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Related Concept Videos

Nuclear Stability03:18

Nuclear Stability

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 in the...
Nuclear Fusion02:45

Nuclear Fusion

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...
Conditions on Early Earth02:06

Conditions on Early Earth

Around 4 billion years ago, oceans began to condense on earth while volcanic eruptions released nitrogen, carbon dioxide, methane, ammonia, and hydrogen into the primordial atmosphere. However, organisms with the characteristics of life were not initially present on earth. Scientists have used experimentation to determine how organisms evolved that could grow, reproduce, and maintain an internal environment.
Conditions on Early Earth02:06

Conditions on Early Earth

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Nuclear Fission02:50

Nuclear Fission

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 number of different...
Schwarzschild Radius and Event Horizon01:21

Schwarzschild Radius and Event Horizon

No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape velocity with the...

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Related Experiment Video

Updated: May 18, 2026

Laser-heating and Radiance Spectrometry for the Study of Nuclear Materials in Conditions Simulating a Nuclear Power Plant Accident
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Laser-heating and Radiance Spectrometry for the Study of Nuclear Materials in Conditions Simulating a Nuclear Power Plant Accident

Published on: December 14, 2017

Critical conditions for core-collapse supernovae.

Uri Keshet1, Shmuel Balberg

  • 1Physics Department, Ben-Gurion University of the Negev, Be'er-Sheva 84105, Israel. ukeshet@bgu.ac.il

Physical Review Letters
|September 26, 2012
PubMed
Summary

Supernova explosions occur when neutrino luminosity surpasses a critical threshold, overwhelming hydrostatic pressure. This critical point depends on proto-neutron star mass and neutrino temperature, guiding supernova models.

Area of Science:

  • Astrophysics
  • Nuclear Physics
  • Computational Physics

Background:

  • Core-collapse supernovae are approximated by accretion onto proto-neutron stars (PNS).
  • Steady-state solutions for accretion are crucial for understanding supernova dynamics.
  • Neutrino-driven winds and explosions are key phenomena in stellar evolution.

Purpose of the Study:

  • To analytically determine the critical conditions for supernova explosion onset.
  • To investigate the relationship between neutrino luminosity, PNS properties, and explosion dynamics.
  • To provide a theoretical framework for interpreting numerical supernova simulations.

Main Methods:

  • Analytical derivation of critical neutrino luminosity (L(c)) and shock radius (R).
  • Analysis of steady-state accretion solutions onto a proto-neutron star.

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  • Comparison of analytical results with existing numerical simulation data.

    • Main Results:

    • A critical neutrino luminosity (L(c)) is identified, above which explosion is favored.
    • The critical luminosity scales as L(c) ∝ M^2 T^2 (with logarithmic corrections).
    • The optimal shock radius scales as R ∝ M/T, where M is PNS mass and T is neutrino temperature.

    Conclusions:

    • The breakdown of steady-state accretion solutions provides a pathway to supernova explosions.
    • Analytical predictions for L(c) and R align with numerical supernova simulations.
    • The near-critical accretion flow can be modeled as a ballistic shell over an isothermal layer.