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Atomic Structure01:33

Atomic Structure

All matter is composed of atoms, the smallest individual units of elements. Each atom is made up of three subatomic particles: protons, neutrons, and electrons. Together, these three particles account for the mass and the charge of an atom.The History of Atomic TheoryThe first person to propose that everything on Earth is made up of tiny particles was the Greek philosopher Democritus, around 450 B.C. He used the term atomos, Greek for “indivisible,” from which the modern term “atom” is derived.
Atomic Orbitals02:44

Atomic Orbitals

An atomic orbital represents the three-dimensional regions in an atom where an electron has the highest probability to reside. The radial distribution function indicates the total probability of finding an electron within the thin shell at a distance r from the nucleus. The atomic orbitals have distinct shapes which are determined by l, the angular momentum quantum number. The orbitals are often drawn with a boundary surface, enclosing densest regions of the cloud.
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 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...
Atomic Structure01:17

Atomic Structure

The Greek philosopher Democritus proposed that everything on Earth is made up of tiny particles called atomos, Greek for "indivisible," from which the modern term "atom" is derived. In the 19th century, John Dalton proposed the atomic theory that is still largely correct today. He put forth five postulates to explain how atoms made up the world around us. (1) All matter is composed of infinitely small particles or atoms. (2) All atoms of a given element are identical to one another and (3) are...

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関連する実験動画

Updated: Jul 19, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
06:04

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 15, 2013

孤立した恒星形成:雲の形成から核の崩壊まで

Derek Ward-Thompson1

  • 1Department of Physics and Astronomy, Cardiff University, Post Office Box 913, Cardiff, UK. D.Ward-Thompson@astro.cf.ac.uk

Science (New York, N.Y.)
|January 5, 2002
PubMed
まとめ

恒星形成は天体物理学における根本的な問題である. 現在のモデルは,高度な技術とコンピューティング能力にもかかわらず,星形成地域における乱流と磁場の観測を説明するために苦労しています.

科学分野:

  • 天体物理学 天体物理学
  • スター・フォーメーション
  • 宇宙物理学 宇宙物理学

背景:

  • 恒星形成は天体物理学の根本的な問題であり,銀河系と太陽系の進化を理解する上で極めて重要です.
  • 重要な物理的プロセスは,不均一な磁場を持つ乱流性,部分的にイオン化された媒体を含む.
  • 現在進行中の議論は,乱流の崩壊時間,磁場と乱流の相互作用に焦点を当てています.

研究 の 目的:

  • 恒星形成を制御する複雑な物理的プロセスを調査する.
  • 渦巻と磁場に関する観測データと理論モデルを調和させる.
  • 恒星の進化の時間スケールとメカニズムに関する理解を深めること.

主な方法:

  • ミリメートル波カメラからの高度な観測データを活用して,温度と密度プロフィールを分析します.
  • 崩壊する物体と崩壊前の物体の寿命に関する統計的計算を行う.
  • 磁気および乱流効果を含む複雑な計算モデルを開発する.

主要な成果:

  • 技術の進歩により,恒星形成地域の詳細な観測が可能になりました.
  • コンピューティング能力の向上により,物理的なプロセスのより洗練されたモデリングが容易になります.

さらに関連する動画

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
09:44

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

Synthesis of Single-Crystalline Core-Shell Metal-Organic Frameworks
05:26

Synthesis of Single-Crystalline Core-Shell Metal-Organic Frameworks

Published on: February 10, 2023

関連する実験動画

Last Updated: Jul 19, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
06:04

Simulation of the Planetary Interior Differentiation Processes in the Laboratory

Published on: November 15, 2013

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System
09:44

Laboratory Drop Towers for the Experimental Simulation of Dust-aggregate Collisions in the Early Solar System

Published on: June 5, 2014

Synthesis of Single-Crystalline Core-Shell Metal-Organic Frameworks
05:26

Synthesis of Single-Crystalline Core-Shell Metal-Organic Frameworks

Published on: February 10, 2023

  • 観測されたすべての現象を正確に再現する単一の現在のモデルはありません.
  • 結論:

    • 恒星形成は,天体物理学における複雑な課題であり続けている.
    • 現在のモデルは,観測された恒星形成プロセスを完全に説明するのに不十分です.
    • 磁場,乱流,観測データを効果的に統合するためにさらなる研究が必要である.