| dbo:abstract
|
- Als Eisenlinien werden in der Physik die Spektrallinien des Elements Eisen bezeichnet. (de)
- The K-line is a spectral peak in astronomical spectrometry used, along with the , to observe and describe the light spectrum of stars. The K-line is associated with iron (Fe) and is described as being from emissions at ~6.4keV (thousands of electron volts). On 5 October 2006 NASA announced the results of research using the Japanese JAXA Suzaku satellite, after earlier work with the XMM-Newton satellite. "The observations include clocking the speed of a black hole's spin rate and measuring the angle at which matter pours into the void, as well as evidence for a wall of X-ray light pulled back and flattened by gravity."The study teams observed X-ray emissions from the "broad iron K line" near the event horizon of several super-massive black holes of galaxies called MCG-6-30-15 and MCG-5-23-16. The normally narrow K-line is broadened by the doppler shift (red shift or blue shift) of the X-ray light emitted by matter being affected by the gravity of the black hole. The results coincide with predictions Albert Einstein's theory of general relativity. The teams were led by Andrew Fabian of Cambridge University, England, and of NASA's Goddard Space Flight Center, Greenbelt, Maryland, United States. (en)
- 在天文学光谱学中，K线与，都是一种谱峰，用以观测和描述恒星的光谱。K线与铁相关，是来自6.14keV（千电子伏特）附近的发射线。 2006年10月5日，NASA宣布早期使用日本宇宙航空研究开发机构的朱雀卫星与XMM-牛顿卫星协同工作的结果，“对黑洞旋转速率的计时及对物质倒进空洞的角度的观测，连同X光被重力拉回压平所形成的一道墙的证据。”研究团队观测了来自“宽铁K线”的X射线的发射，这些“宽铁K线”接近于星系MCG-6-30-15和MCG-5-23-16的数个超大质量黑洞的事件视界。普通的窄K线被物质所发射的X射线的多普勒效应（红移或蓝移）所拓宽，而这些物质受到黑洞重力的影响。最后结果與爱因斯坦的广义相对论所预言相同。该研究团队由来自剑桥大学的安德鲁·费边和来自美国戈达德太空飞行中心的所领导。 (zh)
|
| dbo:wikiPageExternalLink
| |
| dbo:wikiPageID
| |
| dbo:wikiPageLength
|
- 2086 (xsd:nonNegativeInteger)
|
| dbo:wikiPageRevisionID
| |
| dbo:wikiPageWikiLink
| |
| dbp:wikiPageUsesTemplate
| |
| dcterms:subject
| |
| rdf:type
| |
| rdfs:comment
|
- Als Eisenlinien werden in der Physik die Spektrallinien des Elements Eisen bezeichnet. (de)
- 在天文学光谱学中，K线与，都是一种谱峰，用以观测和描述恒星的光谱。K线与铁相关，是来自6.14keV（千电子伏特）附近的发射线。 2006年10月5日，NASA宣布早期使用日本宇宙航空研究开发机构的朱雀卫星与XMM-牛顿卫星协同工作的结果，“对黑洞旋转速率的计时及对物质倒进空洞的角度的观测，连同X光被重力拉回压平所形成的一道墙的证据。”研究团队观测了来自“宽铁K线”的X射线的发射，这些“宽铁K线”接近于星系MCG-6-30-15和MCG-5-23-16的数个超大质量黑洞的事件视界。普通的窄K线被物质所发射的X射线的多普勒效应（红移或蓝移）所拓宽，而这些物质受到黑洞重力的影响。最后结果與爱因斯坦的广义相对论所预言相同。该研究团队由来自剑桥大学的安德鲁·费边和来自美国戈达德太空飞行中心的所领导。 (zh)
- The K-line is a spectral peak in astronomical spectrometry used, along with the , to observe and describe the light spectrum of stars. The K-line is associated with iron (Fe) and is described as being from emissions at ~6.4keV (thousands of electron volts). (en)
|
| rdfs:label
|
- Eisenlinien (Physik) (de)
- K-line (x-ray) (en)
- K线 (X射线) (zh)
|
| owl:differentFrom
| |
| owl:sameAs
| |
| prov:wasDerivedFrom
| |
| foaf:isPrimaryTopicOf
| |
| is dbo:wikiPageDisambiguates
of | |
| is dbo:wikiPageRedirects
of | |
| is dbo:wikiPageWikiLink
of | |
| is foaf:primaryTopic
of | |
