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関連する概念動画

Detection of Black Holes01:10

Detection of Black Holes

1.7K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
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Atomic Nuclei: Nuclear Magnetic Moment00:59

Atomic Nuclei: Nuclear Magnetic Moment

3.0K
All atomic nuclei are positively charged. When they have a nonzero spin, they behave like rotating charges. As a consequence of their charge and spin, these nuclei generate a magnetic field (B). This, in turn, gives rise to a magnetic moment (μ), which is randomly oriented in the absence of an external magnetic field. When an external magnetic field (B0) is applied, the magnetic moment vectors can align with the field or against it in 2 + 1 orientations. A hydrogen nucleus, which is just a...
3.0K
Atomic Nuclei: Magnetic Resonance01:05

Atomic Nuclei: Magnetic Resonance

1.2K
The number of nuclear spins aligned in the lower energy state is slightly greater than those in the higher energy state. In the presence of an external magnetic field, as the spins precess at the Larmor frequency, the excess population results in a net magnetization oriented along the z axis. When a pulse or a short burst of radio waves at the Larmor frequency is applied along the x axis, the coupling of frequencies causes resonance and flips the nuclear spins of the excess population from the...
1.2K
Atomic Nuclei: Nuclear Relaxation Processes01:23

Atomic Nuclei: Nuclear Relaxation Processes

1.1K
In the absence of an external magnetic field, nuclear spin states are degenerate and randomly oriented. When a magnetic field is applied, the spins begin to precess and orient themselves along (lower energy) or against (higher energy) the direction of the field. At equilibrium, a slight excess population of spins exists in the lower energy state. Because the direction of the magnetic field is fixed as the z-axis,  the precessing magnetic moments are randomly oriented around the z-axis.
1.1K
Magnetic Fields01:27

Magnetic Fields

6.0K
A moving charge or a current creates a magnetic field in the surrounding space, in addition to its electric field. The magnetic field exerts a force on any other moving charge or current that is present in the field. Like an electric field, the magnetic field is also a vector field. At any position, the direction of the magnetic field is defined as the direction in which the north pole of a compass needle points.
A magnetic field is defined by the force that a charged particle experiences...
6.0K
Magnetic Field Lines01:19

Magnetic Field Lines

5.4K
The representation of magnetic fields by magnetic field lines is very useful in visualizing the strength and direction of the magnetic field. Each of the magnetic field lines forms a closed loop. The field lines emerge from the north pole (N), loop around to the south pole (S), and continue through the bar magnet back to the north pole.
Magnetic field lines follow several hard-and-fast rules:
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関連する実験動画

Updated: May 1, 2026

High-Sensitivity Nuclear Magnetic Resonance at Giga-Pascal Pressures: A New Tool for Probing Electronic and Chemical Properties of Condensed Matter under Extreme Conditions
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High-Sensitivity Nuclear Magnetic Resonance at Giga-Pascal Pressures: A New Tool for Probing Electronic and Chemical Properties of Condensed Matter under Extreme Conditions

Published on: October 10, 2014

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普通の銀河の強い磁場は,赤道偏移が高く,正常な銀河では強い磁場がある.

Martin L Bernet1, Francesco Miniati, Simon J Lilly

  • 1Department of Physics, ETH Zürich, Wolfgang-Pauli-Strasse 16, CH-8093 Zürich, Switzerland.

Nature
|July 18, 2008
PubMed
まとめ

初期の銀河は,今日の銀河に匹敵する強力な磁場を持っていた. この研究は,これらの強力な銀河磁場を初期の宇宙の正常な銀河と結びつけ,それらの起源と時間尺度に関する以前の仮定に異議を唱えます.

科学分野:

  • 天文学と天体物理学について
  • コスミック・マグネティズム (宇宙磁気) とは
  • 銀河の進化 銀河の進化 銀河の進化

背景:

  • 銀河の磁場の起源と増幅は,未だに十分に理解されていない.
  • ダイナモ効果は,宇宙時間におけるシード磁場を拡大するメカニズムであると考えられています.
  • 以前の研究では,初期の銀河と現在の銀河の磁場強度が比較可能であることが示唆されていたが,その分布は不明であった.

研究 の 目的:

  • 初期の宇宙における磁場の起源と分布を調査する.
  • 高磁場強度が正常な銀河や特定のクワザール環境と関連しているかどうかを判断する.
  • ダイナモ効果による磁場増幅の時間スケールを制限する.

主な方法:

  • 遠いクワザールの高解像度スペクトルの分析.
  • 磁場強度を追跡するための回転量 (RMs) の測定.
  • 銀河のハロ環境を示すMg II吸収線とRMの相関. 銀河のハロ環境を示す.

主要な成果:

  • 高回転度測定とクワザールにおける強いMg II吸収線との間に明確な関連性が見られた.
  • Mg IIの吸収線は,クエザールまでの視線に沿って,正常な銀河のハローを追跡する.

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Optimized Setup and Protocol for Magnetic Domain Imaging with In Situ Hysteresis Measurement

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Optimizing Magnetic Force Microscopy Resolution and Sensitivity to Visualize Nanoscale Magnetic Domains
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Optimizing Magnetic Force Microscopy Resolution and Sensitivity to Visualize Nanoscale Magnetic Domains

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Last Updated: May 1, 2026

High-Sensitivity Nuclear Magnetic Resonance at Giga-Pascal Pressures: A New Tool for Probing Electronic and Chemical Properties of Condensed Matter under Extreme Conditions
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High-Sensitivity Nuclear Magnetic Resonance at Giga-Pascal Pressures: A New Tool for Probing Electronic and Chemical Properties of Condensed Matter under Extreme Conditions

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Optimized Setup and Protocol for Magnetic Domain Imaging with In Situ Hysteresis Measurement
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Optimized Setup and Protocol for Magnetic Domain Imaging with In Situ Hysteresis Measurement

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Optimizing Magnetic Force Microscopy Resolution and Sensitivity to Visualize Nanoscale Magnetic Domains
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  • これは,宇宙が現在の年齢の3分の1しかなかったときに,強い,組織化された磁場が正常な銀河に存在していたことを示しています.

    • 結論:

    • 重要な強さの有組織磁場は,初期の宇宙の通常の銀河と関連しています.
    • この発見は,そのような場は後に発達するか,異常な銀河環境に限定されているという考えに異議を唱える.
    • この結果は,銀河ダイナモの作用と宇宙磁力の進化のモデルに重要な制約を与える.