Near-Earth supernova - Wikipedia

In this activity, the behavioral objectives are: (1) the students will be able to estimate the composition of elements within a given population, and (2) the students should be able to determine what object the population represents based on the composition of the given population. This activity is allotted one class period for completion and discussion.

the term supernova nucleosynthesis is ..

This is the limit to what a star can do (the reason why is mentioned later).

The supernova is pointed by the arrow

The behavioral objectives for this activity include: (1) students will learn how white light can be separated into its various colors, (2) students will learn the mathematical relationships between wavelength, frequency, and energy of light, (3) students will learn how to solve for a variable by rearranging an algebraic equation, and (4) students will learn about the nature of light and the electromagnetic spectrum. After reading the article entitled "What is Electromagnetic Radiation?" the students will be able to use the following equations: c = Λf and E = hf to complete the worksheet entitled "Calculation Investigation". Using the aforementioned equations, the students will be able to solve for different variables with the proper units by rearranging the algebraic equations. The time allocated for this activity is one class period.

Scientists call this supernova nucleosynthesis.

The main activity for this unit will be for each cooperative learning group to prepare and present a fifteen minute power point presentation on a different aspect of the origin of the elements. After briefly presenting the basic foundations of the Big Bang theory and nucleosynthesis, each group will be assigned one of the following topics for their presentation: history of the Big Bang theory, stellar evolution, Big Bang nucleosynthesis, stellar nucleosynthesis, supernova nucleosynthesis, nuclear fusion reactions, and neutron capture reactions. The students will be escorted to the high school library where they will research their topics for two days using both written and electronic resources. The following two days each group will prepare their power point presentation. Presentation and discussion of their work will take place over the last few days of this unit.

Category:Supernovae - Wikipedia
08/08/2016 · What is Nucleosynthesis

Superluminous supernova - Wikipedia

Second, because of the breaking apart of the iron nuclei in the central core, there is a high concentration of neutrons (called the neutron flux) that are ejected from the core during the supernova.

What happens during Supernova nucleosynthesis as compared to nucleosynthesis …

27/11/2011 · What is Stellar Nucleosynthesis

The layers containing the heavy elements may be blown off by the supernova explosion, and provide the raw material of heavy elements in the distant hydrogen clouds which condense to form new stars.

Supernova r-process nucleosynthesis : Physics - reddit

Supernova nucleosynthesis; Cosmic ray spallation;

When the core temperature exceeds 100MK, helium nuclei begin to fuse to form carbon and oxygen. At this point non-relativistic degeneracy sets in, and the active life of the star has reached an end. The outer envelope has been shed out, and what remains is a hot, inert stellar core, called a white dwarf. It is very small and dense (the mass must be lower than 1.4 times the solar mass), and the size is very similar to the size of the Earth. All the results of stellar evolution become forever trapped within the white dwarf that begins to cool down to eventually become a dark cinder in the sky. For higher mass stars, however, the evolution does not end up there, but it continues to subsequent stages. There, at yet deeper levels, heavier elements are synthesized by the fusion of helium nuclei up to iron-56. Elements having mass numbers less than 56 and that are not multiples of 4 are produced in side reactions with neutrons. Moving in toward the core of the star helium is converted into carbon by the triple alpha process at 10 8 K. At a larger depth, the temperature increases to the point where carbon atoms will undergo fusion to produce neon at temperatures in the range of 10 9 K. As the depth (and temperature) of the star continues to increases neon will go on to form oxygen. Oxygen will fuse to form silicon, and silicon in turn will go on to form nickel. At this point the star is classified as a red giant and has been undergoing stellar evolution. Silicon will begin to burn at 4 x 10 9 K forming iron which cannot undergo any further stellar nucleosynthesis because of its high binding energies. A few elements having masses larger than 5 6Fe are formed through the equilibrium process. Eventually the fuel will be exhausted at which point energy production ceases, gravity causes the core to collapse, and the star undergoes a massive explosion, or type II supernova. The elements synthesized just prior to a supernova explosion would include: hydrogen, helium, carbon, oxygen, neon, magnesium, silicon, sulfur, chlorine, argon, potassium, calcium, titanium, vanadium, chromium, manganese, iron, cobalt, and nickel. (14, 15, 16, 17, 18, 19).