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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.
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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...
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...
Nuclear Transmutation03:20

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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 protons being...
Atomic Nuclei: Nuclear Spin State Population Distribution01:14

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Updated: Jun 16, 2026

Measurement and Analysis of Atomic Hydrogen and Diatomic Molecular AlO, C2, CN, and TiO Spectra Following Laser-induced Optical Breakdown
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Measurement and Analysis of Atomic Hydrogen and Diatomic Molecular AlO, C2, CN, and TiO Spectra Following Laser-induced Optical Breakdown

Published on: February 14, 2014

超新星2007biは,ペア不安定性爆発として登場する.

A Gal-Yam1, P Mazzali, E O Ofek

  • 1Benoziyo Center for Astrophysics, Faculty of Physics, The Weizmann Institute of Science, Rehovot 76100, Israel. avishay.gal-yam@weizmann.ac.il

Nature
|December 4, 2009
PubMed
まとめ
この要約は機械生成です。

超大質量の恒星は,ペア不安定性超新星として爆発する可能性があります. 超新星SN 2007biの観測はこれを確認し,巨大な星の核と合成された放射性ニッケルを明らかにした.

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関連する実験動画

Last Updated: Jun 16, 2026

Measurement and Analysis of Atomic Hydrogen and Diatomic Molecular AlO, C2, CN, and TiO Spectra Following Laser-induced Optical Breakdown
09:40

Measurement and Analysis of Atomic Hydrogen and Diatomic Molecular AlO, C2, CN, and TiO Spectra Following Laser-induced Optical Breakdown

Published on: February 14, 2014

Magnetically Induced Rotating Rayleigh-Taylor Instability
06:42

Magnetically Induced Rotating Rayleigh-Taylor Instability

Published on: March 3, 2017

Coulomb Explosion Imaging as a Tool to Distinguish Between Stereoisomers
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Published on: August 18, 2017

科学分野:

  • 天文学と天体物理学について
  • 恒星の進化について
  • 超新星物理学 超新星物理学

背景:

  • 巨大な恒星 (10〜100太陽質量) は,鉄核崩壊の超新星として終わる.
  • 超大質量恒星 (>140太陽質量) は,電子・ポジトロン対の生成により,対不安定性超新星を経験することがあります.
  • 移行期恒星 (100-140太陽質量) は,両方の超新星タイプの特性を表す可能性があります.

研究 の 目的:

  • 超新星SN 2007biの性質を調査するために,明るく,ゆっくりと進化する物体.
  • ペア不安定性超新星に関する理論的予測を検証する.
  • 矮星銀河の極大質量星の存在を調査する.

主な方法:

  • 観測天文学は,超新星 SN 2007bi.を中心に研究しています.
  • 爆発した核の質量の推定.
  • 合成された放射性ニッケル-56.6の分析
  • ペア不安定性超新星の理論モデルとの比較.

主要な成果:

  • 超新星SN 2007biは,爆発した核の質量が太陽の質量約100倍であると推定されています.
  • 爆発中に放射性ニッケル-56の太陽質量3倍以上の物質が合成された.
  • 観測結果は,対不安定性超新星モデルと一致しています.

結論:

  • SN 2007biは,ペア不安定性超新星についての強力な証拠を提供します.
  • 矮星銀河は,非常に巨大な恒星を宿し,銀河の恒星質量制限を潜在的に超えている可能性があります.
  • これらの巨大な星は,宇宙で形成された最初の星と類似している可能性があります.