{"title":"银河系凸起的条形模型","authors":"J. Sellwood","doi":"10.1063/1.44022","DOIUrl":null,"url":null,"abstract":"Bars in galaxies acquire a pronounced peanut shape when seen from the side. It is shown that the peanut‐shaped bar in a 3‐D N‐body model has an appearance closely resembling the COBE image of the Milky Way bulge, when viewed from within the disk. Moreover, the projected velocity distribution is not far from isotropic, in agreement with modern kinematic data. Although the model is not a perfect match to the Milky Way, it exhibits a straightforward mechanism for the formation of the observed shape of the Milky Way ‘‘bulge’’ and provides a further argument in favor of a bar in the Galaxy.","PeriodicalId":310353,"journal":{"name":"Back to the Galaxy","volume":"90 1","pages":"0"},"PeriodicalIF":0.0000,"publicationDate":"2008-05-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"2","resultStr":"{\"title\":\"A bar model for the Galactic bulge\",\"authors\":\"J. Sellwood\",\"doi\":\"10.1063/1.44022\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"Bars in galaxies acquire a pronounced peanut shape when seen from the side. It is shown that the peanut‐shaped bar in a 3‐D N‐body model has an appearance closely resembling the COBE image of the Milky Way bulge, when viewed from within the disk. Moreover, the projected velocity distribution is not far from isotropic, in agreement with modern kinematic data. Although the model is not a perfect match to the Milky Way, it exhibits a straightforward mechanism for the formation of the observed shape of the Milky Way ‘‘bulge’’ and provides a further argument in favor of a bar in the Galaxy.\",\"PeriodicalId\":310353,\"journal\":{\"name\":\"Back to the Galaxy\",\"volume\":\"90 1\",\"pages\":\"0\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-05-29\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"2\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Back to the Galaxy\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.44022\",\"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/10.1063/1.44022","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
Bars in galaxies acquire a pronounced peanut shape when seen from the side. It is shown that the peanut‐shaped bar in a 3‐D N‐body model has an appearance closely resembling the COBE image of the Milky Way bulge, when viewed from within the disk. Moreover, the projected velocity distribution is not far from isotropic, in agreement with modern kinematic data. Although the model is not a perfect match to the Milky Way, it exhibits a straightforward mechanism for the formation of the observed shape of the Milky Way ‘‘bulge’’ and provides a further argument in favor of a bar in the Galaxy.
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