L. Hillenbrand, E. Mamajek, J. Stauffer, D. Soderblom, J. Carpenter, M. Meyer
{"title":"从3myr到3gyr的恒星年龄估计","authors":"L. Hillenbrand, E. Mamajek, J. Stauffer, D. Soderblom, J. Carpenter, M. Meyer","doi":"10.1063/1.3099237","DOIUrl":null,"url":null,"abstract":"We present recent progress on quantitative estimation of stellar ages using indicators such as theoretical evolutionary tracks, rotation, rotation‐driven chromospheric and coronal activity, and lithium depletion. Our focus is on roughly solar‐mass and solar‐metallicity stars younger than the Sun. We attempt to characterize the systematic and random error sources and then derive “best” ages along with the dispersion in age arising among the various age estimation methods. Our main application of these techniques is to the evolution of debris disks.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":null,"pages":null},"PeriodicalIF":0.0000,"publicationDate":"2008-12-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"2","resultStr":"{\"title\":\"Stellar Age Estimation from 3 Myr to 3 Gyr\",\"authors\":\"L. Hillenbrand, E. Mamajek, J. Stauffer, D. Soderblom, J. Carpenter, M. Meyer\",\"doi\":\"10.1063/1.3099237\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"We present recent progress on quantitative estimation of stellar ages using indicators such as theoretical evolutionary tracks, rotation, rotation‐driven chromospheric and coronal activity, and lithium depletion. Our focus is on roughly solar‐mass and solar‐metallicity stars younger than the Sun. We attempt to characterize the systematic and random error sources and then derive “best” ages along with the dispersion in age arising among the various age estimation methods. Our main application of these techniques is to the evolution of debris disks.\",\"PeriodicalId\":8453,\"journal\":{\"name\":\"arXiv: Astrophysics\",\"volume\":null,\"pages\":null},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2008-12-06\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"2\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"arXiv: Astrophysics\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.1063/1.3099237\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv: Astrophysics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.1063/1.3099237","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
We present recent progress on quantitative estimation of stellar ages using indicators such as theoretical evolutionary tracks, rotation, rotation‐driven chromospheric and coronal activity, and lithium depletion. Our focus is on roughly solar‐mass and solar‐metallicity stars younger than the Sun. We attempt to characterize the systematic and random error sources and then derive “best” ages along with the dispersion in age arising among the various age estimation methods. Our main application of these techniques is to the evolution of debris disks.
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