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Related Concept Videos

Nuclear Fusion02:45

Nuclear Fusion

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The process of converting very light nuclei into heavier nuclei is also accompanied by the conversion of mass into large amounts of energy, a process called fusion. The principal source of energy in the sun is a net fusion reaction in which four hydrogen nuclei fuse and ultimately produce one helium nucleus and two positrons.
A helium nucleus has a mass that is 0.7% less than that of four hydrogen nuclei; this lost mass is converted into energy during the fusion. This reaction produces about...
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Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

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In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
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Nuclear Fission02:50

Nuclear Fission

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Many heavier elements with smaller binding energies per nucleon can decompose into more stable elements that have intermediate mass numbers and larger binding energies per nucleon—that is, mass numbers and binding energies per nucleon that are closer to the “peak” of the binding energy graph near 56. Sometimes neutrons are also produced. This decomposition of a large nucleus into smaller pieces is called fission. The breaking is rather random with the formation of a large...
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Nuclear Stability03:18

Nuclear Stability

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Protons and neutrons, collectively called nucleons, are packed together tightly in a nucleus. With a radius of about 10−15 meters, a nucleus is quite small compared to the radius of the entire atom, which is about 10−10 meters. Nuclei are extremely dense compared to bulk matter, averaging 1.8 × 1014 grams per cubic centimeter. If the earth’s density were equal to the average nuclear density, the earth’s radius would be only about 200 meters.
To hold positively charged protons together...
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Atomic Nuclei: Nuclear Spin State Population Distribution01:14

Atomic Nuclei: Nuclear Spin State Population Distribution

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Near absolute zero temperatures, in the presence of a magnetic field, the majority of nuclei prefer the lower energy spin-up state to the higher energy spin-down state. As temperatures increase, the energy from thermal collisions distributes the spins more equally between the two states. The Boltzmann distribution equation gives the ratio of the number of spins predicted in the spin −½ (N−) and spin +½ (N+) states.
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Nuclear Transmutation03:20

Nuclear Transmutation

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Nuclear transmutation is the conversion of one nuclide into another. It can occur by the radioactive decay of a nucleus, or the reaction of a nucleus with another particle. The first manmade nucleus was produced in Ernest Rutherford’s laboratory in 1919 by a transmutation reaction, the bombardment of one type of nuclei with other nuclei or with neutrons. Rutherford bombarded nitrogen-14 atoms with high-speed α particles from a natural radioactive isotope of radium and observed...
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Diffuse neutrino background from past core collapse supernovae.

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Detecting the diffuse supernova neutrino background (DSNB) is crucial for understanding core collapse supernovae and neutrino physics. Future experiments promise DSNB detection, offering insights into cosmic events and fundamental physics.

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Area of Science:

  • Cosmic explosions and particle physics.
  • High-energy astrophysics and neutrino physics.

Background:

  • Core collapse supernovae are powerful cosmic explosions emitting thermal neutrinos.
  • These neutrinos form the diffuse supernova neutrino background (DSNB), a significant radiation background.
  • DSNB detection offers insights into supernova modeling, neutrino physics, and cosmic rates.

Approach:

  • Reviewing key DSNB calculation ingredients.
  • Discussing potential insights from DSNB detection, including black hole formation and non-standard neutrino interactions.
  • Providing an overview of current neutrino experiments poised for DSNB detection.

Key Points:

  • DSNB detection is a major goal in astrophysics and particle physics.
  • Understanding DSNB aids in modeling supernovae and neutrino properties.
  • Future neutrino experiments are nearing DSNB detection capability.

Conclusions:

  • DSNB detection promises significant advancements in understanding the Universe.
  • This field holds potential for breakthrough discoveries in fundamental physics.
  • Continued research and experimental efforts are vital for unlocking DSNB's secrets.