Stellar Active Region Evolution – II. Identification and Evolution of Variance Morphologies in Ca II H+K Time Series |
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| Authors: | Donahue R A Dobson A K Baliunas S L |
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| Institution: | (1) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, 02138, U.S.A.;(2) Mount Wilson Institute, Pasadena, CA, 91106, U.S.A;(3) Department of Astronomy, Whitman College, Walla Walla, WA, 99362, U.S.A;(4) Center for Automated Space Science and Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, 37203, U.S.A |
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| Abstract: | The relative distribution of pooled variance computed at various time scales for records of chromospheric activity has been calculated for approximately 100 stars observed at Mount Wilson Observatory. As shown in Paper I, analysis of the pooled variance provides a technique for estimating the lifetimes of stellar active regions and their influence on chromospheric time series used for determining rotation and activity cycle periods. Pooled variance diagrams may be divided into three morphological types which depend to a large extent on a star's mean level of chromospheric activity (i.e., age) and B-V color (i.e., mass), and possibly depend on star's evolutionary state. |
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