{"title":"快速旋转恒星的振荡","authors":"B. Dintrans, M. Rieutord","doi":"10.1553/CIA147S65","DOIUrl":null,"url":null,"abstract":"The effects of rapid rotation on stellar pulsation is examined using an accurate 2D numerical method. We compare the results of these non-perturbative calculations with those of perturbative methods and find that frequency differences exceed 0.08 μHz on half of the modes when the rotation rate is 15% of the keplerian (break-up) limit. The differences between the two results is mainly attributed to the approximate treatment of the centrifugal force in perturbative methods. We also explore different levels of approximation for the Coriolis force.","PeriodicalId":151133,"journal":{"name":"Third Coast","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2001-11-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"4","resultStr":"{\"title\":\"Oscillations of rapidly rotating stars\",\"authors\":\"B. Dintrans, M. Rieutord\",\"doi\":\"10.1553/CIA147S65\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"The effects of rapid rotation on stellar pulsation is examined using an accurate 2D numerical method. We compare the results of these non-perturbative calculations with those of perturbative methods and find that frequency differences exceed 0.08 μHz on half of the modes when the rotation rate is 15% of the keplerian (break-up) limit. The differences between the two results is mainly attributed to the approximate treatment of the centrifugal force in perturbative methods. We also explore different levels of approximation for the Coriolis force.\",\"PeriodicalId\":151133,\"journal\":{\"name\":\"Third Coast\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2001-11-23\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"4\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Third Coast\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1553/CIA147S65\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Third Coast","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1553/CIA147S65","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
The effects of rapid rotation on stellar pulsation is examined using an accurate 2D numerical method. We compare the results of these non-perturbative calculations with those of perturbative methods and find that frequency differences exceed 0.08 μHz on half of the modes when the rotation rate is 15% of the keplerian (break-up) limit. The differences between the two results is mainly attributed to the approximate treatment of the centrifugal force in perturbative methods. We also explore different levels of approximation for the Coriolis force.
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