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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.
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The probability of having two carbon-13 atoms next to each other is negligible because of the low natural abundance of carbon-13. Consequently, peak splitting due to carbon-carbon spin-spin coupling is not observed in spectra. However, protons up to three sigma bonds away split the carbon signal according to the n+1 rule, resulting in complicated spectra.
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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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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.
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There are two ways to determine the amount of heat involved in a chemical change: measure it experimentally, or calculate it from other experimentally determined enthalpy changes. Some reactions are difficult, if not impossible, to investigate and make accurate measurements for experimentally. And even when a reaction is not hard to perform or measure, it is convenient to be able to determine the heat involved in a reaction without having to perform an experiment.
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Following the work of Ernest Rutherford and his colleagues in the early twentieth century, the picture of atoms consisting of tiny dense nuclei surrounded by lighter and even tinier electrons continually moving about the nucleus was well established. This picture was called the planetary model since it pictured the atom as a miniature “solar system” with the electrons orbiting the nucleus like planets orbiting the sun. The simplest atom is hydrogen, consisting of a single proton as...
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Extending the Hoyle-State Paradigm to ^{12}C+^{12}C Fusion.

P Adsley1,2, M Heine3,4, D G Jenkins5,6,7

  • 1School of Physics, University of the Witwatersrand, Johannesburg 2050, South Africa.

Physical Review Letters
|September 16, 2022
PubMed
Summary
This summary is machine-generated.

Researchers identified new ^{12}C+^{12}C cluster states in ^{24}Mg, potentially clarifying carbon burning in stars and supernovae. These findings offer updated ^{12}C+^{12}C fusion reaction rates for astrophysical models.

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Area of Science:

  • Nuclear Astrophysics
  • Stellar Evolution
  • Exotic Nuclear Clusters

Background:

  • Carbon burning is crucial for massive stars, Type Ia supernovae, and X-ray superbursts.
  • Directly measuring the ^{12}C+^{12}C fusion cross section is difficult due to sub-barrier resonances.

Purpose of the Study:

  • Investigate ^{12}C+^{12}C cluster structures near the Coulomb barrier.
  • Determine the impact of newly identified states on ^{12}C+^{12}C fusion rates.

Main Methods:

  • Studied the ^{24}Mg(α,α')^{24}Mg reaction.
  • Identified 0+ states in ^{24}Mg near the ^{12}C+^{12}C threshold.
  • Analyzed decay modes, particularly to ^{20}Ne(ground state)+α.

Main Results:

  • Discovered several 0+ states in ^{24}Mg with potential dominant ^{12}C+^{12}C cluster configurations.
  • Observed decay patterns not seen in ^{20}Ne(α,α0)^{20}Ne scattering, supporting the cluster hypothesis.
  • These states may significantly influence sub-barrier ^{12}C+^{12}C fusion.

Conclusions:

  • The identified ^{12}C+^{12}C cluster states offer new insights into stellar nucleosynthesis.
  • Updated ^{12}C+^{12}C fusion reaction rates are provided, improving astrophysical models.
  • Analogous to the Hoyle state's role in helium burning, these states could be key in carbon burning.