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相关概念视频

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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相关实验视频

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

孤立恒星形成:从云的形成到核心的崩.

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
概括

恒星形成是一个基本的天体物理学问题. 目前的模型很难解释在恒星形成区域中对流和磁场的观测,尽管技术和计算能力先进.

科学领域:

  • 天体物理学 天体物理学
  • 星星形成的形成
  • 宇宙物理学 宇宙物理学

背景情况:

  • 恒星形成是一个基本的天体物理问题,对于理解星系和太阳系演变至关重要.
  • 关键的物理过程涉及流,部分电离介质与不均的磁场.
  • 目前正在进行的辩论重点是流衰变时间以及磁场和流的相互作用.

研究的目的:

  • 为了研究控制恒星形成的复杂物理过程.
  • 将理论模型与有关流和磁场的观测数据相协调.
  • 推进我们对恒星进化的时间尺度和机制的理解.

主要方法:

  • 利用毫米波摄像机的先进观测数据来分析温度和密度概况.
  • 对崩和崩前物体的寿命进行统计计算.
  • 开发复杂的计算模型,包括磁性和流效应.

主要成果:

  • 技术进步使得可以详细观察恒星形成区域.
  • 增加的计算能力有助于更复杂的物理过程的建模.
  • 没有一个单一的当前模型能够准确地复制所有观察到的现象.

结论:

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

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

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Last Updated: Jul 19, 2026

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

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

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  • 恒星形成仍然是天体物理学中一个复杂的挑战.
  • 目前的模型不足以完全解释观测到的恒星形成过程.
  • 需要进一步的研究才能有效地整合磁场,流和观测数据.