Answers
... T4, whilst CNO goes as about T16. Hence, a modest increase in core temperature (higher mass star cores are hotter than lower mass) leads to a massive increase in the CNO rate, but only a modest rise in the p-p rate. ...
... T4, whilst CNO goes as about T16. Hence, a modest increase in core temperature (higher mass star cores are hotter than lower mass) leads to a massive increase in the CNO rate, but only a modest rise in the p-p rate. ...
Nuclear Astrophysics (a Cosmic Cookbook)
... Opposite charges attract A negatively charged electron feels an attractive force towards a proton ...
... Opposite charges attract A negatively charged electron feels an attractive force towards a proton ...
Fission and Fusion Power Point
... by inserting CADMIUM RODS into the reaction chamber. These rods absorb some of the NEUTRONS produced and slow the CHAIN REACTION so that it can proceed at a CONTROLLED RATE. ...
... by inserting CADMIUM RODS into the reaction chamber. These rods absorb some of the NEUTRONS produced and slow the CHAIN REACTION so that it can proceed at a CONTROLLED RATE. ...
High Energy Observational Astrophysics
... Sun will emit in its entire lifetime) If a main sequence star has a mass of over 8 times the mass of the Sun it is destined to be a type II supernova ...
... Sun will emit in its entire lifetime) If a main sequence star has a mass of over 8 times the mass of the Sun it is destined to be a type II supernova ...
Why can the sun persistently produce energy for the stable output of
... 4. Why nuclear fusion does not occur readily? Since atomic nuclei consist of positively charged protons, they repel each other by virtue of electrostatic force. Under high temperature condition, particles possess sufficient kinetic energy to overcome the electrostatic repulsion and approach each ...
... 4. Why nuclear fusion does not occur readily? Since atomic nuclei consist of positively charged protons, they repel each other by virtue of electrostatic force. Under high temperature condition, particles possess sufficient kinetic energy to overcome the electrostatic repulsion and approach each ...
Fission and Fusion
... In this example, a stray neutron strikes an atom of U-235. It absorbs the neutron and becomes an unstable atom of U-236. It then undergoes fission. Notice that more neutrons are released in the reaction. These neutrons can strike other U-235 atoms to initiate their fission. ...
... In this example, a stray neutron strikes an atom of U-235. It absorbs the neutron and becomes an unstable atom of U-236. It then undergoes fission. Notice that more neutrons are released in the reaction. These neutrons can strike other U-235 atoms to initiate their fission. ...
Notes: Nuclear Chemistry
... has a limited penetrating power and a +1 charge. Positrons have limited penetration into matter because when a positron comes into contact with an electron, they annihilate each other producing two γ-rays. Positrons are deflected towards the negative end in a magnetic or electric field. Annihilation ...
... has a limited penetrating power and a +1 charge. Positrons have limited penetration into matter because when a positron comes into contact with an electron, they annihilate each other producing two γ-rays. Positrons are deflected towards the negative end in a magnetic or electric field. Annihilation ...
08 October: Stellar life after the Main Sequence
... Why mass is destiny: the more mass, the more fuel, but more massive stars use up their fuel at much higher rates ...
... Why mass is destiny: the more mass, the more fuel, but more massive stars use up their fuel at much higher rates ...
Unit 8 Astronomy
... When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 times the mass of the ______ hydrogen can do this with no problem: they burn _____________, helium carbon and then _____ ...
... When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 times the mass of the ______ hydrogen can do this with no problem: they burn _____________, helium carbon and then _____ ...
Structure of the nucleus • It is now known that the nucleus consists of
... In beta decay, a neutron within the unstable nucleus changes into a proton, with the emission of a fast-moving electron from with the nucleus (discussed in more detail in Key ...
... In beta decay, a neutron within the unstable nucleus changes into a proton, with the emission of a fast-moving electron from with the nucleus (discussed in more detail in Key ...
ppt - Fusion Technology Institute
... But, the free space approximation is not accurate for the conditions involved. The DD-reaction yield can be orders of magnitude higher than predicted by extrapolation of the standard (free space) DD-reaction cross-section to lower deuteron energies. These enhancement (non-linear) effects came from a ...
... But, the free space approximation is not accurate for the conditions involved. The DD-reaction yield can be orders of magnitude higher than predicted by extrapolation of the standard (free space) DD-reaction cross-section to lower deuteron energies. These enhancement (non-linear) effects came from a ...
Star Factories: Nuclear Fusion and the Creation of the Elements
... table) then where do all the gold, silver, lead, uranium, etc... come from? ...
... table) then where do all the gold, silver, lead, uranium, etc... come from? ...
The Sun: Our Star (Chapter 14) The source of the Sun`s energy has
... The source of the Sun’s energy has long been a mystery, especially since the great distance between Earth and the Sun was first measured. Geologists argued that Earth’s geology needed 100s of millions of years to form, and physicists argued that no energy source could make the Sun shine for that lon ...
... The source of the Sun’s energy has long been a mystery, especially since the great distance between Earth and the Sun was first measured. Geologists argued that Earth’s geology needed 100s of millions of years to form, and physicists argued that no energy source could make the Sun shine for that lon ...
Star Cycle [Recovered]
... When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 times the mass of the ______ hydrogen can do this with no problem: they burn _____________, helium carbon and then _____ ...
... When all of the __________ hydrogen in the central regions is converted to helium, the star will begin to “burn” carbon helium into _______________. sun Stars heavier than about 5 times the mass of the ______ hydrogen can do this with no problem: they burn _____________, helium carbon and then _____ ...
The Interior Structure of Neutron Stars
... ->More energetically favourable for neutrons to form outside the nucleus. This is because we have reached the ρ where the highest occupied neutron energy level is just at the neutron Fermi energy. As ρ increases further more neutrons “drip” free of nuclei & we get heavy nuclei in a neutron and elect ...
... ->More energetically favourable for neutrons to form outside the nucleus. This is because we have reached the ρ where the highest occupied neutron energy level is just at the neutron Fermi energy. As ρ increases further more neutrons “drip” free of nuclei & we get heavy nuclei in a neutron and elect ...
Sources of energy and the origin of the chemical elements
... and small (relative to the Sun) star is called a White Dwarf. Stars with M< 0.4 M¤ will not become red giants because they do not become hot enough for He burning, but their lifetimes will be longer than the present age of the Universe. Typical C,O white dwarf specs: • mass of about 1 M¤ (on aver ...
... and small (relative to the Sun) star is called a White Dwarf. Stars with M< 0.4 M¤ will not become red giants because they do not become hot enough for He burning, but their lifetimes will be longer than the present age of the Universe. Typical C,O white dwarf specs: • mass of about 1 M¤ (on aver ...
Name: Period: ______ Date: Fission and Fusion Simulations Fission
... 12. How much power is generated (look at the graph to the right. You don’t have to come up with a number…describe)? ...
... 12. How much power is generated (look at the graph to the right. You don’t have to come up with a number…describe)? ...
(1) and
... Kinematic energy (=1/2Mv2) of Ia and CC SN are ~1051 erg. A large fraction should be converted to the thermal energy: kT = 3mv2/16 However observed thermal energy (kTe) is ~1049 erg This large missing energy would be contained in protons and other ions (the ion temperature kTi). But, no evidence is ...
... Kinematic energy (=1/2Mv2) of Ia and CC SN are ~1051 erg. A large fraction should be converted to the thermal energy: kT = 3mv2/16 However observed thermal energy (kTe) is ~1049 erg This large missing energy would be contained in protons and other ions (the ion temperature kTi). But, no evidence is ...
Stellar Nucleosynthesis
... • Great triumphs of 20th century physics – Discovery that sun, stars are mostly H – Explanation of nuclear fusion reactions powering sun • Nuclear Binding Energy • Quantum mechanics • Weak interaction ( beta decay) ...
... • Great triumphs of 20th century physics – Discovery that sun, stars are mostly H – Explanation of nuclear fusion reactions powering sun • Nuclear Binding Energy • Quantum mechanics • Weak interaction ( beta decay) ...
Where Did the Elements Come From?
... change one atom into another. • This cannot be accomplished in ordinary chemical reactions. • The first transmutation to be documented was that of nitrogen becoming oxygen when struck by an alpha particle and adding a proton to the nitrogen atom. ...
... change one atom into another. • This cannot be accomplished in ordinary chemical reactions. • The first transmutation to be documented was that of nitrogen becoming oxygen when struck by an alpha particle and adding a proton to the nitrogen atom. ...
Homework 2 key: Radiation processes, Larmor formula
... (a) What fraction of the star's radiation is capable of ionizing neutral hydrogen? Plot the Planck function vs. frequency; indicate the region of ionizing photons with a vertical line (use the 'marker' option in MathCAD plots). ...
... (a) What fraction of the star's radiation is capable of ionizing neutral hydrogen? Plot the Planck function vs. frequency; indicate the region of ionizing photons with a vertical line (use the 'marker' option in MathCAD plots). ...
The following slide show is a compilation of slides from... have been produced by different members of the fusion and...
... which is emitted when two light nuclei combine to form a single more stable nuclei. The sun and stars derive their energy from fusion. ...
... which is emitted when two light nuclei combine to form a single more stable nuclei. The sun and stars derive their energy from fusion. ...
regan-kent-25nov09a
... • Gold has 79 protons (i.e. Z=79) • Start with Z=78 protons (i.e. Platinum) • Specifically 196Pt ( Pt = Z=78, N=196-78=118) • Reaction is 196Pt + neutron to make 197Pt • 197Pt is radioactive and ‘beta-decays’ to make ...
... • Gold has 79 protons (i.e. Z=79) • Start with Z=78 protons (i.e. Platinum) • Specifically 196Pt ( Pt = Z=78, N=196-78=118) • Reaction is 196Pt + neutron to make 197Pt • 197Pt is radioactive and ‘beta-decays’ to make ...
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.