Where Did the Elements Come From?
... • Not all elements are found on Earth – some were found in the spectra of the stars • Synthetic elements have been created by man ...
... • Not all elements are found on Earth – some were found in the spectra of the stars • Synthetic elements have been created by man ...
AQA - Rev Checklist PHY
... dangers of their emissions Radioactive substances emit radiation from the nuclei of their atoms all the time. These nuclear radiations can be very useful but may also be very dangerous. It is important to understand the properties of different types of nuclear radiation. To understand what happens ...
... dangers of their emissions Radioactive substances emit radiation from the nuclei of their atoms all the time. These nuclear radiations can be very useful but may also be very dangerous. It is important to understand the properties of different types of nuclear radiation. To understand what happens ...
Teaching STEM through `Inside the Atom`
... wall poster describing the “big questions” about our Universe that scientists are trying to answer and how the amazing LHC will help them do so. Inside the atom: nuclear activity in the UK. A full-colour A5 leaflet that opens out into an A2 double-sided wall poster describing the activity of the nuc ...
... wall poster describing the “big questions” about our Universe that scientists are trying to answer and how the amazing LHC will help them do so. Inside the atom: nuclear activity in the UK. A full-colour A5 leaflet that opens out into an A2 double-sided wall poster describing the activity of the nuc ...
Star formation and Evolution
... + 4He --> 16O + photon (for 500M K) 16O + 4He --> 20Ne + photon (for 500M K) 16O + 16O --> 32S + photon (for 1 billion K) And so on until iron is produced, Reactions to heavier elements go faster and faster : creating oxygen , Neon, Magnesium takes 1000 years, production of sulfur takes few days. ...
... + 4He --> 16O + photon (for 500M K) 16O + 4He --> 20Ne + photon (for 500M K) 16O + 16O --> 32S + photon (for 1 billion K) And so on until iron is produced, Reactions to heavier elements go faster and faster : creating oxygen , Neon, Magnesium takes 1000 years, production of sulfur takes few days. ...
Presentation - Copernicus.org
... tracked before work [1] in which possibility of acceleration of particles in electric fields of a thundercloud up to the energies sufficient for initiation of nuclear reaction is discussed. During recent decades increase of neutron flux during of thunderstorm activity, both in orbital experiments, a ...
... tracked before work [1] in which possibility of acceleration of particles in electric fields of a thundercloud up to the energies sufficient for initiation of nuclear reaction is discussed. During recent decades increase of neutron flux during of thunderstorm activity, both in orbital experiments, a ...
A high-power liquid-lithium target for production of keV
... for production of keV-energy neutrons Research workshop on Nuclear Structure and Astrophysics with Radioactive Beams ...
... for production of keV-energy neutrons Research workshop on Nuclear Structure and Astrophysics with Radioactive Beams ...
Astronomy 112: The Physics of Stars Class 17 Notes: Core Collapse
... it has no nuclear reactions, so it becomes isothermal. If it gets to be more than roughly 10% of the stellar mass, it will exceed the Schönberg-Chandrasekhar limit and begin contracting dynamically. If it becomes degenerate, degeneracy pressure can slow the collapse, but if the core exceeds the Cha ...
... it has no nuclear reactions, so it becomes isothermal. If it gets to be more than roughly 10% of the stellar mass, it will exceed the Schönberg-Chandrasekhar limit and begin contracting dynamically. If it becomes degenerate, degeneracy pressure can slow the collapse, but if the core exceeds the Cha ...
Atoms and the Periodic Table Atoms and Elements
... orbital can be calculated. Around every nucleus, their are shells of orbitals for the electrons. Three kinds of electron orbitals are shown below. The pictures of orbitals represent a mathematical function showing 90% probability of finding an electron in the area enclosed by the shape. An s orbital ...
... orbital can be calculated. Around every nucleus, their are shells of orbitals for the electrons. Three kinds of electron orbitals are shown below. The pictures of orbitals represent a mathematical function showing 90% probability of finding an electron in the area enclosed by the shape. An s orbital ...
Physics 9 Fall 2010 - faculty.ucmerced.edu
... (b) Because all of the resistors are identical, the points c and d are at the same potential. This means that if we connected a wire between points c and d, then no current would flow along it. Thus, if we added a resistor between these two points, it would do nothing, and so the equivalent resistan ...
... (b) Because all of the resistors are identical, the points c and d are at the same potential. This means that if we connected a wire between points c and d, then no current would flow along it. Thus, if we added a resistor between these two points, it would do nothing, and so the equivalent resistan ...
Physics 12
... b. How much force is required to make the 34 μC move as indicated above? 6. An alpha particle (4 x mass of a proton and twice its charge) is travelling at 2.4 x 106 m/s when it is 8.0 m away from a 7.6 x 10-5 C positive charge. What is the alpha particle’s distance of closest approach (how close can ...
... b. How much force is required to make the 34 μC move as indicated above? 6. An alpha particle (4 x mass of a proton and twice its charge) is travelling at 2.4 x 106 m/s when it is 8.0 m away from a 7.6 x 10-5 C positive charge. What is the alpha particle’s distance of closest approach (how close can ...
Neutrons and Protons
... 5.06x10-29 kg of mass released as energy when protons & neutrons combined to form Helium nucleus. This is the ‘binding’ energy of the nucleus. ...
... 5.06x10-29 kg of mass released as energy when protons & neutrons combined to form Helium nucleus. This is the ‘binding’ energy of the nucleus. ...
50 Sure shot Questions ( XII
... binding energy per nucleon, nucleons are tightly bound. This implies that energy will be released in the process which justifies the energy release in fission reaction. Nuclear fusion: When two light nuclei (A<10) are combined to form a heavier nuclei, the binding energy of the fused heavier nuclei ...
... binding energy per nucleon, nucleons are tightly bound. This implies that energy will be released in the process which justifies the energy release in fission reaction. Nuclear fusion: When two light nuclei (A<10) are combined to form a heavier nuclei, the binding energy of the fused heavier nuclei ...
doc - Jnoodle
... between the shells can be sent out as a photon photon = "particle" of light or other electromagnetic radiation. The energy of the photon is: E = hf in an emission spectrum : since there are only certain possibilities to fall in an atom (shell 2 -> 1, 3 -> 1, 4 -> 1 , ..., 3 - >2, 4 -> 2, ...) only c ...
... between the shells can be sent out as a photon photon = "particle" of light or other electromagnetic radiation. The energy of the photon is: E = hf in an emission spectrum : since there are only certain possibilities to fall in an atom (shell 2 -> 1, 3 -> 1, 4 -> 1 , ..., 3 - >2, 4 -> 2, ...) only c ...
Nuclear drip line
In nuclear physics, the boundaries for nuclear particle-stability are called drip lines. Atomic nuclei contain both protons and neutrons—the number of protons defines the identity of that element (ie, carbon always has 6 protons), but the number of neutrons within that element may vary (carbon-12 and its isotope carbon-13, for example). The number of isotopes each element may have is visually represented by plotting boxes, each of which represents a unique nuclear species, on a graph with the number of neutrons increasing on the abscissa (X axis) and number of protons increasing along the ordinate (Y axis). The resulting chart is commonly referred to as the table of nuclides, and is to nuclear physics what the periodic table of the elements is to chemistry.An arbitrary combination of protons and neutrons does not necessarily yield a stable nucleus. One can think of moving up and/or to the right across the nuclear chart by adding one type of nucleon (i.e. a proton or neutron, both called nucleons) to a given nucleus. However, adding nucleons one at a time to a given nucleus will eventually lead to a newly formed nucleus that immediately decays by emitting a proton (or neutron). Colloquially speaking, the nucleon has 'leaked' or 'dripped' out of the nucleus, hence giving rise to the term ""drip line"". Drip lines are defined for protons, neutrons, and alpha particles, and these all play important roles in nuclear physics. The nucleon drip lines are at the extreme of the proton-to-neutron ratio: at p:n ratios at or beyond the driplines, no stable nuclei can exist. The location of the neutron drip line is not well known for most of the nuclear chart, whereas the proton and alpha driplines have been measured for a wide range of elements. The nucleons drip out of such unstable nuclei for the same reason that water drips from a leaking faucet: in the water case, there is a lower potential available that is great enough to overcome surface tension and so produces a droplet; in the case of nuclei, the emission of a particle from a nucleus, against the strong nuclear force, leaves the total potential of the nucleus and the emitted particle in a lower state. Because nucleons are quantized, only integer values are plotted on the table of isotopes; this indicates that the drip line is not linear but instead looks like a step function up close.