{"title":"银河系凸出的X射线光晕——6.7 keV线映射","authors":"K. Koyama, S. Yamauchi","doi":"10.1063/1.44016","DOIUrl":null,"url":null,"abstract":"The 6.7 keV line is the K‐shell resonance transition from a Helium like iron (FeXXV) and is the most intense line in an optically thin cosmic plasma with a temperature ranging from 107 to 108 K. Therefore optically thin hot plasma in our Galaxy can be selected by the 6.7 keV line. This paper report on the 6.7 keV line map and discuss on the nature of the hot gas components in our Galaxy.","PeriodicalId":310353,"journal":{"name":"Back to the Galaxy","volume":"52 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2008-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"X‐ray halo from the Galactic bulge ‐The 6.7 keV line mapping\",\"authors\":\"K. Koyama, S. Yamauchi\",\"doi\":\"10.1063/1.44016\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The 6.7 keV line is the K‐shell resonance transition from a Helium like iron (FeXXV) and is the most intense line in an optically thin cosmic plasma with a temperature ranging from 107 to 108 K. Therefore optically thin hot plasma in our Galaxy can be selected by the 6.7 keV line. This paper report on the 6.7 keV line map and discuss on the nature of the hot gas components in our Galaxy.\",\"PeriodicalId\":310353,\"journal\":{\"name\":\"Back to the Galaxy\",\"volume\":\"52 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-05-29\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Back to the Galaxy\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.44016\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Back to the Galaxy","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.44016","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
X‐ray halo from the Galactic bulge ‐The 6.7 keV line mapping
The 6.7 keV line is the K‐shell resonance transition from a Helium like iron (FeXXV) and is the most intense line in an optically thin cosmic plasma with a temperature ranging from 107 to 108 K. Therefore optically thin hot plasma in our Galaxy can be selected by the 6.7 keV line. This paper report on the 6.7 keV line map and discuss on the nature of the hot gas components in our Galaxy.
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