less massive than this burn H on the main sequence via the pp chain. 12: Residual heat. Neutron stars are born when the cores of massive stars collapse at the end of their evolution. Afte ...
helium
... temperature, T, don’t depend on what happened at earlier times and higher temperature ...
... temperature, T, don’t depend on what happened at earlier times and higher temperature ...
Neutrinos and Nucleosynthesis
... simulations. Today one knows that elements are produced in a process which is called nucleosynthesis. There are different types of nucleosynthesis. One type is the supernova nucleosynthesis. During a supernova nucleosynthesis elements heavier than 56 Fe are produced through different processes, whic ...
... simulations. Today one knows that elements are produced in a process which is called nucleosynthesis. There are different types of nucleosynthesis. One type is the supernova nucleosynthesis. During a supernova nucleosynthesis elements heavier than 56 Fe are produced through different processes, whic ...
ppt - Department of Physics & Astronomy at the University of Utah
... deposit vast quantities of material that has been “cooked” in the “bowels” of stars… • Can check stellar models against observed abundance of elements • Core collapse supernovae are responsible for the significant quantities of Oxygen in the universe • Production of heavier elements occur via rproce ...
... deposit vast quantities of material that has been “cooked” in the “bowels” of stars… • Can check stellar models against observed abundance of elements • Core collapse supernovae are responsible for the significant quantities of Oxygen in the universe • Production of heavier elements occur via rproce ...
nuclear fusion atoms
... 4. Ninety-five percent of matter in the universe is found in ___________________ . 5. By looking deep into space, we can see back in time about __________________ billion years. 6. Many cosmologists say the ________ _________ Theory helps explain why the universe has universal forces and continues t ...
... 4. Ninety-five percent of matter in the universe is found in ___________________ . 5. By looking deep into space, we can see back in time about __________________ billion years. 6. Many cosmologists say the ________ _________ Theory helps explain why the universe has universal forces and continues t ...
Blackholes - Indiana University Astronomy
... The Origin of Elements • The process by which elements (nuclei) are created (synthesized) is called nucleosynthesis • Nucleosynthesis has occurred since the creation of the universe and will essentially go on forever • The elements created come together to form everything material we know, includin ...
... The Origin of Elements • The process by which elements (nuclei) are created (synthesized) is called nucleosynthesis • Nucleosynthesis has occurred since the creation of the universe and will essentially go on forever • The elements created come together to form everything material we know, includin ...
death_high_mass_2b
... reach the molecular clouds around it, but when it does it will set off star formation. ...
... reach the molecular clouds around it, but when it does it will set off star formation. ...
Stars: from Adolescence to Old Age
... Shell burning starts •outer layers of star expand •core continues to contract ...
... Shell burning starts •outer layers of star expand •core continues to contract ...
Star formation and Evolution
... Stars are formed when part of a interstellar gas cloud contracts under its own gravitational force; as it collapses, the center becomes hotter until nuclear fusion begins in the core. Interstellar gas and dust, which make up the interstellar medium, are concentrated in the disk of the Galaxy ...
... Stars are formed when part of a interstellar gas cloud contracts under its own gravitational force; as it collapses, the center becomes hotter until nuclear fusion begins in the core. Interstellar gas and dust, which make up the interstellar medium, are concentrated in the disk of the Galaxy ...
Document
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
... with the nuclear binding energy B(Z,N) Some features of this equation: • in NSE there is a mix of free nucleons and nuclei • higher density favors (heavier) nuclei • higher temperature favors free nucleons (or lighter nuclei) • nuclei with high binding energy are strongly favored ...
Slide 1
... hope to see the “Higgs Boson” and gain some more understanding not only to why those extra chips make us fatter but why the molecules themselves have the property that we assign as “mass” ...
... hope to see the “Higgs Boson” and gain some more understanding not only to why those extra chips make us fatter but why the molecules themselves have the property that we assign as “mass” ...
stars - Iowa State University
... found themselves at a profound loss to explain how exactly dying stars could blow away these clouds. Now astrophysicists propose that unexpected chemical reactions during the formation of stardust could help solve this mystery. "In the long run, the new scenario may have an important impact on our u ...
... found themselves at a profound loss to explain how exactly dying stars could blow away these clouds. Now astrophysicists propose that unexpected chemical reactions during the formation of stardust could help solve this mystery. "In the long run, the new scenario may have an important impact on our u ...
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.