短期間のG-ray burst GRB 130603Bに関連した"キロノヴァ"です
N R Tanvir1, A J Levan, A S Fruchter
1Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK. nrt3@le.ac.uk
Nature
|August 6, 2013
まとめ
短時間のガンマ線爆発 (GRB) は,コンパクトなオブジェクトの合併と関連しています. GRB 130603Bの観測はキロノヴァを明らかにし,GRBの起源とr-プロセス要素の場所としての合併を確認しました.
科学分野:
- 天体物理学 天体物理学
- 核天体物理学 核天体物理学とは
- 宇宙ガンマ線爆発 (Cosmic Gamma-Ray Bursts) とは,宇宙のガンマ線が爆発したときに発生する現象です.
背景:
- 短時間ガンマ線爆発 (GRB) は,短い,激しい宇宙線の閃光です.
- 彼らの起源は議論されており,コンパクトオブジェクトの合併が主要な仮説である.
- 融合により,中性子に富んだ元素とキロノバが生成されると予測されている.
研究 の 目的:
- 短期間のGRBsの祖先モデルを確認するために.
- r-プロセス要素の起源を調査する.
- キロノヴァを合併の電磁対称物として識別する.
主な方法:
- GRB 130603B.の光学および近赤外線観測
- GRBの後に発生した一時的な放射の分析.
- 観測をキロノヴァの理論モデルと比較する.
主要な成果:
- GRB 130603B.を伴ったキロノヴァの有力な証拠
- 観測された放射は,放射性崩壊で動いているキロノヴァの予測と一致する.
- イベントのエネルギー分布は,近赤外線放射と一致しています.
結論:
- コンパクトオブジェクトの合併は,短期間のGRBの祖先として確認されています.
- これらの合併は,rプロセスの要素の生産のための重要なサイトです.
- キロノバは,重力波源の代替的な電磁気シグネチャを提供する.
さらに関連する動画
関連する概念動画
03:23Types of Radioactivity
The most common types of radioactivity are α decay, β decay, γ decay, neutron emission, and electron capture.
Alpha (α) decay is the emission of an α particle from the nucleus. For example, polonium-210 undergoes α decay:
Alpha (α) decay is the emission of an α particle from the nucleus. For example, polonium-210 undergoes α decay:
01:21Schwarzschild Radius and Event Horizon
No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape velocity with the...
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape velocity with the...
02:45Nuclear 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...
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...
02:50Nuclear 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...
01:23Atomic Nuclei: Nuclear Relaxation Processes
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. This...
01:10Detection of Black Holes
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...
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...