Nuclear Physics
... a. Relate the energy produced through fission and fusion by stars as a driving force in the universe. b. Explain how the instability of radioactive isotopes results in spontaneous nuclear reactions. ...
... a. Relate the energy produced through fission and fusion by stars as a driving force in the universe. b. Explain how the instability of radioactive isotopes results in spontaneous nuclear reactions. ...
helium
... protons and 2 neutrons has been changed to 12 protons and 1 4He nucleus. The mass of 4He is approximately 4 times the mass of a proton. This leads to a very specific prediction for the mass fraction of the Universe which is in the form of helium: ...
... protons and 2 neutrons has been changed to 12 protons and 1 4He nucleus. The mass of 4He is approximately 4 times the mass of a proton. This leads to a very specific prediction for the mass fraction of the Universe which is in the form of helium: ...
Supernovae
... • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe)… thus they are ve ...
... • Neutrinos detected consistent with number expected from supernova in LMC in Feb 1987. • Probably type II SN because originator was massive B star (20 M) • Neutrinos are rarely absorbed so energy changed little over many x 10 9 years (except for loss due to expansion of Universe)… thus they are ve ...
Excited states of 136−138Sb from β decay
... provide important input into r-process calculations, especially as the exact site of this astrophysical reaction is presently unclear. The nucleus 135 Sb is the most neutron-rich one currently whose excited states have been studied via β decay3) . The Sb nuclei have one valence proton with respect t ...
... provide important input into r-process calculations, especially as the exact site of this astrophysical reaction is presently unclear. The nucleus 135 Sb is the most neutron-rich one currently whose excited states have been studied via β decay3) . The Sb nuclei have one valence proton with respect t ...
Lecture 9
... They all have large cross-sections and fast reaction rates ⇒ deuterium efficiently converts to 4 He. ...
... They all have large cross-sections and fast reaction rates ⇒ deuterium efficiently converts to 4 He. ...
Here
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
... protons) combine to form 1 helium nucleus (which has two protons and two neutrons). • The details are a bit complex: In the Sun, 6 hydrogen nuclei are involved in a sequence that produces two hydrogen nuclei and one helium nucleus. This is the proton-proton chain. In more massive stars, a carbon ...
STARS
... Red Giants and Supergiants • When a star runs out of hydrogen, it begins to die • Energy from fusion no ...
... Red Giants and Supergiants • When a star runs out of hydrogen, it begins to die • Energy from fusion no ...
R. Delaunay
... a rich distribution of growth products (see Figure 1) [3]. The fast creation of reactive fragments is due to ion collisions with molecule nuclei, a process specific to ion interaction with matter. Classical molecular dynamics simulations of the entire collision process, from the ion impact to the fo ...
... a rich distribution of growth products (see Figure 1) [3]. The fast creation of reactive fragments is due to ion collisions with molecule nuclei, a process specific to ion interaction with matter. Classical molecular dynamics simulations of the entire collision process, from the ion impact to the fo ...
Star Formation and Lifetimes
... The inward collapse of material causes the center of the protostar to become very hot and dense. Once the central temperature and density reach critical levels, nuclear fusion begin. During the fusion reaction, hydrogen atoms are combined together to form helium atoms. When this happens, photons of ...
... The inward collapse of material causes the center of the protostar to become very hot and dense. Once the central temperature and density reach critical levels, nuclear fusion begin. During the fusion reaction, hydrogen atoms are combined together to form helium atoms. When this happens, photons of ...
Full text - terrapub
... The ASPERA ion composition spectrometer made it possible to measure the distribution of different ion species. It was shown (Lundin et al., 1990; Norberg et al., 1993) that the inner magnetosphere of Mars is filled not only by O+-ions but contains also a substantial admixture of molecular ions (O2+, ...
... The ASPERA ion composition spectrometer made it possible to measure the distribution of different ion species. It was shown (Lundin et al., 1990; Norberg et al., 1993) that the inner magnetosphere of Mars is filled not only by O+-ions but contains also a substantial admixture of molecular ions (O2+, ...
Order-of-Magnitude Physics – Solution Set 4
... where the LHS is the time rate of change of the thermal energy density and the RHS is the divergence of the heat flux, with the heat flux written in terms of the thermal conductivity kc . Now the LHS is dominated by the ions which are not degenerate (the electrons are mostly degenerate and so can’t ...
... where the LHS is the time rate of change of the thermal energy density and the RHS is the divergence of the heat flux, with the heat flux written in terms of the thermal conductivity kc . Now the LHS is dominated by the ions which are not degenerate (the electrons are mostly degenerate and so can’t ...
Document
... have exactly the same set of quantum numbers 2) It is impossible to define the position & momentum of a particle to an accuracy better than Planck’s constant, h. I.e., if !x & !px are the uncertainties in the position & momentum of a particle, respectively, then • Pressure arises from the random mot ...
... have exactly the same set of quantum numbers 2) It is impossible to define the position & momentum of a particle to an accuracy better than Planck’s constant, h. I.e., if !x & !px are the uncertainties in the position & momentum of a particle, respectively, then • Pressure arises from the random mot ...
PowerPoint
... • Radioactive decay can be used for radioactive dating, by comparing the intensity left over after a given time to that predicted by the half life of the isotope. • Positron emitters can be used for PET scanning of isotope distribution inside a human/animal body. ...
... • Radioactive decay can be used for radioactive dating, by comparing the intensity left over after a given time to that predicted by the half life of the isotope. • Positron emitters can be used for PET scanning of isotope distribution inside a human/animal body. ...
5Stars_Part_Two
... Pulsars: 1. Pulsars emit pulses some as short as 1/40th of a second. 2. There are many things they could not be. 3. The only thing small enough, and rotating fast enough was a neutron star ...
... Pulsars: 1. Pulsars emit pulses some as short as 1/40th of a second. 2. There are many things they could not be. 3. The only thing small enough, and rotating fast enough was a neutron star ...
Microsoft Word - LifeCycleInteractive
... in the star is decreased, then gravity will now be stronger than the gas pressure. 1 Nuclear Fusion This results in an unstable star. What should happen next? 2 Out of Fuel Fusion Stops 18. The3star’s core has contracted. That means that density has increased, and the atoms are closer 4 Core togethe ...
... in the star is decreased, then gravity will now be stronger than the gas pressure. 1 Nuclear Fusion This results in an unstable star. What should happen next? 2 Out of Fuel Fusion Stops 18. The3star’s core has contracted. That means that density has increased, and the atoms are closer 4 Core togethe ...
Mike Zellner
... • Photons which create the spectra are emitted when and excited electron jumps from a higher energy orbital to an orbital of lower energy w=(Ea - Eb)/hbar • Concerned only with the Lyman a emissions (n=2 to n=1) ...
... • Photons which create the spectra are emitted when and excited electron jumps from a higher energy orbital to an orbital of lower energy w=(Ea - Eb)/hbar • Concerned only with the Lyman a emissions (n=2 to n=1) ...
MAJOR NUCLEAR BURNING STAGES The Coulomb barrier is
... 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will require increasingly high temperatures to overcome the increased electrical repulsion. 2.The amount of energy released by each successive reaction stage decreases so that later nuclear burning stages become ...
... 1.Successive nuclear burning stages, involving more massive nuclei with higher charges, will require increasingly high temperatures to overcome the increased electrical repulsion. 2.The amount of energy released by each successive reaction stage decreases so that later nuclear burning stages become ...
Lec10_2D
... In addition to ejecting a large amount of (nuclear processed) matter into space, a supernova explosions will leave behind a stellar remnant. In the remnant, the electrons of atoms are crushed into their nucleus. The star becomes one gigantic atomic nucleus made up only of neutrons – a neutron star. ...
... In addition to ejecting a large amount of (nuclear processed) matter into space, a supernova explosions will leave behind a stellar remnant. In the remnant, the electrons of atoms are crushed into their nucleus. The star becomes one gigantic atomic nucleus made up only of neutrons – a neutron star. ...
Star Formation Triggers More Star Formation
... solar masses: – The core temperature rises very fast. – Star’s internal pressure rises so fast it completely overcomes gravity – Star explodes, shedding large amounts of mass – Enough mass is shed to bring star below 120 solar mass limit ...
... solar masses: – The core temperature rises very fast. – Star’s internal pressure rises so fast it completely overcomes gravity – Star explodes, shedding large amounts of mass – Enough mass is shed to bring star below 120 solar mass limit ...
Chapter 15. The Chandrasekhar Limit, Iron-56 and Core
... Iron core. It cannot go beyond iron, because 56 F e is the most stable atom, in terms of binding energy per nucleon (see slide accompanying the lecture). It represents the dividing point between fission and fusion as sources of nuclear energy. Lighter atoms can be fused together to form more massive ...
... Iron core. It cannot go beyond iron, because 56 F e is the most stable atom, in terms of binding energy per nucleon (see slide accompanying the lecture). It represents the dividing point between fission and fusion as sources of nuclear energy. Lighter atoms can be fused together to form more massive ...
UNIFYING THEORY OF LOW-ENERGY NUCLEAR REACTION AND
... scale cavities [3-6]. The ground-state (superfluidity state) solution is used to obtain theoretical formulae for estimating the probabilities and rates of nuclear fusion for N identical Bose nuclei confined in a ion trap or an atomic cluster. Most recently, we have investigated the effect of a gener ...
... scale cavities [3-6]. The ground-state (superfluidity state) solution is used to obtain theoretical formulae for estimating the probabilities and rates of nuclear fusion for N identical Bose nuclei confined in a ion trap or an atomic cluster. Most recently, we have investigated the effect of a gener ...
Origin of the Elements and Atomic Structure
... • How are the different Earth systems ( lithospherebiosphere-hydrosphere-atmosphere) coupled to each other. • What is the fate of toxic pollutants in the ...
... • How are the different Earth systems ( lithospherebiosphere-hydrosphere-atmosphere) coupled to each other. • What is the fate of toxic pollutants in the ...
Fusor
A fusor is a device that uses an electric field to heat ions to conditions suitable for nuclear fusion. The machine has a voltage between two metal cages inside a vacuum. Positive ions fall down this voltage drop, building up speed. If they collide in the center, they can fuse. This is a type of Inertial electrostatic confinement device.A Farnsworth–Hirsch fusor is the most common type of fusor. This design came from work by Philo T. Farnsworth (in 1964) and Robert L. Hirsch in 1967. A variant of fusor had been proposed previously by William Elmore, James L. Tuck, and Ken Watson at the Los Alamos National Laboratory though they never built the machine.Fusors have been built by various institutions. These include academic institutions such as the University of Wisconsin–Madison, the Massachusetts Institute of Technology and government entities, such as the Atomic Energy Organization of Iran and the Turkish Atomic Energy Authority. Fusors have also been developed commercially, as sources for neutrons by DaimlerChrysler Aerospace and as a method for generating medical isotopes. Fusors have also become very popular for hobbyists and amateurs. A growing number of amateurs have performed nuclear fusion using simple fusor machines.